Astrophysical X-ray source

1820: 1921: 1135:'s galactic center appears to harbor an X-ray source characteristic of a black hole of a million or more solar masses. Seen above, the false-color X-ray picture shows a number of X-ray sources, likely X-ray binary stars, within Andromeda's central region as yellowish dots. The blue source located right at the galaxy's center is coincident with the position of the suspected massive black hole. While the X-rays are produced as material falls into the black hole and heats up, estimates from the X-ray data show Andromeda's central source to be very cold – only about million degrees, compared to the tens of millions of degrees indicated for Andromeda's X-ray binaries. 950: 1109: 2658: 1659: 1755:, a compact group of galaxies discovered about 130 years ago and located about 280 million light years from Earth, provides a rare opportunity to observe a galaxy group in the process of evolving from an X-ray faint system dominated by spiral galaxies to a more developed system dominated by elliptical galaxies and bright X-ray emission. Being able to witness the dramatic effect of collisions in causing this evolution is important for increasing our understanding of the origins of the hot, X-ray bright halos of gas in groups of galaxies. 1792: 1749: 1040: 2529:

transition region fluxes; the latter can be followed up to mid-A type stars at quite high levels. Whether or not these atmospheres are indeed heated acoustically and drive an "expanding", weak and cool corona or whether they are heated magnetically, the X-ray deficit and the low coronal temperatures clearly attest to the inability of these stars to maintain substantial, hot coronae in any way comparable to cooler active stars, their appreciable chromospheres notwithstanding.

2127: 442: 2365:, while in heliocentric orbits, were hit at 10:51 am EST by a blast of gamma ray radiation. This contact raised the radiation readings on both the probes Konus experiments from a normal 100 counts per second to over 200,000 counts a second, in only a fraction of a millisecond. This giant flare was detected by numerous spacecraft and with these detections was localized by the interplanetary network to SGR 0526-66 inside the N-49 SNR of the 2312: 1291: 1031:

unresolved in the ROSAT picture. The dark side of the Moon's disk shadows this X-ray background radiation coming from the deep space. A few X-rays only seem to come from the shadowed lunar hemisphere. Instead, they originate in Earth's geocorona or extended atmosphere which surrounds the orbiting X-ray observatory. The measured lunar X-ray luminosity of ~1.2 × 10 W makes the Moon one of the weakest known non-terrestrial X-ray sources.

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beamed or exceeds the Eddington limit, the ULX may be a stellar-mass black hole. The nearby spiral galaxy NGC 1313 has two compact ULXs, X-1 and X-2. For X-1 the X-ray luminosity increases to a maximum of 3 × 10 W, exceeding the Eddington limit, and enters a steep power-law state at high luminosities more indicative of a stellar-mass black hole, whereas X-2 has the opposite behavior and appears to be in the hard X-ray state of an IMBH.

1632:. Here the filament absorbs soft X-rays between 100 and 300 eV, indicating that the hot gas is located behind the filament. This filament may be part of a shell of neutral gas that surrounds the hot bubble. Its interior is energized by UV light and stellar winds from hot stars in the Orion OB1 association. These stars energize a superbubble about 1200 lys across which is observed in the optical (Hα) and X-ray portions of the spectrum. 2053: 1740:. On the right side of the images is the visual image of the constellation. On the left is Orion as seen in X-rays only. Betelgeuse is easily seen above the three stars of Orion's belt on the right. The brightest object in the visual image is the full moon, which is also in the X-ray image. The X-ray colors represent the temperature of the X-ray emission from each star: hot stars are blue-white and cooler stars are yellow-red. 1518: 1613: 5401: 515: 1569: 1728:. On the left is Orion as seen in X-rays only. Betelgeuse is easily seen above the three stars of Orion's belt on the right. The X-ray colors represent the temperature of the X-ray emission from each star: hot stars are blue-white and cooler stars are yellow-red. The brightest object in the optical image is the full moon, which is also in the X-ray image. The X-ray image was actually obtained by the 1972: 1455: 1128: 1721: 1375:. The new X-ray observation shows three distinct structures: an outer, horseshoe-shaped ring about 2 light years in diameter, a hot inner core about 3 light-months in diameter, and a hot central source less than 1 light-month in diameter which may contain the superstar that drives the whole show. The outer ring provides evidence of another large explosion that occurred over 1,000 years ago. 994: 2640: 744:-related variations are observed in the flux of solar X-ray and UV or EUV radiation. Rotation is one of the primary determinants of the magnetic dynamo, but this point could not be demonstrated by observing the Sun: the Sun's magnetic activity is in fact strongly modulated (due to the 11-year magnetic spot cycle), but this effect is not directly dependent on the rotation period. 504: 159: 1397: 1876: 966:, scientists have detected X-rays from a low mass brown dwarf in a multiple star system. This is the first time that a brown dwarf this close to its parent star(s) (Sun-like stars TWA 5A) has been resolved in X-rays. "Our Chandra data show that the X-rays originate from the brown dwarf's coronal plasma which is some 3 million degrees Celsius", said Yohko Tsuboi of 1064:

what Swift's XRT sees", said Stefan Immler, of the Goddard Space Flight Center. This interaction, called charge exchange, results in X-rays from most comets when they pass within about three times Earth's distance from the sun. Because Lulin is so active, its atomic cloud is especially dense. As a result, the X-ray-emitting region extends far sunward of the comet.

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to spread out. The entire line has been shifted to longer wavelengths (left, red) because of the neutron star's powerful gravity. The line is brighter toward shorter wavelengths (right, blue) because Einstein's special theory of relativity predicts that a high-speed source beamed toward Earth will appear brighter than the same source moving away from Earth.

984: 756: 998:(light blue lines) generates strong electric fields in the space around the planet. Charged particles (white dots), trapped in Jupiter's magnetic field, are continually being accelerated (gold particles) down into the atmosphere above the polar regions, so auroras are almost always active on Jupiter. Observation period: 17 hrs, 24–26 February 2003. 2596:. The X-ray flux corresponds to a total energy density of about 5 x 10 eV/cm. The ROSAT soft X-ray diffuse background (SXRB) image shows the general increase in intensity from the Galactic plane to the poles. At the lowest energies, 0.1 – 0.3 keV, nearly all of the observed soft X-ray background (SXRB) is thermal emission from ~10 K plasma. 2215:, as of 1996, only X Per and LSI+61°303 have X-ray outbursts of much higher luminosity and harder spectrum (kT ~ 10–20 keV) vs. (kT ≤ 1 keV); however, LSI+61°303 further distinguishes itself by its strong, outbursting radio emission. "The radio properties of LSI+61°303 are similar to those of the "standard" high-mass X-ray binaries such as 921: 33: 946:. The absence of X-rays from LP 944-20 during the non-flaring period is also a significant result. It sets the lowest observational limit on steady X-ray power produced by a brown dwarf star, and shows that coronas cease to exist as the surface temperature of a brown dwarf cools below about 2500 °C and becomes electrically neutral. 2261: 733:

flight, T. Burnight wrote, "The sun is assumed to be the source of this radiation although radiation of wavelength shorter than 4 Å would not be expected from theoretical estimates of black body radiation from the solar corona." And, of course, people have seen the solar corona in scattered visible light during solar eclipses.

1628:. Soft X-rays are emitted by hot gas (T ~ 2–3 MK) in the interior of the superbubble. This bright object forms the background for the "shadow" of a filament of gas and dust. The filament is shown by the overlaid contours, which represent 100 micrometre emission from dust at a temperature of about 30 K as measured by 1992:"We've seen these asymmetric lines from many black holes, but this is the first confirmation that neutron stars can produce them as well. It shows that the way neutron stars accrete matter is not very different from that of black holes, and it gives us a new tool to probe Einstein's theory", says Tod Strohmayer of 2406:"Young, fast-spinning pulsars were not thought to have enough magnetic energy to generate such powerful bursts", says Marjorie Gonzalez, formerly of McGill University in Montreal, Canada, now based at the University of British Columbia in Vancouver. "Here's a normal pulsar that's acting like a magnetar." 1978:

spectrum from superheated iron atoms at the inner edge of the accretion disk orbiting the neutron star in Serpens X-1. The line is usually a symmetrical peak, but it exhibits the classic features of distortion due to relativistic effects. The extremely fast motion of the iron-rich gas causes the line

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may be due to a collision with a smaller galaxy such as those in the lower left of the image. The most recent star burst (star formation due to compression waves) has lit up the Cartwheel rim, which has a diameter larger than the Milky Way. There is an exceptionally large number of black holes in the

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The Chandra X-ray image is of the quasar PKS 1127-145, a highly luminous source of X-rays and visible light about 10 billion light years from Earth. An enormous X-ray jet extends at least a million light years from the quasar. Image is 60 arcsec on a side. RA 11h 30 m 7.10s Dec −14° 49' 27"

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In the late 1930s, the presence of a very hot, tenuous gas surrounding the Sun was inferred indirectly from optical coronal lines of highly ionized species. In the mid-1940s radio observations revealed a radio corona around the Sun. After detecting X-ray photons from the Sun in the course of a rocket

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In addition to discrete sources which stand out against the sky, there is good evidence for a diffuse X-ray background. During more than a decade of observations of X-ray emission from the Sun, evidence of the existence of an isotropic X-ray background flux was obtained in 1956. This background flux

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The observations from NASA's Chandra X-ray Observatory showed that the object had brightened in X-rays, confirming that the bursts were from the pulsar, and that its spectrum had changed to become more magnetar-like. The fact that PSR J1846's spin rate is decelerating also means that it has a strong

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PSR J1846-0258 is in the constellation Aquila. It had been classed as a normal pulsar because of its fast spin (3.1 s) and pulsar-like spectrum. RXTE caught four magnetar-like X-ray bursts on 31 May 2006, and another on 27 July 2006. Although none of these events lasted longer than 0.14-second, they

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One of the rings, caused by a major eruption, is a shock wave 85,000 light-years in diameter around the black hole. Other remarkable features observed include narrow X-ray emitting filaments up to 100,000 light-years long, and a large cavity in the hot gas caused by a major eruption 70 million years

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This light curve of Her X-1 shows long term and medium term variability. Each pair of vertical lines delineate the eclipse of the compact object behind its companion star. In this case, the companion is a 2 Solar-mass star with a radius of nearly four times that of the Sun. This eclipse shows us the

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are thought to represent shock waves produced by matter rushing away from the superstar at supersonic speeds. The temperature of the shock-heated gas ranges from 60 MK in the central regions to 3 MK on the horseshoe-shaped outer structure. "The Chandra image contains some puzzles for existing ideas

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of the star is strong enough to prevent the formation of an accretion disc. The material in the disc gets very hot because of friction, and emits X-rays. The material in the disc slowly loses its angular momentum and falls into the compact star. In neutron stars and white dwarfs, additional X-rays

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In visible light, 4C 71.07 is less than impressive, just a distant speck of light. It is in radio and in X-rays – and now, gamma rays – that this object really shines. 4C 71.07 is its designation in the Fourth Cambridge Survey of radio sources. Its redshift of z=2.17, puts it about 11 billion

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In this sample of images from 2004, bright X-ray arcs of low energy (0.1 – 10 keV) are generated during auroral activity. The images are superimposed on a simulated image of Earth. The color code of the X-ray arcs represent brightness, with maximum brightness shown in red. Distance from the North

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notes, "PSR J1846's actual magnetic field could be much stronger than the measured amount, suggesting that many young neutron stars classified as pulsars might actually be magnetars in disguise, and that the true strength of their magnetic field only reveals itself over thousands of years as they

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commented, "We're seeing the gas whipping around just outside the neutron star's surface,". "And since the inner part of the disk obviously can't orbit any closer than the neutron star's surface, these measurements give us a maximum size of the neutron star's diameter. The neutron stars can be no

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Pictor A is a galaxy that may have a black hole at its center which has emitted magnetized gas at extremely high speed. The bright spot at the right in the image is the head of the jet. As it plows into the tenuous gas of intergalactic space, it emits X-rays. Pictor A is X-ray source designated H

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as it closed to 63 Gm of Earth. For the first time, astronomers can see simultaneous UV and X-ray images of a comet. "The solar wind – a fast-moving stream of particles from the sun – interacts with the comet's broader cloud of atoms. This causes the solar wind to light up with X-rays, and that's

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In the Röntgensatellit (ROSAT) image of the Moon, pixel brightness corresponds to X-ray intensity. The bright lunar hemisphere shines in X-rays because it re-emits X-rays originating from the sun. The background sky has an X-ray glow in part due to the myriad of distant, powerful active galaxies,

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In the few genuine late A- or early F-type coronal emitters, their weak dynamo operation is generally not able to brake the rapidly spinning star considerably during their short lifetime so that these coronae are conspicuous by their severe deficit of X-ray emission compared to chromospheric and

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Hot X-ray emitting gas pervades the galaxy cluster MS 0735.6+7421 in Camelopardus. Two vast cavities – each 600,000 lyrs in diameter appear on opposite sides of a large galaxy at the center of the cluster. These cavities are filled with a two-sided, elongated, magnetized bubble of extremely

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Jupiter shows intense X-ray emission associated with auroras in its polar regions (Chandra observatory X-ray image on the left). The accompanying schematic illustrates how Jupiter's unusually frequent and spectacular auroral activity is produced. Jupiter's strong, rapidly rotating magnetic field

