202:. Which type of line is observed depends on the type of material and its temperature relative to another emission source. An absorption line is produced when photons from a hot, broad spectrum source pass through a cooler material. The intensity of light, over a narrow frequency range, is reduced due to absorption by the material and re-emission in random directions. By contrast, a bright emission line is produced when photons from a hot material are detected, perhaps in the presence of a broad spectrum from a cooler source. The intensity of light, over a narrow frequency range, is increased due to emission by the hot material.
2763:
2133:
2923:
2903:
25:
60:
2273:
2233:
2173:
1813:
1793:
1253:
2883:
2843:
2823:
2803:
2353:
2153:
2093:
1993:
1873:
1833:
1753:
1713:
1593:
1453:
1213:
1193:
1033:
1333:
39:
2723:
2633:
2573:
2513:
2413:
2373:
2213:
2193:
1973:
1693:
1633:
1433:
1393:
1373:
1293:
2433:
1413:
1133:
1093:
973:
2743:
2613:
2553:
2493:
2453:
2393:
2333:
2293:
2253:
2053:
1913:
1853:
1773:
1673:
1653:
1613:
1573:
1353:
1233:
1013:
2783:
1733:
2863:
2703:
2473:
2313:
2113:
2073:
1933:
1893:
1533:
1513:
1493:
1173:
993:
2013:
1273:
1113:
1073:
2668:
2033:
1313:
1053:
2593:
2533:
1553:
1473:
1153:
1953:
80:
382:). In addition, its center may be shifted from its nominal central wavelength. There are several reasons for this broadening and shift. These reasons may be divided into two general categories – broadening due to local conditions and broadening due to extended conditions. Broadening due to local conditions is due to effects which hold in a small region around the emitting element, usually small enough to assure
144:
457:: The collision of other particles with the light emitting particle interrupts the emission process, and by shortening the characteristic time for the process, increases the uncertainty in the energy emitted (as occurs in natural broadening). The duration of the collision is much shorter than the lifetime of the emission process. This effect depends on both the
487:. The form of the line profile is determined by the functional form of the perturbing force with respect to distance from the perturbing particle. There may also be a shift in the line center. The general expression for the lineshape resulting from quasistatic pressure broadening is a 4-parameter generalization of the Gaussian distribution known as a
191:), the photon is absorbed. Then the energy will be spontaneously re-emitted, either as one photon at the same frequency as the original one or in a cascade, where the sum of the energies of the photons emitted will be equal to the energy of the one absorbed (assuming the system returns to its original state).
411:) with the uncertainty of its energy. Some authors use the term "radiative broadening" to refer specifically to the part of natural broadening caused by the spontaneous radiative decay. A short lifetime will have a large energy uncertainty and a broad emission. This broadening effect results in an unshifted
835:
Each of these mechanisms can act in isolation or in combination with others. Assuming each effect is independent, the observed line profile is a convolution of the line profiles of each mechanism. For example, a combination of the thermal
Doppler broadening and the impact pressure broadening yields a
3104:
Rothman, L.S.; Gordon, I.E.; Babikov, Y.; Barbe, A.; Chris Benner, D.; Bernath, P.F.; Birk, M.; Bizzocchi, L.; Boudon, V.; Brown, L.R.; Campargue, A.; Chance, K.; Cohen, E.A.; Coudert, L.H.; Devi, V.M.; Drouin, B.J.; Fayt, A.; Flaud, J.-M.; Gamache, R.R.; Harrison, J.J.; Hartmann, J.-M.; Hill, C.;
433:
depending on the velocity of the atom relative to the observer. The higher the temperature of the gas, the wider the distribution of velocities in the gas. Since the spectral line is a combination of all of the emitted radiation, the higher the temperature of the gas, the broader the spectral line
793:
Opacity broadening is an example of a non-local broadening mechanism. Electromagnetic radiation emitted at a particular point in space can be reabsorbed as it travels through space. This absorption depends on wavelength. The line is broadened because the photons at the line center have a greater
814:
due to a finite line-of-sight velocity projection. If different parts of the emitting body have different velocities (along the line of sight), the resulting line will be broadened, with the line width proportional to the width of the velocity distribution. For example, radiation emitted from a
770:
is a general term for broadening because some emitting particles are in a different local environment from others, and therefore emit at a different frequency. This term is used especially for solids, where surfaces, grain boundaries, and stoichiometry variations can create a variety of local
386:. Broadening due to extended conditions may result from changes to the spectral distribution of the radiation as it traverses its path to the observer. It also may result from the combining of radiation from a number of regions which are far from each other.