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to white dwarf. X-ray images reveal clouds of multimillion degree gas that have been compressed and heated by the fast stellar wind. Eventually the central star collapses to form a white dwarf. For a billion or so years after a star collapses to form a white dwarf, it is "white" hot with surface

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was detected by BATSE as a source of soft gamma rays and hard X-rays. "What BATSE has discovered is that it can be a soft gamma-ray source", McCollough said. QSO 0836+7107 is the faintest and most distant object to be observed in soft gamma rays. It has already been observed in gamma rays by the

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Zhitnik IA; Logachev YI; Bogomolov AV; Denisov YI; Kavanosyan SS; Kuznetsov SN; Morozov OV; Myagkova IN; Svertilov SI; Ignat'ev AP; Oparin SN; Pertsov AA; Tindo IP (2006). "Polarization, temporal, and spectral parameters of solar flare hard X-rays as measured by the SPR-N instrument onboard the

2388:"We are watching one type of neutron star literally change into another right before our very eyes. This is a long-sought missing link between different types of pulsars", says Fotis Gavriil of NASA's Goddard Space Flight Center in Greenbelt, Maryland, and the University of Maryland, Baltimore. 2206:

is a periodic, radio-emitting binary system that is also the gamma-ray source, CG135+01. LSI+61°303 is a variable radio source characterized by periodic, non-thermal radio outbursts with a period of 26.5 d, attributed to the eccentric orbital motion of a compact object, probably a neutron star,

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channel multiplier array observation. "The broad-band spectrum of this DA white dwarf can be explained as emission from a homogeneous, high-gravity, pure hydrogen atmosphere with a temperature near 28,000 K." These observations of PG 1658+441 support a correlation between temperature and helium

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black hole. Many ULXs show strong variability and may be black hole binaries. To fall into the class of intermediate-mass black holes (IMBHs), their luminosities, thermal disk emissions, variation timescales, and surrounding emission-line nebulae must suggest this. However, when the emission is

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was launched on 31 July 2001 to coincide with the 23rd solar cycle maximum. The solar flare of 29 October 2003 apparently showed a significant degree of linear polarization (> 70% in channels E2 = 40–60 keV and E3 = 60–100 keV, but only about 50% in E1 = 20–40 keV) in hard X-rays, but other

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Supernova 2005ke, which was detected in 2005, is a Type Ia supernova, an important "standard candle" explosion used by astronomers to measure distances in the universe. Shown here is the event in optical, ultraviolet and X-ray wavelengths. This is the first X-ray image of a Type Ia, and it has

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Chandra image of the hot X-ray emitting gas that pervades the galaxy cluster MS 0735.6+7421 in Camelopardus. Two vast cavities – each 600,000 lyrs in diameter appear on opposite sides of a large galaxy at the center of the cluster. These cavities are filled with a two-sided, elongated,

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at ~160 pc. It is relatively isolated from other star-forming clouds, so it is unlikely that older pre-main sequence (PMS) stars have drifted into the field. The total stellar population is 200–300. The Cha I cloud is further divided into the North cloud or region and South cloud or main

2453:, on the other hand, appears to be always X-ray dark. The X-ray flux from the entire stellar surface corresponds to a surface flux limit that ranges from 30–7000 ergs s cm at T=1 MK, to ~1 erg s cm at higher temperatures, five orders of magnitude below the quiet Sun X-ray surface flux. 2626:

X-ray observations offer the possibility to detect (X-ray dark) planets as they eclipse part of the corona of their parent star while in transit. "Such methods are particularly promising for low-mass stars as a Jupiter-like planet could eclipse a rather significant coronal area."

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Electric potentials of about 10 million volts, and currents of 10 million amps – a hundred times greater than the most powerful lightning bolts – are required to explain the auroras at Jupiter's poles, which are a thousand times more powerful than those on Earth.

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This Chandra X-ray image of Radio Galaxy Pictor A shows a spectacular jet emanating from the center of the galaxy (left) and extends across 360 thousand lyr toward a brilliant hot spot. Image is 4.2 arcmin across. RA 05h 19 m 49.70s Dec −45° 46' 45" in Pictor. Instrument:

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on 16 August 1680). Possible explanations lean toward the idea that the source star was unusually massive and had previously ejected much of its outer layers. These outer layers would have cloaked the star and reabsorbed much of the light released as the inner star collapsed.

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On Earth, auroras are triggered by solar storms of energetic particles, which disturb Earth's magnetic field. As shown by the swept-back appearance in the illustration, gusts of particles from the Sun also distort Jupiter's magnetic field, and on occasion produce auroras.

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and Christopher Thompson in 1992, but the first recorded burst of gamma rays thought to have been from a magnetar was on 5 March 1979. These magnetic fields are hundreds of thousands of times stronger than any man-made magnet, and quadrillions of times more powerful than

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Saturn's X-ray spectrum is similar to that of X-rays from the Sun indicating that Saturn's X-radiation is due to the reflection of solar X-rays by Saturn's atmosphere. The optical image is much brighter, and shows the beautiful ring structures, which were not detected in

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observatory: the blue, green, and red channels show the 17.1 nm, 19.5 nm, and 28.4 nm, respectively. These TRACE filters are most sensitive to emission from 1, 1.5, and 2 million degree plasma, thus showing the entire corona and detail of coronal loops in the lower solar

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The Chandra three-color image (inset) is a region of the supernova remnant Puppis A (wide-angle view from ROSAT in blue). reveals a cloud being torn apart by a shock wave produced in a supernova explosion. ROSAT image is 88 arcmin across; Chandra image 8 arcmin across.

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imaged it on 28 January 2009. This image merges data acquired by Swift's Ultraviolet/Optical Telescope (blue and green) and X-Ray Telescope (red). At the time of the observation, the comet was 99.5 million miles from Earth and 115.3 million miles from the

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in Tokyo. "This brown dwarf is as bright as the Sun today in X-ray light, while it is fifty times less massive than the Sun", said Tsuboi. "This observation, thus, raises the possibility that even massive planets might emit X-rays by themselves during their youth!"

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While neutron stars and black holes are the quintessential point sources of X-rays, all main sequence stars are likely to have hot enough coronae to emit X-rays. A- or F-type stars have at most thin convection zones and thus produce little coronal activity.

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from LP 944-20 could have its origin in the turbulent magnetized hot material beneath the brown dwarf's surface. A sub-surface flare could conduct heat to the atmosphere, allowing electric currents to flow and produce an X-ray flare, like a stroke of

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from Earth and after the Sun is the strongest X-ray source in the sky at energies below 20 keV. Its X-ray output is 2.3 × 10 W, about 60,000 times the total luminosity of the Sun. Scorpius X-1 itself is a neutron star. This system is classified as a

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rich deposits of neon, magnesium, and silicon were discovered. These elements are among those that form the building blocks for habitable planets. The clouds imaged contain magnesium and silicon at 16 and 24 times respectively, the abundance in the

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B collides with gas in the group, a huge shock wave bigger than the Milky Way spreads throughout the medium between the galaxies, heating some of the gas to temperatures of millions of degrees where they emit X-rays detectable with the NASA

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observations timed to coincide with the expected eclipse of the X-ray source allowed an accurate determination of the mass of the X-ray source (at least 1.2 solar masses), establishing the X-ray source as a rare, ultra-massive white dwarf.

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Stephan's Quintet are of interest because of their violent collisions. Four of the five galaxies in Stephan's Quintet form a physical association, and are involved in a cosmic dance that most likely will end with the galaxies merging. As

2385:(RXTE) has revealed that the youngest known pulsing neutron star has thrown a temper tantrum. The collapsed star occasionally unleashes powerful bursts of X-rays, which are forcing astronomers to rethink the life cycle of neutron stars. 2185:: when the effects of the Doppler shift are subtracted, there is a residual redshift which corresponds to a velocity of about 12,000 kps. This does not represent an actual velocity of the system away from the Earth; rather, it is due to 825:

When the core of a medium mass star contracts, it causes a release of energy that makes the envelope of the star expand. This continues until the star finally blows its outer layers off. The core of the star remains intact and becomes a

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What is the evolutionary relationship between pulsars and magnetars? Astronomers would like to know if magnetars represent a rare class of pulsars, or if some or all pulsars go through a magnetar phase during their life cycles. NASA's

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range, resolving solar features to 2.5 arc seconds with a temporal resolution of 0.5–2 seconds. SXT was sensitive to plasma in the 2–4 MK temperature range, making it an ideal observational platform to compare with data collected from

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Map of the column density of Galactic neutral hydrogen in the same projection as the 0.25 keV SXRB. Note the general negative correlation between the 0.25 keV diffuse X-ray background and the neutral hydrogen column density shown

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and hence define a new class of massive X-ray binaries: Supergiant Fast X-ray Transients (SFXTs). XTE J1739–302 is one of these. Discovered in 1997, remaining active only one day, with an X-ray spectrum well fitted with a thermal

2189:, which makes moving clocks appear to stationary observers to be ticking more slowly. In this case, the relativistically moving excited atoms in the jets appear to vibrate more slowly and their radiation thus appears red-shifted. 1983:

As of 27 August 2007, discoveries concerning asymmetric iron line broadening and their implications for relativity have been a topic of much excitement. With respect to the asymmetric iron line broadening, Edward Cackett of the

628: 2011:. "There could be exotic kinds of particles or states of matter, such as quark matter, in the centers of neutron stars, but it's impossible to create them in the lab. The only way to find out is to understand neutron stars." 2248:(temperature of ~20 keV), resembling the spectral properties of accreting pulsars, it was at first classified as a peculiar Be/X-ray transient with an unusually short outburst. A new burst was observed on 8 April 2008 with 1906:(W24). In probably the first catalogue of galactic X-ray sources, two Sgr X-1s are suggested: (1) at 1744–2312 and (2) at 1755–2912, noting that (2) is an uncertain identification. Source (1) seems to correspond to S11. 1694:. In the image, red represents low, green intermediate, and blue high-energy (temperature) X-rays. Image is 4 arcmin on a side. RA 10h 49 m 52.5s Dec +32° 59' 6". Observation date: 28 April 2001. Instrument: ACIS. 3867:

Alcala JM; Krautter J; Schmitt JHMM; Covino E; Wichmann R; Mundt R (November 1995). "A study of the Chamaeleon star forming region from the ROSAT all-sky survey. I. X-ray observations and optical identifications".

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Real mass transfer variations may be occurring in V Sge similar to SSXS RX J0513.9-6951 as revealed by analysis of the activity of the SSXS V Sge where episodes of long low states occur in a cycle of ~400 days.

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Chandra X-ray (left) and Hubble optical (right) images of Saturn on 14 April 2003. Observation period: 20 hrs, 14–15 April 2003. Color code: red (0.4 – 0.6 keV), green (0.6 – 0.8 keV), blue (0.8 – 1.0 keV).

315:. These electrons can also interact with visible light emitted by the disk around the AGN or the black hole at its center. These photons accelerate the electrons, which then emit X- and gamma-radiation via 258:

A view of 4C 71.07 from observations by the Burst and Transient Source Experiment. This helped convince scientists that they were studying data from the quasar and not some other source in the neighborhood.

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HD 49798 is a subdwarf star that forms a binary system with RX J0648.0-4418. The subdwarf star is a bright object in the optical and UV bands. The orbital period of the system is accurately known. Recent

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Mazets EP, Aptekar RL, Cline TL, Frederiks DD, Goldsten JO, Golenetskii SV, Hurley K, von Kienlin A, Pal'shin VD (2008). "A Giant Flare from a Soft Gamma Repeater in the Andromeda Galaxy, M31".

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Negueruela, I.; Smith, D. M.; Reig, P.; Chaty, S.; Torrejón, J. M. (2006). "Supergiant Fast X-ray Transients: A New Class of High Mass X-ray Binaries Unveiled by INTEGRAL". In Wilson, A. (ed.).

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With no strong central nuclear energy source, the interior of a brown dwarf is in a rapid boiling, or convective state. When combined with the rapid rotation that most brown dwarfs exhibit,

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of 8σ, it was found that the spatial offset of the center of the total mass from the center of the baryonic mass peaks cannot be explained with an alteration of the gravitational force law.

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of lower-energy photons by relativistic electrons, knock-on collisions of fast protons with atomic electrons, and atomic recombination, with or without additional electron transitions.

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The Chamaeleon II dark cloud contains some 40 X-ray sources. Observation in Chamaeleon II was carried out from 10 to 17 September 1993. Source RXJ 1301.9-7706, a new WTTS candidate of

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remnant (4U 0000+72) initially emitted radiation in the X-ray bands (1970–1977). Strangely, when it was observed at a later time (2008) X-ray radiation was not detected. Instead, the

2518:(α TrA / α Trianguli Australis) appears to be a Hybrid star (parts of both sides) in the "Dividing Line" of evolutionary transition to red giant. α TrA can serve to test the several 2563:

inject enormous amounts of energy into their surroundings, which leads to hypersonic turbulence. The resultant structures – of varying sizes – can be observed, such as

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is a large star forming region (SFR) that includes the Chamaeleon I, Chamaeleon II, and Chamaeleon III dark clouds. It occupies nearly all of the constellation and overlaps into

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Kashyap V, Rosner R, Harnden FR Jr, Maggio A, Micela G, Sciortino S (1994). "X-ray emission on hybrid stars: ROSAT observations of alpha Trianguli Australis and IOTA Aurigae".

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is rather consistently observed over a wide range of energies. The early high-energy end of the spectrum for this diffuse X-ray background was obtained by instruments on board

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magnetic field braking the rotation. The implied magnetic field is trillions of times stronger than Earth's field, but it's 10 to 100 times weaker than a typical magnetar.

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Using the orbiting Chandra X-ray telescope, astronomers have imaged the center of our near-twin island universe, finding evidence for a bizarre object. Like the Milky Way,

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Black holes give off radiation because matter falling into them loses gravitational energy which may result in the emission of radiation before the matter falls into the

1500: 400:, 1316, 1332, 1395, 2563, 4374, 4382, 4406, 4472, 4594, 4636, 4649, and 5128. The X-ray emission can be explained as thermal bremsstrahlung from hot gas (0.5–1.5 keV). 2417:

images show PSR J1846-0258 in Kes 75 in October 2000 (left) and June 2006 (right). The pulsar brightened in X-rays after giving off powerful outbursts earlier in 2006.

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The Perseus galaxy cluster is one of the most massive objects in the universe, containing thousands of galaxies immersed in a vast cloud of multimillion degree gas.

1807:. Observation dates: 13 pointings between 8 August 2002 and 20 October 2004. Color code: Energy (Red 0.3–1.2 keV, Green 1.2-2 keV, Blue 2–7 keV). Instrument: ACIS. 2211:~26,000 K and luminosity of ~10 erg s. Photometric observations at optical and infrared wavelengths also show a 26.5 d modulation. Of the 20 or so members of the 307:

bject (QSO) that emits baffling amounts of radio energy. This radio emission is caused by electrons spiraling (thus accelerating) along magnetic fields producing

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false-color image in X-rays between 500 eV and 1.1 keV of the Chamaeleon I dark cloud. The contours are 100 μm emission from dust measured by the IRAS satellite.

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Knigge C, Gilliland RL, Dieball A, Zurek DR, Shara MM, Long KS (2006). "A blue straggler binary with three progenitors in the core of a globular cluster?".

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are formed by the merger of smaller units of matter, such as galaxy groups or individual galaxies. The infalling material (which contains galaxies, gas and

1920: 1856:−42° 41' 41.40" in Puppis. Observation date: 4 September 2005. Color code: Energy (Red 0.4–0.7 keV; Green 0.7–1.2 keV; Blue 1.2–10 keV). Instrument: ACIS. 4672: 2525:

There is also a rather abrupt onset of X-ray emission around spectral type A7-F0, with a large range of luminosities developing across spectral class F.

3755: 3516:

Nusinov AA, Kazachevskaya TV (2006). "Extreme ultraviolet and X-ray emission of solar flares as observed from the CORONAS-F spacecraft in 2001–2003".

2662:

pole to the black circle is 3,340 km (2,080 mi). Observation dates: 10 pointings between 16 December 2003 – 13 April 2004. Instrument: HRC.

3958:

Alcalá JM; Covino E; Sterzik MF; Schmitt JHMM; Krautter J; Neuhäuser R (March 2000). "A ROSAT pointed observation of the Chamaeleon II dark cloud".

344: 5331: 5050: 2239:, characterized by short outbursts with very fast rise times (tens of minutes) and typical durations of a few hours that are associated with OB 1591:

The Draco nebula (a soft X-ray shadow) is outlined by contours and is blue-black in the image by ROSAT of a portion of the constellation Draco.

640:(IMXB) is a binary star system where one of the components is a neutron star or a black hole. The other component is an intermediate mass star. 2647:

satellite. The area of brightest X-ray emission is red. Such X-rays are not dangerous because they are absorbed by lower parts of the Earth's

2392: 2333:

is a type of neutron star with an extremely powerful magnetic field, the decay of which powers the emission of copious amounts of high-energy

2026:'s superb spectral capabilities to survey Serpens X-1. The Suzaku data confirmed the XMM-Newton result regarding the iron line in Serpens X-1. 1577:

The jet exhibited in X-rays coming from PKS 1127-145 is likely due to the collision of a beam of high-energy electrons with microwave photons.

4479: 2846: 1360: 1282:

X-ray image of Sirius A and B shows Sirius B to be more luminous than Sirius A. Whereas in the visual range, Sirius A is the more luminous.

2403:

all packed the wallop of at least 75,000 Suns. "Never before has a regular pulsar been observed to produce magnetar bursts", says Gavriil.

2177:. The material in the jet traveling from the secondary to the primary does so at 26% of light speed. The spectrum of SS 433 is affected by 205:

heated to between 10 and 10 K depending on the size of the cluster. This very hot gas emits X-rays by thermal bremsstrahlung emission, and

2018:, Bhattacharyya and Strohmayer observed Serpens X-1, which contains a neutron star and a stellar companion. Cackett and Jon Miller of the 1662:

This Chandra X-ray image reveals a large cloud of hot gas that extends throughout the Hydra A galaxy cluster. Image is 2.7 arcmin across.

2608:

By comparing the soft X-ray background with the distribution of neutral hydrogen, it is generally agreed that within the Milky Way disk,

5557: 3841: 3687: 3480:

Aschwanden MJ (2002). "Observations and models of coronal loops: From Yohkoh to TRACE, In: Magnetic coupling of the solar atmosphere".

2109:+57° 40' 00.00" is a field of view that is almost free of absorption by neutral hydrogen gas within the Milky Way. It is known as the 1321:

absorbing optical wavelength radiation before it reached Earth (although it is possible that it was recorded as a sixth magnitude star

265: 3827: 2398:

image shows the supernova Kes 75 with the young, normal pulsar, neutron star PSR J1846-0258 in the center of the blue area at the top.

5443: 2342: 4256:

Taylor AR, Young G, Peracaula M, Kenny HT, Gregory PC (1996). "An X-ray outburst from the radio emitting X-ray binary LSI+61°303".

5169: 1886:

Sagittarius A East, the spiral structure Sagittarius A West, and a very bright compact radio source at the center of the spiral,

549:

star. The dense white dwarf can accumulate gas donated from the companion. When the dwarf reaches the critical mass of 1.4

255: 202: 4987: 1342: 1108: 4665: 3027:

Podsiadlowski P, Rappaport S, Pfahl E (2001). "Evolutionary Binary Sequences for Low- and Intermediate-Mass X-ray Binaries".

637: 4401: 5273: 3712:

Cravens, T. E., Comet Hyakutake X-ray source: Charge transfer of solarwind heavy ions, Geophys. Res. Lett., 24, 105, 1997.

2249: 1056: 1047: 348: 327: 2113:. Hundreds of X-ray sources from other galaxies, some of them supermassive black holes, can be seen through this window. 5436: 4939: 4079:

Wood KS, Meekins JF, Yentis DJ, Smathers HW, McNutt DP, Bleach RD (December 1984). "The HEAO A-1 X-ray source catalog".

2657: 1658: 897:

According to theory, an object that has a mass of less than about 8% of the mass of the Sun cannot sustain significant

461:, which means that the material cannot fall in directly, but spins around the black hole. This material often forms an 4583:

Posson-Brown P, Kashyap VL, Pease DO, Drake JJ (2006). "Dark Supergiant: Chandra's Limits on X-rays from Betelgeuse".

2503: 2382: 2091: 1997: 473:

surface with high speed. In case of a neutron star, the infall speed can be a sizeable fraction of the speed of light.

2818:"BATSE finds most distant quasar yet seen in soft gamma rays Discovery will provide insight on formation of galaxies" 913:

and brown dwarfs occurs with objects that have masses below about 1% of the mass of the Sun, or 10 times the mass of

417:(ULXs) are pointlike, nonnuclear X-ray sources with luminosities above the Eddington limit of 3 × 10 W for a 20 36:

X-rays start at ~0.008 nm and extend across the electromagnetic spectrum to ~8 nm, over which Earth's atmosphere is

5324: 5106: 4898: 3339: 2135: 1638: 1334: 1311: 1258: 937:

sets up conditions for the development of a strong, tangled magnetic field near the surface. The flare observed by

414: 409: 186: 153: 114: 2921:

Feng H, Kaaret P (2006). "Spectral state transitions of the ultraluminous X-RAY sources X-1 and X-2 in NGC 1313".

5345: 5162: 5127: 5120: 4967: 4658: 4026:

Hamaguchi K, Yamauchi S, Koyama K (2005). "X-ray Study of the Intermediate-Mass Young Stars Herbig Ae/Be Stars".

2699: 2515: 2414: 2395: 2347: 2334: 2277: 2065: 1929: 1925: 1766: 1303: 963: 938: 527: 163: 87: 1636:

Within the constellations Orion and Eridanus and stretching across them is a soft X-ray "hot spot" known as the

811:

demonstrate for most flares observed by CORONAS-F in 2001–2003 UV radiation preceded X-ray emission by 1–10 min.

609:

star HD 77581. The X-ray emission of the neutron star is caused by the capture and accretion of matter from the

485:

in very short timescales. The variation in luminosity can provide information about the size of the black hole.

5567: 5368: 5134: 2643:

This composite image contains the first picture of the Earth in X-rays, taken in March 1996, with the orbiting

2572: 1621: 1416: 842:

X-ray emission has been detected from PG 1658+441, a hot, isolated, magnetic white dwarf, first detected in an

721: 233: 4566: 113:

Furthermore, celestial entities in space are discussed as celestial X-ray sources. The origin of all observed

3751: 1948:−33° 42' 58.80" in Sculptor. Color code: Ultraviolet (blue), Optical (green), X-ray (purple), Infrared (red). 807:

Variations of solar-flare emission in soft X-rays (10–130 nm) and EUV (26–34 nm) recorded on board

481:

are generated when the material hits their surfaces. X-ray emission from black holes is variable, varying in

5501: 5229: 5015: 4874: 4853: 4812: 4776: 4744: 2609: 2320: 2296: 2285: 2061: 1937: 1791: 1385: 1295: 855: 776: 578: 381: 292: 91: 67: 2817: 1748: 650:

overflow. X-1 is the prototype for the massive X-ray binaries although it falls on the borderline, ~2

5562: 5282: 5155: 5148: 5071: 4865: 3900:

Feigelson ED, Lawson WA (October 2004). "An X-ray census of young stars in the Chamaeleon I North Cloud".

2374: 2366: 2057: 2019: 2008: 1985: 1933: 1607: 1443: 1299: 1210:

magnetized bubble of extremely high-energy electrons that emit radio waves. Image is 4.2 arcmin per side.

1096:, striving to understand the generation of X-rays by the apparent source helps to understand the Sun, the 1039: 598: 558:, a thermonuclear explosion ensues. As each Type Ia shines with a known luminosity, Type Ia are used as " 508:

provided observational evidence that Type Ia are the explosion of a white dwarf orbiting a red giant star.

469:

and neutron stars, but in these the infalling gas releases additional energy as it slams against the high-

377: 2974:

Mauche CW, Liedahl DA, Akiyama S, Plewa T (2007). "Hydrodynamic and Spectral Simulations of HMXB Winds".

1882:(or Sgr A) is a complex at the center of the Milky Way. It consists of three overlapping components, the 5252: 4946: 4884: 4737: 4707: 4288: 3489: 2409: 1737: 1725: 1671: 1625: 1140: 1120: 711: 691: 312: 137: 5416: 1795:

Chandra observations of the central regions of the Perseus galaxy cluster. Image is 284 arcsec across.

1294:

Cassiopeia A: a false color image composited of data from three sources. Red is infrared data from the

1080:

constellations are areas of the sky. Each of these contains remarkable X-ray sources. Some of them are

830:. The white dwarf is surrounded by an expanding shell of gas in an object known as a planetary nebula. 565:

SN 2005ke is the first Type Ia supernova detected in X-ray wavelengths, and it is much brighter in the

2284:. These loops and rings are generated by variations in the rate at which material is ejected from the 2003:"This is fundamental physics", says Sudip Bhattacharyya also of NASA's Goddard Space Flight Center in 1023:

Some of the detected X-rays, originating from solar system bodies other than the Sun, are produced by

5244: 5176: 4994: 4932: 4723: 4700: 4693: 4613: 4524: 4416: 4369: 4342: 4302: 4265: 4221: 4162: 4123: 4088: 4045: 3998: 3967: 3919: 3877: 3790: 3737: 3624: 3606:"Max Planck Institute for Extraterrestrial Physics: Super Soft X-ray Sources – Discovered with ROSAT" 3577: 3525: 3446: 3402: 3365: 3315: 3236: 3183: 3136: 3089: 3046: 2993: 2940: 2878: 2782: 2737: 2440: 1752: 843: 48: 3650: 791:

at their footpoints. Coronal loops populate both active and quiet regions of the solar surface. The

779:

of the Sun. These highly structured and elegant loops are a direct consequence of the twisted solar

5375: 5317: 5113: 5064: 4960: 4907: 4730: 2564: 2538: 2004: 1471: 393: 308: 4483: 2315:

Magnetar SGR 1900+14 is in the exact center of the image, which shows a surrounding ring of gas 7

2126: 2046:. Color code: Energy (red 0.4-2keV, green 2-8keV, blue 4-8keV). Image is about 50 arcmin per side. 5516: 5506: 5404: 5303: 5008: 4978: 4925: 4860: 4808: 4783: 4584: 4540: 4514: 4332: 4292: 4061: 4035: 3935: 3909: 3808: 3541: 3462: 3418: 3392: 3331: 3305: 3252: 3226: 3199: 3173: 3105: 3062: 3036: 3009: 2983: 2956: 2930: 2896: 2798: 2772: 2679: 2182: 2023: 1431: 1132: 320: 316: 141: 2288:

in jets. The distribution of loops suggests that minor eruptions occur every six million years.