819:, will be broadened due to the line-of-sight variations in velocity on opposite sides of the star (this effect usually referred to as rotational broadening). The greater the rate of rotation, the broader the line. Another example is an imploding
843:
However, the different line broadening mechanisms are not always independent. For example, the collisional effects and the motional
Doppler shifts can act in a coherent manner, resulting under some conditions even in a collisional
3271:
3245:
755:
688:
629:
574:
479:), thereby altering the frequency of the emitted radiation. The duration of the influence is much longer than the lifetime of the emission process. This effect depends on the
899:
because they remain largely unchanged for a given chemical element, independent of their chemical environment. Longer wavelengths correspond to lower energies, where the
91:
of this sunlight is the "source." This is the spectrum of a blue sky somewhat close to the horizon, looking east with the sun to the west at around 3–4 pm on a clear day.
127:. These "fingerprints" can be compared to the previously collected ones of atoms and molecules, and are thus used to identify the atomic and molecular components of
785:
Certain types of broadening are the result of conditions over a large region of space rather than simply upon conditions that are local to the emitting particle.
3057:
3037:
524:
3299:
703:
is often useful in describing the profile. The energy shift as a function of distance between the interacting particles is given in the wings by e.g. the
232:
Depending on the material and its physical conditions, the energy of the involved photons can vary widely, with the spectral lines observed across the
429:
The atoms in a gas which are emitting radiation will have a distribution of velocities. Each photon emitted will be "red"- or "blue"-shifted by the
581:
occurs when the perturbing particle is of the same type as the emitting particle, which introduces the possibility of an energy exchange process.
446:
The presence of nearby particles will affect the radiation emitted by an individual particle. There are two limiting cases by which this occurs:
108:
3249:
640:, which results from the interaction of an emitter with an electric field, causing a shift in energy that is quadratic in the field strength.
3391:
3185:
3053:
104:
794:
reabsorption probability than the photons at the line wings. Indeed, the reabsorption near the line center may be so great as to cause a
205:
Spectral lines are highly atom-specific, and can be used to identify the chemical composition of any medium. Several elements, including
415:. The natural broadening can be experimentally altered only to the extent that decay rates can be artificially suppressed or enhanced.
771:
environments for a given atom to occupy. In liquids, the effects of inhomogeneous broadening is sometimes reduced by a process called
359:
183:(which is connected to its frequency) to allow a change in the energy state of the system (in the case of an atom this is usually an
3356:
3333:
3045:
321:
383:
342:
3060:, Volume 36, by Instytut Podstawowych Problemów Techniki (Polska Akademia Nauk), publisher: Państwowe Wydawn. Naukowe., 1995,
879:. Many spectral lines occur at wavelengths outside this range. At shorter wavelengths, which correspond to higher energies,
3200:
For example, in the following article, decay was suppressed via a microwave cavity, thus reducing the natural broadening:
83:
Absorption lines for air, under indirect illumination, so that the gas is not directly between source and detector. Here,
798:
in which the intensity at the center of the line is less than in the wings. This process is also sometimes called
3002:
904:
876:
861:
766:
329:
233:
152:
3105:
Hodges, J.T.; Jacquemart, D.; Jolly, A.; Lamouroux, J.; Le Roy, R.J.; Li, G.; Long, D.A.; et al. (2013).