4198: 1139:

Multiple X-ray sources have been detected in the Andromeda Galaxy, using observations from the

808: 748: 5526: 5521: 5511: 5310: 5296: 5095: 5080: 5057: 5001: 4769: 4432: 3845: 2842: 2675: 2644: 2621: 2427: 2377:

had a long period of low emissions, except the significant burst in 1979, and a couple after.

2212: 2198: 2171: 1883: 1864: 1552: 1546: 1318: 1314: 602: 538: 523: 494: 441: 133: 71: 3738:"Hubble site news center: Fireworks Near a Black Hole in the Core of Seyfert Galaxy NGC 4151" 3664: 2323:. The magnetar itself is not visible at this wavelength, but it has been seen in X-ray light. 269:

years away in a 12 to 15-billion year-old universe (using z=1 as 5 billion light years).

5215: 5194: 5029: 5022: 4621: 4532: 4424: 4377: 4269: 4229: 4225: 4170: 4131: 4096: 4053: 4006: 3971: 3927: 3881: 3798: 3723: 3691: 3632: 3585: 3533: 3454: 3410: 3323: 3319: 3244: 3191: 3144: 3097: 3054: 3001: 2948: 2886: 2790: 2745: 2741: 2311: 2163: 1953: 1915: 1867:(SNR) about 10 light-years in diameter. The supernova occurred approximately 3700 years ago. 1843: 1690:

Chandra image of two galaxies (Arp 270) in the early stage of a merger in the constellation

1616:

This ROSAT PSPC false-color image is of a portion of a nearby stellar wind superbubble (the

1112: 1073: 831: 783:

flux within the solar body. The population of coronal loops can be directly linked with the

458: 125: 37: 1989:

larger than 18 to 20.5 miles across, results that agree with other types of measurements."

1971: 1503:, located in the Chamaeleon III dark cloud, is the brightest Herbig Ae/Be star in the sky. 1290: 646:

is composed of a neutron star accreting matter from a normal star (HZ Her) probably due to

5361: 5036: 4953: 4891: 4846: 4790: 3502: 3164:

S. K. Antiochos; et al. (1999). "The Dynamic Formation of Prominence Condensations".

2686:. These electrons move along the Earth's magnetic field and eventually strike the Earth's 2519: 2446: 2236: 2102: 1941: 1895: 1849: 1796: 1786: 1703: 1663: 1534: 1211: 1190: 1167: 1116: 1093: 967: 559: 2763:

Clowe D; et al. (2006). "A Direct Empirical Proof of the Existence of Dark Matter".

1193:. The cluster is filled with a vast cloud of 50 MK gas that radiates strongly in X rays. 110:, although most of the X-ray brightness of the Moon arises from reflected solar X-rays. 17: 4617: 4528: 4420: 4373: 4346: 4306: 4233: 4166: 4127: 4092: 4049: 4002: 3923: 3794: 3628: 3581: 3529: 3450: 3406: 3369: 3240: 3187: 3140: 3093: 3050: 2997: 2944: 2882: 2786: 2749: 2052: 1384:

of how a star can produce such hot and intense X-rays," says Prof. Kris Davidson of the

673:

The first extrasolar X-ray source was discovered on 12 June 1962. This source is called

5491: 5476: 5208: 5141: 5043: 4639:

Kupperian JE Jr; Friedman H (1958). "Experiment research US progr. for IGY to 1.7.58".

2544: 2457: 2423: 2269: 2245: 1899: 1887: 1774: 1594:

Abell 2256 is a galaxy cluster of more than 500 galaxies. The double structure of this

1530: 1517: 1326: 1261: 1186: 898: 863: 477: 462: 365: 360: 226: 222: 198: 194: 167: 129: 99: 59: 4428: 2571:

of hot gas, by X-ray satellite telescopes. The Sun is currently traveling through the

2391: 2280:

indicate the presence of loops and rings in the hot X-ray emitting gas that surrounds

1612: 5551: 5266: 4544: 4065: 3545: 3466: 3335: 3109: 2900: 2683: 2511: 2469: 2203: 2186: 2178: 2080: 1903: 1879: 1496: 1495:"Chamaeleon III appears to be devoid of current star-formation activity." HD 104237 ( 1484: 1467: 1364: 1322: 1246: 454: 369: 206: 118: 3939: 3422: 3256: 3066: 3013: 2960: 1396: 514: 330:(CGRO) is the Burst and Transient Source Experiment (BATSE) which detects in the 20 5486: 5471: 5222: 5201: 4819: 3812: 3203: 2834: 2802: 2576: 2548: 2499: 2483: 2476: 2370: 2224: 2174: 2151: 2110: 2043: 1568: 1359: 1219: 1024: 772: 768: 695: 674: 668: 643: 622: 610: 103: 95: 2090:+69° 40′ 46.0″. It was detected in January 2006 by the 1454: 1241: 1174:−52° 12' 21". Observation date: 30 August 1999. Instrument: ACIS. Aka: Cl 1409+524 1127: 124:

A combination of many unresolved X-ray sources is thought to produce the observed

4440: 2166:

with the primary either a black hole or neutron star and the secondary is a late

5289: 2568: 2350:. As of 2003, they are the most magnetic objects ever detected in the universe. 2167: 2159: 2143: 2106: 1945: 1853: 1800: 1720: 1709: 1667: 1380: 1368: 1354: 1215: 1171: 1060: 1043: 906: 892: 867: 827: 820: 784: 741: 566: 542: 466: 218: 190: 83: 79: 63: 5428: 3605: 2599: 993: 5481: 5259: 5236: 4716: 3828:"Universe Today – Fermi Telescope Makes First Big Discovery: Gamma Ray Pulsar" 3537: 3458: 3327: 3149: 3124: 2687: 2648: 2639: 2556: 2552: 2507: 2450: 2316: 2300: 2281: 2265: 2240: 2220: 2098: 2083: 2015: 1975: 1686: 1522: 1512: 1205: 1143: 1085: 934: 879: 686: 651: 647: 606: 550: 503: 482: 446: 436: 418: 339: 4114:

Ouellette GA (1967). "Development of a catalogue of galactic x-ray sources".

5536: 5496: 5460: 5354: 4681: 4011: 3986: 3080:

Priedhorsky WC, Holt SS (1987). "Long-term cycles in cosmic X-ray sources".

2560: 2491: 2461: 2362: 2358: 2338: 1699: 1691: 1345:

detected the pulsar was emitting gamma ray radiation, the first of its kind.

1338: 1154: 943: 902: 870:. This requires a flow of material sufficiently high to sustain the fusion. 835: 682: 546: 264: 158: 4436: 4040: 3217:

Steeghs, D.; Casares, J (2002). "The Mass Donor of Scorpius X-1 Revealed".

1875: 1446:. The mean density of X-ray sources is about one source per square degree. 1182: 1163: 920: 3651:"XMM-Newton weighs up a rare white dwarf and finds it to be a heavyweight" 3356:

Gould RJ, Burbidge GR (1965). "High energy cosmic photons and neutrinos".

2038: 716: 4589: 4297: 3914: 3397: 3310: 3231: 3178: 3041: 3005: 2935: 2777: 2593: 2589: 2495: 2329: 2299:(AGN) that is a strong source of multiwavelength radiation, particularly 1860: 1838: 1770: 1761: 1586: 1412: 1401: 1400:

Two supermassive black holes spiraling towards merger near the center of

1254: 1236: 1097: 1081: 796: 788: 780: 678: 613:

of the supergiant companion. Vela X-1 is the prototypical detached HMXB.

594: 589: 396:(NGCs) have been observed to be X-ray bright due to hot gaseous coronae: 210: 175: 121:

or gas at coronal cloud temperatures for however long or brief a period.

983: 755: 182:) = 0.3, meaning its light has wavelengths stretched by a factor of 1.3. 4360:

Baade W, Minkowski R (1954). "On the Identification of Radio Sources".

3101: 2076: 1966: 1804: 1678:

A large cloud of hot gas extends throughout the Hydra A galaxy cluster.

1372: 1279: 1197:

observed that the central galaxy is a strong, complex source of X rays.

1194: 914: 519: 470: 397: 3636: 5384: 4457: 3803: 3778: 2216: 2155: 2147: 2131: 1273: 1178: 1159: 1089: 910: 847: 792: 725: 288: 283: 245: 214: 171: 52: 627: 254: 209:

from metals (in astronomy, 'metals' often means all elements except

201:. The infalling gas collides with gas already in the cluster and is 32: 4625: 4536: 4381: 4175: 4151:"The Distribution of Galactic X-Ray Sources from Scorpio to Cygnus" 4150: 4135: 4100: 4057: 3931: 3590: 3565: 3414: 3248: 3195: 3058: 2952: 2891: 2866: 2794: 2260: 449:, which was the first strong black hole candidate to be discovered. 4519: 4337: 2988: 2671: 2656: 2638: 2598: 2445:

During the solar cycle, as shown in the sequence of images of the

2354: 2125: 2037: 1919: 1842: 1818: 1790: 1747: 1729: 1719: 1685: 1657: 1611: 1595: 1567: 1516: 1459: 1453: 1439: 1419: 1358: 1240: 1204: 1153: 1107: 801: 760: 58:

Several types of astrophysical objects emit X-rays. They include

1993: 1924:

This image combines data from four different observatories: the

1629: 1435: 1162:, a strongly X-ray emitting galaxy cluster in the constellation 107: 75: 5432: 4654: 5531: 4826: 3985:

Yamauchi S, Hamaguchi K, Koyama K, Murakami H (October 1998).

2678:

satellite. Energetically charged particles from the Sun cause

2353:

On 5 March 1979, after dropping probes into the atmosphere of

1557: 1371:

exhibits a superstar at its center as seen in this image from

1077: 859: 707: 373: 335: 331: 4458:"HLD user program, at Dresden High Magnetic Field Laboratory" 2551:

from young clusters of stars (often with giant or supergiant

1166:. The cluster is filled with gas. Image is 42 arcsec across. 4650: 4197:

Gibb M, Bhattacharyya S, Strohmayer T, Cackett E, Miller J.

948: 1650:, a 25° area of interlocking arcs of Hα emitting filaments. 1573:

in Crater. Observation date: 28 May 2000. Instrument: ACIS.

795:

Soft X-ray Telescope (SXT) observed X-rays in the 0.25–4.0

787:, it is for this reason coronal loops are often found with 4199:"Astronomers Pioneer New Method for Probing Exotic Matter" 3623:. AIP Conference Proceedings. Vol. 637. p. 333. 2449:, the Sun is almost X-ray dark, almost an X-ray variable. 1027:. Scattered solar X-rays provide an additional component. 862:. Super soft X-rays are believed to be produced by steady 924:

Chandra image of LP 944-20 before flare and during flare.

720:

The corona of the Sun as seen in the X-ray region of the

170:. Exposure time was 140 hours. The scale is shown in mega 51:

with physical properties which result in the emission of

1537:. It is one of the most massive objects in the universe. 858:(SSXS) radiates soft X-rays in the range of 0.09 to 2.5 465:. Similar luminous accretion disks can also form around 4567:"Powerful Explosions Suggest Neutron Star Missing Link" 2373:, located 20,000 light-years away in the constellation 1732:

satellite during the All-Sky Survey phase in 1990–1991.

834:

seem to mark the transition of a medium mass star from

724:

on 8 May 1992 by the soft X-ray telescope on board the

677:, the first X-ray source found in the constellation of 2547:

gas, in the temperature range 10 – 10 K emits X-rays.

2543:

The Hot Ionized Medium (HIM), sometimes consisting of

1724:

On the right is the visual image of the constellation

1674:. Observation date: 30 October 1999. Instrument: ACIS. 1521:

Chandra X-ray Observatory image of the galaxy cluster

2674:

in X-rays was taken in March 1996, with the orbiting

2341:. The theory regarding these objects was proposed by 866:

on a white dwarf's surface of material pulled from a

3566:"X-rays from the magnetic white dwarf PG 1658 + 441" 2502:. There is an apparent X-ray "dividing line" in the 2369:. And, Konus detected another source in March 1979: 5186: 5094: 4977: 4917: 4838: 4800: 4761: 4754: 3987:"ASCA Observations of the Chamaeleon II Dark Cloud" 3564:Pravdo SH, Marshall FE, White NE, Giommi P (1986). 752:observations have generally only set upper limits. 4323:Sidoli L (2008). "Transient outburst mechanisms". 901:in its core. This marks the dividing line between 759:This is a false-color, 3-layer composite from the 698:, while the donor star is only 0.42 solar masses. 1046:was passing through the constellation Libra when 476:In some neutron star or white dwarf systems, the 368:are a class of galaxies with nuclei that produce 3895: 3893: 3891: 2464:. The cause of the X-ray deficiency may involve 2022:, along with Bhattacharyya and Strohmayer, used 804:coronal loops radiating in the EUV wavelengths. 681:, located in the direction of the center of the 545:in orbit around either another white dwarf or a 3779:"Did Flamsteed see the Cassiopeia A supernova?" 2728:Morrison P (1967). "Extrasolar X-ray Sources". 2154:, with an often resolvable pair of radio jets. 1404:, some 25,000 light years away from each other. 106:bodies emit X-rays, the most notable being the 4395: 4393: 4391: 3842:"Chandra Takes X-ray Image of Repeat Offender" 3752:"The Dog Star, Sirius, and its Tiny Companion" 2207:around a rapidly rotating B0 Ve star, with a T 1957:rim of the galaxy as can be seen in the inset. 1100:as a whole, and how these affect us on Earth. 5444: 4666: 4400:Kouveliotou C, Duncan RC, Thompson C (2003). 3953: 3951: 3949: 3621:Activity of the super-soft X-ray source V Sge 2460:Betelgeuse, hardly any X-rays are emitted by 1736:In the adjacent images are the constellation 1076:has been divided into 88 constellations. The 747:Solar flares usually follow the solar cycle. 197:as it falls into the cluster's gravitational 8: 3125:"Nobel Lecture: The dawn of x-ray astronomy" 1940:(infrared/red). Image is 160 arcsec across. 1227:high-energy electrons that emit radio waves. 659:, between high- and low-mass X-ray binaries. 4287:. ESA Special Publications. Vol. 604. 4212:Margon B (1984). "Observations of SS 433". 4149:Gursky H, Gorenstein P, Giacconi R (1967). 3682: 3680: 3678: 3676: 3674: 2634: 2042:Chandra mosaic of the X-ray sources in the 2033: 978: 846:IPC observation and later identified in an 498: 249: 5451: 5437: 5429: 4758: 4673: 4659: 4651: 4192: 4190: 4188: 4186: 2860: 2858: 2723: 2721: 2719: 2717: 2715: 1411:is a galaxy cluster, containing a galaxy ( 4588: 4578: 4576: 4518: 4336: 4318: 4316: 4296: 4251: 4249: 4247: 4245: 4243: 4174: 4039: 4010: 3913: 3802: 3589: 3559: 3557: 3555: 3396: 3309: 3230: 3177: 3148: 3040: 2987: 2934: 2890: 2865:Forman W, Jones C, Tucker W (June 1985). 2839:Galaxies in the Universe: An Introduction 2776: 2482:strong attenuation by an overlying thick 2319:across in infrared light, as seen by the 4560: 4558: 4556: 4554: 3284: 3282: 3280: 3278: 3276: 3274: 3272: 3270: 3268: 3266: 2867:"Hot coronae around early-type galaxies" 2829: 2827: 2408: 2390: 2310: 2259: 2235:There are a growing number of recurrent 2231:Supergiant fast X-ray transients (SFXTs) 2051: 1970: 1874: 1598:image shows the merging of two clusters. 1395: 1289: 1126: 1038: 992: 982: 919: 754: 715: 694:(LMXB); the neutron star is roughly 1.4 626: 562:" to measure distances in the universe. 513: 502: 440: 345:Energetic Gamma Ray Experiment Telescope 263: 253: 157: 31: 2711: 2612:are absorbed by this neutral hydrogen. 2268:jet of matter ejected from M87 at near 1712:+32° 59′ 6″. 1551:From the Chandra X-ray analysis of the 1302:, and blue and green are data from the 917:. These objects cannot fuse deuterium. 632:orbital period of the system, 1.7 days. 132:, either magnetic or ordinary Coulomb, 4285:Proceedings of the X-ray Universe 2005 3754:. Hubble News Desk. 13 December 2005. 3498: 3487: 2916: 2914: 2912: 2910: 2682:and energize electrons in the Earth's 851:abundance in white dwarf atmospheres. 771:form the basic structure of the lower 2575:, a denser region in the low-density 1898:is at 1745–2900 which corresponds to 1333:CTA 1 is another SNR X-ray source in 1264:has a massive black hole in its core. 1222:. Observation date: 30 November 2003. 1088:at the centers of galaxies. Some are 221:are collisionless and quickly become 128:. The X-ray continuum can arise from 117:is in, near to, or associated with a 7: 5412: 3688:"X-rays from a Brown Dwarf's Corona" 3291:"X-ray astronomy of stellar coronae" 2490:Prominent bright red giants include 1466:The Chamaeleon I (Cha I) cloud is a 4234:10.1146/annurev.aa.22.090184.002451 2750:10.1146/annurev.aa.05.090167.001545 2295:The galaxy also contains a notable 601:(HMXB) system, associated with the 27:Astronomical object emitting X-rays 1932:satellite (ultraviolet/blue); the 1533:Abell 2142 emits X-rays and is in 1298:, orange is visible data from the 380:(AGN), and are thought to contain 287:) is a very energetic and distant 25: 4429:10.1038/scientificamerican0203-34 3758:from the original on 12 July 2006 5411: 5400: 5399: 5170:Southern African Large Telescope 3724:"NASA's Swift Spies Comet Lulin" 1123:light (released 5 January 2016). 70:(AGN), galactic objects such as 4325:37th Cospar Scientific Assembly 3690:. 14 April 2003. Archived from 2837:; Gallagher, J. S. III (2007). 2690:, producing the X-ray emission. 1644:Eridanus Soft X-ray Enhancement 1343:Fermi Gamma-ray Space Telescope 3826:Atkinson N (17 October 2008). 2841:. Cambridge University Press. 1487:K1, is closest to 4U 1302–77. 1470:and one of the nearest active 953:Chandra observation of TWA 5B. 638:intermediate-mass X-ray binary 1: 2130: 1698:Arp260 is an X-ray source in 1057:Swift Gamma-Ray Burst Mission 728:solar observatory spacecraft. 685:. Scorpius X-1 is some 9,000 349:Compton Gamma Ray Observatory 328:Compton Gamma Ray Observatory 4214:Annu. Rev. Astron. Astrophys 2730:Annu. Rev. Astron. Astrophys 1902:, very near to radio source 909:. The dividing line between 376:gas. They are a subclass of 3619:Simon V, Mattei JA (2002). 2475:a suppression by competing 2383:Rossi X-ray Timing Explorer 2348:the field surrounding Earth 2092:Rossi X-ray Timing Explorer 1998:Goddard Space Flight Center 1185:is one of the most distant 839:temperatures of ~20,000 K. 457:. The infalling matter has 415:Ultraluminous X-ray sources 404:Ultraluminous X-ray sources 45:Astrophysical X-ray sources 5584: 5558:Astronomical X-ray sources 2636: 2619: 2536: 2438: 2337:, particularly X-rays and 2196: 2158:is one of the most exotic 2035: 1964: 1913: 1836: 1784: 1639:Orion-Eridanus Superbubble 1605: 1584: 1544: 1510: 1352: 1271: 1234: 1094:astronomical X-ray sources 980: 890: 818: 705: 666: 620: 605:source 4U 0900-40 and the 587: 576: 500: 492: 434: 410:Ultraluminous X-ray source 407: 358: 295:(AGN). QSO 0836+7107 is a 279:quasi-stellar radio source 251: 243: 225:, orbiting in the cluster 154:Galaxy groups and clusters 151: 142:inverse Compton scattering 115:astronomical X-ray sources 88:cataclysmic variable stars 5467: 5394: 5163:Large Binocular Telescope 5128:Extremely Large Telescope 5121:Extremely large telescope 4688: 3538:10.1134/S0038094606020043 3459:10.1134/S003809460602002X 3328:10.1007/s00159-004-0023-2 3150:10.1103/RevModPhys.75.995 3029:The Astrophysical Journal 2700:Astronomical radio source 2670:The first picture of the 2533:X-ray interstellar medium 2516:Alpha Trianguli Australis 2335:electromagnetic radiation 2150:that is a radio emitting 2146:is a smaller cousin of a 1952:The unusual shape of the 1930:Galaxy Evolution Explorer 1926:Chandra X-ray Observatory 1767:Chandra X-ray Observatory 1491:Chamaeleon III dark cloud 1422:spiraling towards merger. 1304:Chandra X-ray Observatory 1059:satellite was monitoring 964:Chandra X-ray Observatory 573:X-ray emission from stars 528:Chandra X-ray Observatory 164:Chandra X-ray Observatory 18:Astronomical X-ray source 5135:Gran Telescopio Canarias 4081:Astrophys. J. Suppl. Ser 2583:Diffuse X-ray background 2573:Local Interstellar Cloud 1829:0517-456 and 3U 0510-44. 1479:Chamaeleon II dark cloud 1417:supermassive black holes 1379:Three structures around 1337:. A pulsar in the CTA 1 722:electromagnetic spectrum 597:is a pulsing, eclipsing 489:Supernova remnants (SNR) 382:supermassive black holes 347:(EGRET) also aboard the 338:range. QSO 0836+7107 or 234:statistical significance 92:super soft X-ray sources 5502:Extragalactic astronomy 5230:Astrology and astronomy 4940:Gravitational radiation 4270:1996A&A...305..817T 4226:1984ARA&A..22..507M 3972:2000A&A...355..629A 3882:1995A&AS..114..109A 3358:Annales d'Astrophysique 3320:2004A&ARv..12...71G 2742:1967ARA&A...5..325M 2510:as they cross from the 2321:Spitzer Space Telescope 2297:active galactic nucleus 2286:supermassive black hole 2213:Be X-ray binary systems 1938:Spitzer Space Telescope 1450:Chamaeleon I dark cloud 1386:University of Minnesota 1296:Spitzer Space Telescope 1068:Celestial X-ray sources 856:super soft X-ray source 579:Stellar X-ray astronomy 293:active galactic nucleus 5149:Hubble Space Telescope 4641:IGY Rocket Report Ser. 3991:Publ. Astron. Soc. Jpn 3497:Cite journal requires 3437:CORONAS-F satellite". 