506:, which results from the interaction of an emitter with an electric field of a charged particle at a distance
710:
704:
643:
584:
529:
358:. These series exist across atoms of all elements, and the patterns for all atoms are well-predicted by the
148:
65:
3155:
2971:
637:
188:
3386:
400:
3283:
3211:
3118:
2961:
896:
700:
404:
399:
The lifetime of excited states results in natural broadening, also known as lifetime broadening. The
2956:
871:
The phrase "spectral lines", when not qualified, usually refers to lines having wavelengths in the
696:
503:
488:
466:
412:
371:
100:
88:
2991:
773:
424:
2762:
2132:
2922:
2902:
3352:
3329:
3227:
3181:
3134:
3049:
3041:
2981:
2976:
2540:
2272:
2232:
2172:
1812:
1792:
1252:
435:
160:
48:
44:
495:
Pressure broadening may also be classified by the nature of the perturbing force as follows:
3291:
3219:
3173:
3151:
3126:
2882:
2842:
2822:
2802:
2352:
2152:
2092:
1992:
1872:
1832:
1752:
1712:
1592:
1452:
1332:
1212:
1192:
1032:
939:
928:
872:
820:
284:
269:
268:, though some of the Fraunhofer "lines" are blends of multiple lines from several different
253:
84:
69:
2722:
2632:
2572:
2512:
2432:
2412:
2372:
2212:
2192:
1972:
1692:
1632:
1432:
1412:
1392:
1372:
1292:
1132:
1092:
972:
59:
24:
2986:
2782:
2742:
2612:
2552:
2492:
2452:
2392:
2332:
2292:
2252:
2052:
1912:
1852:
1772:
1732:
1672:
1652:
1612:
1572:
1352:
1232:
1012:
257:
475:: The presence of other particles shifts the energy levels in the emitting particle (see
3287:
3215:
3122:
2862:
2702:
2472:
2312:
2112:
2072:
2012:
1932:
1892:
1532:
1512:
1492:
1272:
1172:
1112:
1072:
992:
38:
3348:
3202:
Gabrielse, Gerald; H. Dehmelt (1985). "Observation of
Inhibited Spontaneous Emission".
2667:
2032:
1312:
1052:
908:
509:
430:
379:
354:
222:
172:
119:
range, compared with the nearby frequencies. Spectral lines are often used to identify
2592:
2532:
1552:
1472:
1152:
3380:
3007:
2996:
916:
912:
837:
811:
476:
375:
337:
288:
280:
180:
1952:
79:
3012:
2750:
2120:
927:
For each element, the following table shows the spectral lines which appear in the
884:
849:
408:
348:
333:
143:
3367:
225:
of the material, so they are widely used to determine the physical conditions of
3130:
3017:
2910:
2890:
880:
484:
462:
218:
3295:
3223:
3156:
On a
Heuristic Viewpoint Concerning the Production and Transformation of Light
2966:
2260:
2220:
2160:
1800:
1780:
1240:
313:
237:
3138:
3036:"Van der Waals profile" appears as lowercase in almost all sources, such as:
378:
with a nonzero range of frequencies, not a single frequency (i.e., a nonzero
2934:
2870:
2830:
2810:
2790:
2340:
2140:
2080:
1980:
1860:
1820:
1740:
1700:
1580:
1440:
1320:
1200:
1180:
1020:
317:
241:
217:, were discovered by spectroscopic means. Spectral lines also depend on the
116:
3231:
3106:
2710:
2675:
2640:
2620:
2560:
2500:
2420:
2400:
2360:
2200:
2180:
1960:
1680:
1620:
1420:
1400:
1380:
1360:
1280:
1120:
1080:
960:
900:
888:
325:
264:
for a line at 393.366 nm emerging from singly-ionized calcium atom,
210:
184:
168:
124:
3177:
3082:
2930:
2770:
2730:
2600:
2480:
2440:
2380:
2320:
2280:
2240:
2040:
1900:
1840:
1760:
1720:
1660:
1640:
1600:
1560:
1340:
1220:
1000:
824:
480:
458:
214:
2850:
2690:
2460:
2300:
2100:
2060:
2000:
1920:
1880:
1520:
1500:
1480:
1260:
1160:
1100:
1060:
980:
206:
176:
132:
275:
In other cases, the lines are designated according to the level of
229:
and other celestial bodies that cannot be analyzed by other means.
3040:
by Clive
Anthony Croxton, 1980, A Wiley-Interscience publication,
2655:
2020:
1300:
1040:
892:
526:, causing a shift in energy that is linear in the field strength.