2663: 2652: 2605: 2555:surrounding them) and 2514:to become red giants. 2418: 2399: 2367:Large Magellanic Cloud 2324: 2273: 2139: 2069: 2047: 2020:University of Michigan 2009:University of Maryland 1986:University of Michigan 1980: 1949: 1934:Hubble Space Telescope 1891: 1857: 1825: 1808: 1756: 1733: 1695: 1675: 1633: 1574: 1526: 1472:star formation regions 1463: 1405: 1376: 1307: 1300:Hubble Space Telescope 1250: 1223: 1175: 1136: 1124: 1052: 999: 988: 954: 925: 765: 729: 633: 599:high-mass X-ray binary 530: 509: 450: 378:active galactic nuclei 270: 259: 183: 68:active galactic nuclei 41: 5253:Astroparticle physics 4988:Australian Aboriginal 4480:"The Brightest Blast" 4289:European Space Agency 4012:10.1093/pasj/50.5.465 3518:Solar System Research 3439:Solar System Research 2976:Prog Theor Phys Suppl 2660: 2642: 2602: 2431:ramp up in activity." 2412: 2394: 2314: 2276:Observations made by 2263: 2170:. SS 433 lies within 2129: 2055: 2041: 1974: 1936:(visible/green); the 1923: 1878: 1846: 1822: 1794: 1751: 1723: 1689: 1661: 1618:Orion-Eridanus Bubble 1615: 1571: 1520: 1457: 1399: 1362: 1293: 1244: 1208: 1157: 1146:orbiting observatory. 1130: 1111: 1042: 996: 986: 952: 923: 758: 719: 712:Solar X-ray astronomy 692:low-mass X-ray binary 630: 541:is an explosion of a 517: 506: 444: 388:X-ray bright galaxies 372:emission from highly 313:synchrotron radiation 267: 257: 161: 138:synchrotron radiation 35: 5245:Astronomers Monument 5177:Very Large Telescope 4724:Astronomical symbols 3298:Astron Astrophys Rev 3006:10.1143/PTPS.169.196 2565:stellar wind bubbles 2520:Dividing Line models 2117:Exotic X-ray sources 1620:) stretching across 1608:X-rays from Eridanus 217:). The galaxies and 187:Clusters of galaxies 134:black-body radiation 49:astronomical objects 5459:Major subfields of 5318:List of astronomers 4731:Astronomical object 4618:1994ApJ...431..402K 4529:2008ApJ...680..545M 4421:2003SciAm.288b..34K 4374:1954ApJ...119..215B 4347:2008cosp...37.2892S 4307:2006ESASP.604..165N 4167:1967ApJ...150L..75G 4128:1967AJ.....72..597O 4093:1984ApJS...56..507W 4050:2005ApJ...618..360H 4003:1998PASJ...50..465Y 3924:2004ApJ...614..267F 3795:1980Natur.285..132H 3694:on 30 December 2010 3629:2002AIPC..637..333S 3582:1986ApJ...300..819P 3530:2006SoSyR..40..111N 3451:2006SoSyR..40...93Z 3407:2006ApJ...641..281K 3370:1965AnAp...28..171G 3241:2002ApJ...568..273S 3188:1999ApJ...512..985A 3141:2003RvMP...75..995G 3123:Giacconi R (2003). 3094:1987SSRv...45..291P 3051:2002ApJ...565.1107P 2998:2007PThPS.169..196M 2945:2006ApJ...650L..75F 2883:1985ApJ...293..102F 2787:2006ApJ...648L.109C 2539:Interstellar medium 2162:observed. It is an 2005:Greenbelt, Maryland 1803:+41° 30' 37.00" in 1259:intermediate spiral 1253:The X-ray landmark 1218:+74° 14' 51.00" in 518:X-ray image of the 394:early-type galaxies 5517:Physical cosmology 5507:Galactic astronomy 5304:Physical cosmology 4041:astro-ph/0406489v1 3777:Hughes DW (1980). 3345:on 11 August 2011. 3102:10.1007/BF00171997 2664: 2653: 2616:X-ray dark planets 2606: 2468:a turn-off of the 2419: 2400: 2325: 2274: 2140: 2070: 2048: 1981: 1950: 1892: 1858: 1826: 1809: 1757: 1734: 1696: 1676: 1634: 1575: 1527: 1464: 1432:Chamaeleon complex 1406: 1377: 1308: 1251: 1249:image of NGC 4151. 1224: 1176: 1137: 1125: 1053: 1019:X-ray fluorescence 1000: 989: 955: 926: 766: 730: 634: 531: 510: 451: 271: 260: 184: 72:supernova remnants 42: 5545: 5544: 5537:Stellar astronomy 5527:Planetary science 5522:Planetary geology 5512:Orbital mechanics 5426: 5425: 5311:Quantum cosmology 5297:Planetary geology 5090: 5089: 4801:Celestial subject 4486:on 5 October 2008 3960:Astron. Astrophys 3870:Astron. Astrophys 3637:10.1063/1.1518226 2848:978-0-521-67186-6 2668: 2667: 2622:X-ray dark planet 2610:super soft X-rays 2428:McGill University 2199:Be X-ray binaries 2193:Be X-ray binaries 2074: 2073: 1865:supernova remnant 1753:Stephan's Quintet 1553:Antennae Galaxies 1547:Antennae Galaxies 1499:A4e) observed by 1319:interstellar dust 1181:(Cl 1409+524) in 1158:Chandra image of 1117:high-energy X-ray 1004: 1003: 777:transition region 539:Type Ia supernova 535: 534: 495:Supernova remnant 445:Chandra image of 275: 274: 16:(Redirected from 5575: 5453: 5446: 5439: 5430: 5419: 5415: 5414: 5407: 5403: 5402: 5387: 5378: 5371: 5364: 5357: 5348: 5341: 5334: 5332:Medieval Islamic 5327: 5320: 5313: 5306: 5299: 5292: 5285: 5276: 5269: 5262: 5255: 5248: 5239: 5232: 5225: 5218: 5216:Astroinformatics 5211: 5204: 5197: 5195:Archaeoastronomy 5179: 5172: 5165: 5158: 5156:Keck Observatory 5151: 5144: 5137: 5130: 5123: 5116: 5109: 5083: 5074: 5067: 5060: 5053: 5051:Medieval Islamic 5046: 5039: 5032: 5025: 5018: 5011: 5004: 4997: 4990: 4970: 4963: 4956: 4949: 4942: 4935: 4928: 4910: 4901: 4894: 4887: 4880: 4878: 4870: 4868: 4856: 4849: 4829: 4822: 4815: 4793: 4786: 4779: 4772: 4759: 4747: 4740: 4733: 4726: 4719: 4710: 4703: 4696: 4675: 4668: 4661: 4652: 4645: 4644: 4636: 4630: 4629: 4601: 4595: 4594: 4592: 4590:astro-ph/0606387 4580: 4571: 4570: 4565:Naeye R (2008). 4562: 4549: 4548: 4522: 4502: 4496: 4495: 4493: 4491: 4482:. Archived from 4475: 4469: 4468: 4466: 4464: 4454: 4448: 4447: 4446:on 11 June 2007. 4445: 4439:. Archived from 4406: 4397: 4386: 4385: 4357: 4351: 4350: 4340: 4320: 4311: 4310: 4300: 4298:astro-ph/0511088 4280: 4274: 4273: 4258:Astron Astrophys 4253: 4238: 4237: 4209: 4203: 4202: 4194: 4181: 4180: 4178: 4146: 4140: 4139: 4111: 4105: 4104: 4076: 4070: 4069: 4043: 4023: 4017: 4016: 4014: 3982: 3976: 3975: 3955: 3944: 3943: 3917: 3915:astro-ph/0406529 3897: 3886: 3885: 3864: 3858: 3857: 3855: 3853: 3844:. Archived from 3838: 3832: 3831: 3823: 3817: 3816: 3806: 3804:10.1038/285132a0 3774: 3768: 3767: 3765: 3763: 3748: 3742: 3741: 3734: 3728: 3727: 3719: 3713: 3710: 3704: 3703: 3701: 3699: 3684: 3669: 3668: 3661: 3655: 3654: 3647: 3641: 3640: 3616: 3610: 3609: 3602: 3596: 3595: 3593: 3561: 3550: 3549: 3513: 3507: 3506: 3500: 3495: 3493: 3485: 3477: 3471: 3470: 3433: 3427: 3426: 3400: 3398:astro-ph/0511645 3380: 3374: 3373: 3353: 3347: 3346: 3344: 3338:. Archived from 3313: 3311:astro-ph/0406661 3295: 3289:Güdel M (2004). 3286: 3261: 3260: 3234: 3232:astro-ph/0107343 3214: 3208: 3207: 3181: 3179:astro-ph/9808199 3161: 3155: 3154: 3152: 3120: 3114: 3113: 3077: 3071: 3070: 3044: 3042:astro-ph/0107261 3035:(2): 1107–1133. 3024: 3018: 3017: 2991: 2971: 2965: 2964: 2938: 2936:astro-ph/0608066 2918: 2905: 2904: 2894: 2862: 2853: 2852: 2831: 2822: 2821: 2813: 2807: 2806: 2780: 2778:astro-ph/0608407 2771:(2): L109–L113. 2760: 2754: 2753: 2725: 2635: 2435:X-ray dark stars 2237:X-ray transients 2164:eclipsing binary 2089: 2034: 1954:Cartwheel Galaxy 1916:Cartwheel Galaxy 1708: 1670:−12° 05' 45" in 1646:, or simply the 1363:Classified as a 1191:X-ray telescopes 1113:Andromeda Galaxy 1074:celestial sphere 979: 975:X-ray reflection 868:binary companion 832:Planetary nebula 560:standard candles 499: 459:angular momentum 366:Seyfert galaxies 355:Seyfert galaxies 250: 126:X-ray background 21: 5583: 5582: 5578: 5577: 5576: 5574: 5573: 5572: 5568:X-ray astronomy 5548: 5547: 5546: 5541: 5532:Solar astronomy 5463: 5457: 5427: 5422: 5410: 5398: 5390: 5383: 5374: 5367: 5362:X-ray telescope 5360: 5353: 5344: 5337: 5330: 5323: 5316: 5309: 5302: 5295: 5288: 5281: 5272: 5265: 5258: 5251: 5242: 5235: 5228: 5221: 5214: 5207: 5200: 5193: 5182: 5175: 5168: 5161: 5154: 5147: 5140: 5133: 5126: 5119: 5112: 5105: 5097: 5086: 5079: 5070: 5063: 5056: 5049: 5042: 5035: 5028: 5021: 5014: 5007: 5000: 4993: 4986: 4973: 4968:Multi-messenger 4966: 4959: 4952: 4945: 4938: 4931: 4924: 4913: 4906: 4897: 4890: 4883: 4876: 4873: 4864: 4859: 4852: 4845: 4834: 4825: 4818: 4807: 4796: 4791:Space telescope 4789: 4782: 4775: 4768: 4750: 4743: 4736: 4729: 4722: 4715: 4706: 4699: 4692: 4684: 4679: 4649: 4648: 4638: 4637: 4633: 4603: 4602: 4598: 4582: 4581: 4574: 4564: 4563: 4552: 4504: 4503: 4499: 4489: 4487: 4477: 4476: 4472: 4462: 4460: 4456: 4455: 4451: 4443: 4404: 4399: 4398: 4389: 4359: 4358: 4354: 4322: 4321: 4314: 4291:. p. 165. 4282: 4281: 4277: 4255: 4254: 4241: 4211: 4210: 4206: 4196: 4195: 4184: 4148: 4147: 4143: 4113: 4112: 4108: 4087:(12): 507–649. 4078: 4077: 4073: 4025: 4024: 4020: 3984: 3983: 3979: 3957: 3956: 3947: 3899: 3898: 3889: 3866: 3865: 3861: 3851: 3849: 3848:on 24 July 2009 3840: 3839: 3835: 3825: 3824: 3820: 3776: 3775: 3771: 3761: 3759: 3750: 3749: 3745: 3736: 3735: 3731: 3721: 3720: 3716: 3711: 3707: 3697: 3695: 3686: 3685: 3672: 3663: 3662: 3658: 3649: 3648: 3644: 3618: 3617: 3613: 3604: 3603: 3599: 3563: 3562: 3553: 3515: 3514: 3510: 3496: 3486: 3479: 3478: 3474: 3435: 3434: 3430: 3382: 3381: 3377: 3355: 3354: 3350: 3342: 3304:(2–3): 71–237. 3293: 3288: 3287: 3264: 3216: 3215: 3211: 3163: 3162: 3158: 3122: 3121: 3117: 3079: 3078: 3074: 3026: 3025: 3021: 2973: 2972: 2968: 2920: 2919: 2908: 2864: 2863: 2856: 2849: 2833: 2832: 2825: 2815: 2814: 2810: 2762: 2761: 2757: 2727: 2726: 2713: 2708: 2696: 2633: 2624: 2618: 2585: 2541: 2535: 2443: 2441:X-ray dark star 2437: 2309: 2258: 2233: 2210: 2201: 2195: 2138: 2124: 2119: 2087: 2032: 1969: 1963: 1918: 1912: 1896:Galactic Center 1873: 1841: 1835: 1817: 1789: 1787:Perseus Cluster 1783: 1746: 1718: 1706: 1684: 1656: 1648:Eridanus Bubble 1610: 1604: 1589: 1583: 1566: 1549: 1543: 1535:Corona Borealis 1515: 1509: 1507:Corona Borealis 1493: 1481: 1452: 1428: 1394: 1357: 1351: 1288: 1276: 1270: 1239: 1233: 1203: 1187:galaxy clusters 1152: 1106: 1070: 1037: 1035:Comet detection 1021: 977: 968:Chuo University 960: 931: 895: 889: 823: 817: 714: 706:Main articles: 704: 671: 665: 657: 654: 625: 619: 592: 586: 581: 575: 556: 553: 526:as seen by the 497: 491: 439: 433: 424: 421: 412: 406: 390: 363: 357: 321:inverse Compton 248: 242: 162:X-ray photo by 156: 150: 148:Galaxy clusters 98:or black hole ( 60:galaxy clusters 28: 23: 22: 15: 12: 11: 5: 5581: 5579: 5571: 5570: 5565: 5560: 5550: 5549: 5543: 5542: 5540: 5539: 5534: 5529: 5524: 5519: 5514: 5509: 5504: 5499: 5494: 5492:Cosmochemistry 5489: 5484: 5479: 5477:Astrochemistry 5474: 5468: 5465: 5464: 5458: 5456: 5455: 5448: 5441: 5433: 5424: 5423: 5421: 5420: 5408: 5395: 5392: 5391: 5389: 5388: 5381: 5380: 5379: 5372: 5365: 5351: 5350: 5349: 5342: 5335: 5328: 5314: 5307: 5300: 5293: 5286: 5279: 5278: 5277: 5263: 5256: 5249: 5240: 5233: 5226: 5219: 5212: 5209:Astrochemistry 5205: 5198: 5190: 5188: 5184: 5183: 5181: 5180: 5173: 5166: 5159: 5152: 5145: 5142:Hale Telescope 5138: 5131: 5124: 5117: 5110: 5102: 5100: 5092: 5091: 5088: 5087: 5085: 5084: 5077: 5076: 5075: 5061: 5054: 5047: 5040: 5033: 5026: 5019: 5012: 5005: 4998: 4991: 4983: 4981: 4975: 4974: 4972: 4971: 4964: 4957: 4950: 4943: 4936: 4929: 4921: 4919: 4915: 4914: 4912: 4911: 4904: 4903: 4902: 4888: 4881: 4875:Visible-light 4871: 4857: 4850: 4842: 4840: 4836: 4835: 4833: 4832: 4831: 4830: 4816: 4804: 4802: 4798: 4797: 4795: 4794: 4787: 4780: 4773: 4765: 4763: 4756: 4752: 4751: 4749: 4748: 4741: 4734: 4727: 4720: 4713: 4712: 4711: 4697: 4689: 4686: 4685: 4680: 4678: 4677: 4670: 4663: 4655: 4647: 4646: 4631: 4626:10.1086/174494 4596: 4572: 4550: 4537:10.1086/587955 4513:(1): 545–549. 4497: 4470: 4449: 4387: 4382:10.1086/145813 4352: 4312: 4275: 4239: 4204: 4182: 4176:10.1086/180097 4141: 4136:10.1086/110278 4106: 4101:10.1086/190992 4071: 4058:10.1086/423192 4018: 3997:(10): 465–74. 3977: 3945: 3932:10.1086/423613 3908:(10): 267–83. 3887: 3876:(11): 109–34. 3859: 3833: 3818: 3769: 3743: 3729: 3714: 3705: 3670: 3665:"Brown Dwarfs" 3656: 3642: 3611: 3597: 3591:10.1086/163859 3551: 3508: 3499:|journal= 3472: 3428: 3415:10.1086/500311 3391:(1): 281–287. 3375: 3348: 3262: 3249:10.1086/339224 3209: 3196:10.1086/306804 3156: 3115: 3072: 3059:10.1086/324686 3019: 2966: 2953:10.1086/508613 2929:(1): L75–L78. 2906: 2892:10.1086/163218 2854: 2847: 2823: 2808: 2795:10.1086/508162 2755: 2710: 2709: 2707: 2704: 2703: 2702: 2695: 2692: 2666: 2665: 2654: 2632: 2629: 2620:Main article: 2617: 2614: 2584: 2581: 2537:Main article: 2534: 2531: 2488: 2487: 2480: 2479:production, or 2473: 2458:red supergiant 2439:Main article: 2436: 2433: 2424:Victoria Kaspi 2308: 2305: 2257: 2254: 2246:bremsstrahlung 2232: 2229: 2208: 2194: 2191: 2179:Doppler shifts 2136:ULX ray source 2123: 2120: 2118: 2115: 2072: 2071: 2068:image of M 82. 2049: 2031: 2028: 1962: 1959: 1928:(purple); the 1914:Main article: 1911: 1908: 1900:Sagittarius A* 1888:Sagittarius A* 1872: 1869: 1837:Main article: 1834: 1831: 1816: 1813: 1785:Main article: 1782: 1779: 1745: 1742: 1717: 1714: 1683: 1680: 1655: 1652: 1606:Main article: 1603: 1600: 1582: 1579: 1565: 1562: 1545:Main article: 1542: 1539: 1531:galaxy cluster 1511:Main article: 1508: 1505: 1492: 1489: 1480: 1477: 1451: 1448: 1427: 1424: 1393: 1390: 1353:Main article: 1350: 1347: 1327:John Flamsteed 1287: 1284: 1272:Main article: 1269: 1266: 1262:Seyfert galaxy 1235:Main article: 1232: 1231:Canes Venatici 1229: 1202: 1201:Camelopardalis 1199: 1151: 1148: 1105: 1102: 1092:. As with the 1069: 1066: 1036: 1033: 1020: 1017: 1002: 1001: 990: 976: 973: 959: 956: 930: 927: 899:nuclear fusion 891:Main article: 888: 885: 864:nuclear fusion 819:Main article: 816: 813: 703: 700: 667:Main article: 664: 661: 655: 652: 621:Main article: 618: 615: 588:Main article: 585: 582: 574: 571: 569:than expected. 554: 551: 533: 532: 511: 493:Main article: 490: 487: 478:magnetic field 463:accretion disk 435:Main article: 432: 429: 422: 419: 408:Main article: 405: 402: 392:The following 389: 386: 361:Seyfert galaxy 359:Main article: 356: 353: 273: 272: 261: 244:Main article: 241: 238: 227:potential well 199:potential well 195:kinetic energy 168:Bullet Cluster 152:Main article: 149: 146: 130:bremsstrahlung 100:X-ray binaries 26: 24: 14: 13: 10: 9: 6: 4: 3: 2: 5580: 5569: 5566: 5564: 5563:Space plasmas 5561: 5559: 5556: 5555: 5553: 5538: 5535: 5533: 5530: 5528: 5525: 5523: 5520: 5518: 5515: 5513: 5510: 5508: 5505: 5503: 5500: 5498: 5495: 5493: 5490: 5488: 5485: 5483: 5480: 5478: 5475: 5473: 5470: 5469: 5466: 5462: 5454: 5449: 5447: 5442: 5440: 5435: 5434: 5431: 5418: 5409: 5406: 5397: 5396: 5393: 5386: 5382: 5377: 5373: 5370: 5366: 5363: 5359: 5358: 5356: 5352: 5347: 5343: 5340: 5336: 5333: 5329: 5326: 5322: 5321: 5319: 5315: 5312: 5308: 5305: 5301: 5298: 5294: 5291: 5287: 5284: 5280: 5275: 5271: 5270: 5268: 5267:Constellation 5264: 5261: 5257: 5254: 5250: 5247: 5246: 5241: 5238: 5234: 5231: 5227: 5224: 5220: 5217: 5213: 5210: 5206: 5203: 5199: 5196: 5192: 5191: 5189: 5185: 5178: 5174: 5171: 5167: 5164: 5160: 5157: 5153: 5150: 5146: 5143: 5139: 5136: 5132: 5129: 5125: 5122: 5118: 5115: 5111: 5108: 5104: 5103: 5101: 5099: 5093: 5082: 5078: 5073: 5069: 5068: 5066: 5062: 5059: 5055: 5052: 5048: 5045: 5041: 5038: 5034: 5031: 5027: 5024: 5020: 5017: 5013: 5010: 5006: 5003: 4999: 4996: 4992: 4989: 4985: 4984: 4982: 4980: 4976: 4969: 4965: 4962: 4958: 4955: 4951: 4948: 4944: 4941: 4937: 4934: 4930: 4927: 4923: 4922: 4920: 4918:Other methods 4916: 4909: 4905: 4900: 4896: 4895: 4893: 4889: 4886: 4882: 4879: 4872: 4867: 4862: 4858: 4855: 4854:Submillimetre 4851: 4848: 4844: 4843: 4841: 4837: 4828: 4824: 4823: 4821: 4817: 4814: 4813:Extragalactic 4810: 4806: 4805: 4803: 4799: 4792: 4788: 4785: 4781: 4778: 4777:Observational 4774: 4771: 4767: 4766: 4764: 4760: 4757: 4753: 4746: 4742: 4739: 4735: 4732: 4728: 4725: 4721: 4718: 4714: 4709: 4705: 4704: 4702: 4698: 4695: 4691: 4690: 4687: 4683: 4676: 4671: 4669: 4664: 4662: 4657: 4656: 4653: 4642: 4635: 4632: 4627: 4623: 4619: 4615: 4611: 4607: 4600: 4597: 4591: 4586: 4579: 4577: 4573: 4568: 4561: 4559: 4557: 4555: 4551: 4546: 4542: 4538: 4534: 4530: 4526: 4521: 4516: 4512: 4508: 4501: 4498: 4485: 4481: 4474: 4471: 4459: 4453: 4450: 4442: 4438: 4434: 4430: 4426: 4422: 4418: 4414: 4410: 4403: 4396: 4394: 4392: 4388: 4383: 4379: 4375: 4371: 4367: 4363: 4356: 4353: 4348: 4344: 4339: 4334: 4330: 4326: 4319: 4317: 4313: 4308: 4304: 4299: 4294: 4290: 4286: 4279: 4276: 4271: 4267: 4263: 4259: 4252: 4250: 4248: 4246: 4244: 4240: 4235: 4231: 4227: 4223: 4219: 4215: 4208: 4205: 4200: 4193: 4191: 4189: 4187: 4183: 4177: 4172: 4168: 4164: 4160: 4156: 4152: 4145: 4142: 4137: 4133: 4129: 4125: 4121: 4117: 4110: 4107: 4102: 4098: 4094: 4090: 4086: 4082: 4075: 4072: 4067: 4063: 4059: 4055: 4051: 4047: 4042: 4037: 4033: 4029: 4022: 4019: 4013: 4008: 4004: 4000: 3996: 3992: 3988: 3981: 3978: 3973: 3969: 3966:(3): 629–38. 3965: 3961: 3954: 3952: 3950: 3946: 3941: 3937: 3933: 3929: 3925: 3921: 3916: 3911: 3907: 3903: 3896: 3894: 3892: 3888: 3883: 3879: 3875: 3871: 3863: 3860: 3847: 3843: 3837: 3834: 3829: 3822: 3819: 3814: 3810: 3805: 3800: 3796: 3792: 3789:(5761): 132. 3788: 3784: 3780: 3773: 3770: 3757: 3753: 3747: 3744: 3739: 3733: 3730: 3725: 3718: 3715: 3709: 3706: 3693: 3689: 3683: 3681: 3679: 3677: 3675: 3671: 3666: 3660: 3657: 3652: 3646: 3643: 3638: 3634: 3630: 3626: 3622: 3615: 3612: 3607: 3601: 3598: 3592: 3587: 3583: 3579: 3575: 3571: 3567: 3560: 3558: 3556: 3552: 3547: 3543: 3539: 3535: 3531: 3527: 3523: 3519: 3512: 3509: 3504: 3491: 3483: 3476: 3473: 3468: 3464: 3460: 3456: 3452: 3448: 3444: 3440: 3432: 3429: 3424: 3420: 3416: 3412: 3408: 3404: 3399: 3394: 3390: 3386: 3379: 3376: 3371: 3367: 3363: 3359: 3352: 3349: 3341: 3337: 3333: 3329: 3325: 3321: 3317: 3312: 3307: 3303: 3299: 3292: 3285: 3283: 3281: 3279: 3277: 3275: 3273: 3271: 3269: 3267: 3263: 3258: 3254: 3250: 3246: 3242: 3238: 3233: 3228: 3224: 3220: 3213: 3210: 3205: 3201: 3197: 3193: 3189: 3185: 3180: 3175: 3171: 3167: 3160: 3157: 3151: 3146: 3142: 3138: 3134: 3130: 3126: 3119: 3116: 3111: 3107: 3103: 3099: 3095: 3091: 3087: 3083: 3082:Space Sci Rev 3076: 3073: 3068: 3064: 3060: 3056: 3052: 3048: 3043: 3038: 3034: 3030: 3023: 3020: 3015: 3011: 3007: 3003: 2999: 2995: 2990: 2985: 2981: 2977: 2970: 2967: 2962: 2958: 2954: 2950: 2946: 2942: 2937: 2932: 2928: 2924: 2917: 2915: 2913: 2911: 2907: 2902: 2898: 2893: 2888: 2884: 2880: 2877:(6): 102–19. 2876: 2872: 2868: 2861: 2859: 2855: 2850: 2844: 2840: 2836: 2835:Sparke, L. S. 2830: 2828: 2824: 2819: 2812: 2809: 2804: 2800: 2796: 2792: 2788: 2784: 2779: 2774: 2770: 2766: 2759: 2756: 2751: 2747: 2743: 2739: 2736:(1): 325–50. 