291:
I, singly ionized atoms with II, and so on, so that, for example:
142:
112:
78:
3084:
NIST Atomic
Spectra Database, NIST Standard Reference Database 78
340:. Originally all spectral lines were classified into series: the
2580:
2520:
1540:
1460:
1140:
816:
434:
emitted from that gas. This broadening effect is described by a
226:
164:
128:
120:
3272:"Theory of the pressure broadening and shift of spectral lines"
1940:
276:
3111:
99:
is a weaker or stronger region in an otherwise uniform and
3168:
Krainov, Vladimir; Reiss, Howard; Smirnov, Boris (1997).
16:
A distinctive narrow spectral feature of chemical species
695:
occurs when the emitting particle is being perturbed by
362:. These series were later associated with suborbitals.
159:
Spectral lines are the result of interaction between a
713:
646:
587:
532:
512:
324:(for molecular lines). Many spectral lines of atomic
465:
of the gas. The broadening effect is described by a
312:
More detailed designations usually include the line
810:Radiation emitted by a moving source is subject to
749:
682:
623:
568:
518:
3107:"The HITRAN2012 molecular spectroscopic database"
403:relates the lifetime of an excited state (due to
3087:, National Institute of Standards and Technology
2992:Table of emission spectra of gas discharge lamps
915:used to detect neutral hydrogen throughout the
328:also have designations within their respective
179:. When a photon has about the right amount of
907:of hydrogen. At even longer wavelengths, the
194:A spectral line may be observed either as an
8:
3081:Kramida, Alexander; Ralchenko, Yuri (1999),
370:There are a number of effects which control
254:visible part of the electromagnetic spectrum
3038:Statistical mechanics of the liquid surface
933:
738:
729:
712:
671:
662:
645:
612:
603:
586:
557:
548:
531:
511:
483:of the gas, but is rather insensitive to
3073:
3029:
954:
151:(mid) and discrete spectrum lines of a
135:, which would otherwise be impossible.
750:{\displaystyle (\Delta E\sim 1/r^{6})}
683:{\displaystyle (\Delta E\sim 1/r^{4})}
624:{\displaystyle (\Delta E\sim 1/r^{3})}
569:{\displaystyle (\Delta E\sim 1/r^{2})}
374:. A spectral line extends over a tiny
3372:. New York: McGraw-Hill book Company.
3170:Radiative Processes in Atomic Physics
891:. At the much shorter wavelengths of
469:and there may be an associated shift.
287:. Neutral atoms are denoted with the
7:
3345:Spectral Line Broadening by Plasmas
856:Spectral lines of chemical elements
781:Broadening due to non-local effects
717:
650:
591:
536:
438:and there is no associated shift.
14:
3326:Principles of Plasma Spectroscopy
3248:. Fas.harvard.edu. Archived from
815:distant rotating body, such as a
2921:
2901:
2881:
2861:
2841:
2821:
2801:
2781:
2761:
2741:
2721:
2701:
2666:
2631:
2611:
2591:
2571:
2551:
2531:
2511:
2491:
2471:
2451:
2431:
2411:
2391:
2371:
2351:
2331:
2311:
2291:
2271:
2251:
2231:
2211:
2191:
2171:
2151:
2131:
2111:
2091:
2071:
2051:
2031:
2011:
1991:
1971:
1951:
1931:
1911:
1891:
1871:
1851:
1831:
1811:
1791:
1771:
1751:
1731:
1711:
1691:
1671:
1651:
1631:
1611:
1591:
1571:
1551:
1531:
1511:
1491:
1471:
1451:
1431:
1411:
1391:
1371:
1351:
1331:
1311:
1291:
1271:
1251:
1231:
1211:
1191:
1171:
1151:
1131:
1111:
1091:
1071:
1051:
1031:
1011:
991:
971:
58:
37:
23:
3328:. Cambridge: University Press.