2735: 2731: 2724: 2722: 2720: 2718: 2716: 2712: 2705: 2701: 2698: 2697: 2693: 2691: 2689: 2685: 2684:magnetosphere 2681: 2677: 2673: 2659: 2655: 2650: 2646: 2641: 2637: 2630: 2628: 2623: 2615: 2613: 2611: 2601: 2597: 2595: 2591: 2582: 2580: 2578: 2574: 2570: 2566: 2562: 2558: 2554: 2550: 2549:Stellar winds 2546: 2540: 2532: 2530: 2526: 2523: 2521: 2517: 2513: 2512:main sequence 2509: 2505: 2501: 2497: 2493: 2485: 2481: 2478: 2474: 2471: 2467: 2466: 2465: 2463: 2459: 2454: 2452: 2448: 2447:Sun in X-rays 2442: 2434: 2432: 2429: 2425: 2416: 2411: 2407: 2404: 2397: 2393: 2389: 2386: 2384: 2378: 2376: 2372: 2368: 2364: 2360: 2356: 2351: 2349: 2344: 2343:Robert Duncan 2340: 2336: 2332: 2331: 2322: 2318: 2313: 2306: 2304: 2302: 2298: 2293: 2289: 2287: 2283: 2279: 2271: 2267: 2262: 2255: 2253: 2251: 2247: 2242: 2238: 2230: 2228: 2226: 2222: 2218: 2214: 2205: 2200: 2192: 2190: 2188: 2187:time dilation 2184: 2180: 2176: 2173: 2169: 2165: 2161: 2157: 2153: 2149: 2145: 2137: 2133: 2128: 2121: 2116: 2114: 2112: 2108: 2104: 2100: 2095: 2093: 2085: 2082: 2081:constellation 2078: 2067: 2063: 2059: 2054: 2050: 2045: 2040: 2036: 2029: 2027: 2025: 2021: 2017: 2012: 2010: 2006: 2001: 1999: 1995: 1990: 1987: 1977: 1973: 1968: 1960: 1958: 1955: 1947: 1943: 1939: 1935: 1931: 1927: 1922: 1917: 1909: 1907: 1905: 1904:Sagittarius A 1901: 1897: 1889: 1885: 1881: 1880:Sagittarius A 1877: 1870: 1868: 1866: 1862: 1855: 1851: 1845: 1840: 1832: 1830: 1821: 1814: 1812: 1806: 1802: 1798: 1793: 1788: 1780: 1778: 1776: 1773:has a type 2 1772: 1768: 1763: 1754: 1750: 1743: 1741: 1739: 1731: 1727: 1722: 1715: 1713: 1711: 1705: 1701: 1693: 1688: 1681: 1679: 1673: 1669: 1665: 1660: 1653: 1651: 1649: 1645: 1641: 1640: 1631: 1627: 1623: 1619: 1614: 1609: 1601: 1599: 1597: 1592: 1588: 1580: 1578: 1570: 1563: 1561: 1559: 1554: 1548: 1540: 1538: 1536: 1532: 1524: 1519: 1514: 1506: 1504: 1502: 1498: 1497:spectral type 1490: 1488: 1486: 1485:spectral type 1478: 1476: 1473: 1469: 1468:coronal cloud 1461: 1458:This shows a 1456: 1449: 1447: 1445: 1441: 1437: 1433: 1425: 1423: 1421: 1418: 1414: 1410: 1403: 1398: 1391: 1389: 1387: 1382: 1374: 1370: 1366: 1365:peculiar star 1361: 1356: 1348: 1346: 1344: 1340: 1336: 1331: 1328: 1324: 1323:3 Cassiopeiae 1320: 1316: 1313: 1305: 1301: 1297: 1292: 1285: 1283: 1281: 1275: 1267: 1265: 1263: 1260: 1256: 1248: 1247:near-infrared 1243: 1238: 1230: 1228: 1221: 1217: 1213: 1207: 1200: 1198: 1196: 1192: 1188: 1184: 1180: 1173: 1169: 1165: 1161: 1156: 1149: 1147: 1145: 1142: 1134: 1129: 1122: 1118: 1114: 1110: 1103: 1101: 1099: 1095: 1091: 1087: 1083: 1079: 1075: 1067: 1065: 1062: 1058: 1049: 1045: 1041: 1034: 1032: 1028: 1026: 1018: 1016: 1012: 1008: 995: 991: 985: 981: 974: 972: 969: 965: 962:Using NASA's 957: 951: 947: 945: 940: 936: 928: 922: 918: 916: 912: 908: 904: 900: 894: 886: 884: 881: 875: 871: 869: 865: 861: 857: 852: 849: 845: 840: 837: 833: 829: 822: 814: 812: 810: 805: 803: 798: 794: 790: 786: 782: 778: 774: 770: 769:Coronal loops 762: 757: 753: 750: 745: 743: 738: 734: 727: 723: 718: 713: 709: 701: 699: 697: 693: 688: 684: 680: 676: 670: 662: 660: 658: 649: 645: 641: 639: 629: 624: 616: 614: 612: 608: 604: 600: 596: 591: 583: 580: 572: 570: 568: 563: 561: 557: 548: 544: 540: 529: 525: 521: 516: 512: 505: 501: 496: 488: 486: 484: 479: 474: 472: 468: 464: 460: 456: 455:event horizon 448: 443: 438: 430: 428: 425: 416: 411: 403: 401: 399: 395: 387: 385: 383: 379: 375: 371: 370:spectral line 367: 362: 354: 352: 350: 346: 341: 337: 333: 329: 326:On board the 324: 322: 318: 314: 310: 306: 302: 298: 294: 290: 286: 285: 280: 266: 262: 256: 252: 247: 239: 237: 235: 230: 228: 224: 220: 216: 212: 208: 207:line emission 204: 200: 196: 192: 188: 181: 177: 173: 169: 165: 160: 155: 147: 145: 143: 139: 135: 131: 127: 122: 120: 119:coronal cloud 116: 111: 109: 105: 101: 97: 93: 89: 85: 82:containing a 81: 77: 73: 69: 65: 61: 56: 54: 50: 46: 39: 34: 30: 19: 5487:Astrophysics 5472:Astrobiology 5243: 5223:Astrophysics 5202:Astrobiology 4866:Far-infrared 4820:Local system 4755:Astronomy by 4745:... in space 4640: 4634: 4609: 4605: 4599: 4510: 4506: 4500: 4488:. Retrieved 4484:the original 4473: 4461:. Retrieved 4452: 4441:the original 4415:(2): 34–41. 4412: 4408: 4365: 4361: 4355: 4328: 4324: 4284: 4278: 4261: 4257: 4217: 4213: 4207: 4158: 4154: 4144: 4119: 4115: 4109: 4084: 4080: 4074: 4031: 4027: 4021: 3994: 3990: 3980: 3963: 3959: 3905: 3902:Astrophys. J 3901: 3873: 3869: 3862: 3850:. Retrieved 3846:the original 3836: 3821: 3786: 3782: 3772: 3760:. Retrieved 3746: 3732: 3717: 3708: 3696:. Retrieved 3692:the original 3659: 3645: 3620: 3614: 3600: 3573: 3569: 3521: 3517: 3511: 3490:cite journal 3481: 3475: 3442: 3438: 3431: 3388: 3384: 3378: 3361: 3357: 3351: 3340:the original 3301: 3297: 3222: 3218: 3212: 3169: 3165: 3159: 3132: 3129:Rev Mod Phys 3128: 3118: 3088:(3–4): 291. 3085: 3081: 3075: 3032: 3028: 3022: 2979: 2975: 2969: 2926: 2922: 2874: 2871:Astrophys. J 2870: 2838: 2811: 2768: 2764: 2758: 2733: 2729: 2669: 2625: 2607: 2586: 2577:Local Bubble 2569:superbubbles 2542: 2527: 2524: 2500:Gamma Crucis 2489: 2484:chromosphere 2455: 2444: 2420: 2405: 2401: 2387: 2379: 2352: 2328: 2326: 2294: 2290: 2275: 2234: 2202: 2160:star systems 2152:X-ray binary 2141: 2111:Lockman Hole 2105:10 34 00.00 2096: 2075: 2044:Lockman Hole 2013: 2002: 1991: 1982: 1951: 1893: 1859: 1852:08 23 08.16 1827: 1810: 1799:03 19 47.60 1758: 1735: 1697: 1677: 1647: 1643: 1637: 1635: 1617: 1593: 1590: 1576: 1550: 1528: 1494: 1482: 1465: 1429: 1408: 1407: 1378: 1332: 1309: 1277: 1252: 1225: 1220:Camelopardus 1214:07 41 50.20 1189:observed by 1177: 1138: 1071: 1054: 1029: 1025:fluorescence 1022: 1013: 1009: 1005: 961: 932: 907:brown dwarfs 896: 887:Brown dwarfs 876: 872: 853: 841: 824: 815:White dwarfs 806: 767: 746: 739: 735: 731: 696:solar masses 675:Scorpius X-1 672: 669:Scorpius X-1 663:Scorpius X-1 644:Hercules X-1 642: 635: 623:Hercules X-1 617:Hercules X-1 611:stellar wind 593: 564: 536: 475: 467:white dwarfs 452: 413: 391: 364: 325: 323:scattering. 304: 300: 296: 282: 278: 276: 231: 185: 179: 123: 112: 104:Solar System 96:neutron star 80:binary stars 57: 44: 43: 29: 5290:Planetarium 4947:High-energy 4933:Cosmic rays 4885:Ultraviolet 4606:Astrophys J 4507:Astrophys J 4490:17 December 4402:"Magnetars" 4362:Astrophys J 4155:Astrophys J 4028:Astrophys J 3698:16 November 3570:Astrophys J 3385:Astrophys J 3219:Astrophys J 3166:Astrophys J 2982:: 196–199. 2923:Astrophys J 2816:Dooling D. 2765:Astrophys J 2559:created by 2557:shock waves 2553:HII regions 2508:giant stars 2504:H-R diagram 2371:SGR 1900+14 2301:radio waves 2241:supergiants 2168:A-type star 2144:microquasar 2134:- possible 2122:Microquasar 2088:09 55 50.01 2056:A combined 1944:0 37 41.10 1871:Sagittarius 1415:) with two 1381:Eta Carinae 1369:Eta Carinae 1355:Eta Carinae 1312:Cassiopea A 1268:Canis Major 1121:ultraviolet 1086:black holes 1061:Comet Lulin 1044:Comet Lulin 893:Brown dwarf 828:white dwarf 821:White dwarf 785:solar cycle 764:atmosphere. 742:solar cycle 567:ultraviolet 543:white dwarf 431:Black holes 219:dark matter 191:dark matter 84:white dwarf 64:black holes 5552:Categories 5482:Astrometry 5283:Photometry 5260:Binoculars 5237:Astrometry 5098:telescopes 4995:Babylonian 4839:EM methods 4717:Astronomer 4463:4 February 4220:(1): 507. 4034:(1): 260. 3524:(2): 111. 3225:(1): 273. 3172:(2): 985. 3135:(3): 995. 2706:References 2688:ionosphere 2649:atmosphere 2561:supernovae 2506:among the 2462:red giants 2451:Betelgeuse 2339:gamma rays 2282:Messier 87 2270:lightspeed 2256:Messier 87 2204:LSI+61°303 2197:See also: 2183:relativity 2099:Ursa Major 2084:Ursa Major 2079:is in the 2030:Ursa Major 2016:XMM-Newton 2007:, and the 1976:XMM-Newton 1965:See also: 1707:10 49 52.5 1585:See also: 1523:Abell 2142 1513:Abell 2142 1426:Chamaeleon 1335:Cassiopeia 1310:Regarding 1286:Cassiopeia 1144:XMM-Newton 935:convection 905:stars and 880:XMM-Newton 648:Roche lobe 607:supergiant 577:See also: 483:luminosity 447:Cygnus X-1 437:Black hole 223:virialised 5497:Cosmology 5461:astronomy 5355:Telescope 4961:Spherical 4908:Gamma-ray 4877:(optical) 4682:Astronomy 4643:(1): 201. 4545:119284256 4520:0712.1502 4338:0809.3157 4066:119356104 3722:Reddy F. 3546:122895766 3467:120983201 3445:(2): 93. 3336:119509015 3110:120443194 2989:0704.0237 2901:122426629 2492:Aldebaran 2456:Like the 2363:Venera 12 2359:Venera 11 2307:Magnetars 1700:Leo Minor 1692:Leo Minor 1682:Leo Minor 1666:09 18 06 1409:Abell 400 1339:supernova 1170:14 11 20 1133:Andromeda 1104:Andromeda 944:lightning 929:LP 944-20 903:red dwarf 836:red giant 809:CORONAS-F 749:CORONAS-F 683:Milky Way 547:red giant 309:cyclotron 5405:Category 5114:Category 5009:Egyptian 4926:Neutrino 4861:Infrared 4809:Galactic 4784:Sidewalk 4738:Glossary 4708:Timeline 4478:Naye R. 4437:12561456 4331:: 2892. 4116:Astron J 3940:14535693 3762:4 August 3756:Archived 3423:11072226 3257:14136652 3067:16381236 3014:17149878 2961:17728755 2694:See also 2594:Ranger 5 2590:Ranger 3 2496:Arcturus 2330:magnetar 2264:A 5,000 1910:Sculptor 1861:Puppis A 1839:Puppis A 1777:nucleus. 1771:NGC 7319 1762:NGC 7318 1622:Eridanus 1602:Eridanus 1587:3C 390.3 1413:NGC 1128 1402:NGC 1128 1255:NGC 4151 1237:NGC 4151 1098:universe 1082:galaxies 844:Einstein 789:sunspots 781:magnetic 740:Similar 679:Scorpius 656:☉ 595:Vela X-1 590:Vela X-1 584:Vela X-1 555:☉ 522:Type Ia 423:☉ 340:4C 71.07 291:with an 211:hydrogen 193:) gains 176:Redshift 102:). Some 5417:Commons 5369:history 5339:Russian 5187:Related 5096:Optical 5081:Tibetan 5065:Serbian 5058:Persian 5002:Chinese 4979:Culture 4899:History 4770:Amateur 4701:History 4694:Outline 4614:Bibcode 4612:: 402. 4525:Bibcode 4417:Bibcode 4370:Bibcode 4368:: 215. 4343:Bibcode 4303:Bibcode 4266:Bibcode 4264:: 817. 4222:Bibcode 4163:Bibcode 4161:: L75. 4124:Bibcode 4122:: 597. 4089:Bibcode 4046:Bibcode 3999:Bibcode 3968:Bibcode 3920:Bibcode 3878:Bibcode 3852:12 July 3813:4257241 3791:Bibcode 3653:. 2009. 3625:Bibcode 3578:Bibcode 3576:: 819. 3526:Bibcode 3447:Bibcode 3403:Bibcode 3366:Bibcode 3364:: 171. 3316:Bibcode 3237:Bibcode 3204:1207793 3184:Bibcode 3137:Bibcode 3090:Bibcode 3047:Bibcode 2994:Bibcode 2941:Bibcode 2879:Bibcode 2803:2897407 2783:Bibcode 2738:Bibcode 2545:Coronal 2415:Chandra 2396:Chandra 2278:Chandra 2225:Cir X-1 2221:Cyg X-3 2181:and by 2077:M82 X-1 2066:Chandra 2062:Spitzer 1967:Serpens 1961:Serpens 1805:Perseus 1781:Perseus 1775:Seyfert 1744:Pegasus 1373:Chandra 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