473:Quasistatic pressure broadening
390:Broadening due to local effects
384:local thermodynamic equilibrium
806:Macroscopic Doppler broadening
744:
714:
699:. For the quasistatic case, a
677:
647:
618:
588:
563:
533:
1:
320:number (for atomic lines) or
297:— copper ion with +1 charge,
252:Strong spectral lines in the
3392:Spectrum (physical sciences)
3058:Journal of technical physics
3131:10.1016/j.jqsrt.2013.07.002
903:spectral lines include the
883:spectral lines include the
405:spontaneous radiative decay
306:— iron ion with +2 charge,
3408:
931:at about 400-700 nm.
859:
634:Quadratic Stark broadening
451:Impact pressure broadening
422:
419:Thermal Doppler broadening
283:to the designation of the
147:Continuous spectrum of an
3296:10.1080/00018738100101467
3224:10.1103/PhysRevLett.55.67
895:, the lines are known as
366:Line broadening and shift
3246:"Collisional Broadening"
3003:Hydrogen spectral series
877:electromagnetic spectrum
862:Hydrogen spectral series
767:Inhomogeneous broadening
761:Inhomogeneous broadening
693:Van der Waals broadening
234:electromagnetic spectrum
3366:Griem, Hans R. (1964).
3343:Griem, Hans R. (1974).
3324:Griem, Hans R. (1997).
3204:Physical Review Letters
705:Lennard-Jones potential
500:Linear Stark broadening
2972:Electron configuration
751:
684:
638:quadratic Stark effect
625:
570:
520:
455:collisional broadening
156:
92:
897:characteristic X-rays
752:
701:Van der Waals profile
685:
626:
571:
521:
401:uncertainty principle
260:designation, such as
146:
139:Types of line spectra
103:. It may result from
82:
2962:Atomic spectral line
711:
697:Van der Waals forces
644:
585:
579:Resonance broadening
530:
510:
360:Rydberg-Ritz formula
256:often have a unique
3369:Plasma Spectroscopy
3288:1981AdPhy..30..367P
3276:Advances in Physics
3216:1985PhRvL..55...67G
3123:2013JQSRT.130....4R
2957:Absorption spectrum
942:
504:linear Stark effect
489:stable distribution
442:Pressure broadening
372:spectral line shape
101:continuous spectrum
89:Rayleigh scattering
72:(discrete spectrum)
66:Absorption spectrum
30:Continuous spectrum
3270:Peach, G. (1981).
3178:10.1002/3527605606
934:
789:Opacity broadening
774:motional narrowing
747:
680:
621:
566:
516:
467:Lorentzian profile
425:Doppler broadening
413:Lorentzian profile
395:Natural broadening
316:and may include a
157:
93:
3187:978-0-471-12533-4
3054:978-0-471-27663-0
2982:Fourier transform
2977:Emission spectrum
2948:
2947:
940:chemical elements
519:{\displaystyle r}
149:incandescent lamp
49:discrete spectrum
3399:
3373:
3362:
3339:
3311:
3310:
3308:
3307:
3298:. Archived from
3267:
3261:
3260:
3258:
3257:
3242:
3236:
3235:
3198:
3192:
3191:
3165:
3159:
3152:Einstein, Albert
3149:
3143:
3142:
3101:
3095:
3094:
3093:
3092:
3078:
3061:
3034:
2925:
2905:
2885:
2865:
2845:
2825:
2805:
2785:
2765:
2745:
2725:
2705:
2670:
2635:
2615:
2595:
2575:
2555:
2535:
2515:
2495:
2475:
2455:
2435:
2415:
2395:
2375:
2355:
2335:
2315:
2295:
2275:
2255:
2235:
2215:
2195:
2175:
2155:
2135:
2115:
2095:
2075:
2055:
2035:
2015:
1995:
1975:
1955:
1935:
1915:
1895:
1875:
1855:
1835:
1815:
1795:
1775:
1755:
1735:
1715:
1695:
1675:
1655:
1635:
1615:
1595:
1575:
1555:
1535:
1515:
1495:
1475:
1455:
1435:
1415:
1395:
1375:
1355:
1335:
1315:
1295:
1275:
1255:
1235:
1215:
1195:
1175:
1155:
1135:
1115:
1095:
1075:
1055:
1035:
1015:
995:
975:
943:
929:visible spectrum
831:Combined effects
756:
754:
753:
748:
743:
742:
733:
689:
687:
686:
681:
676:
675:
666:
630:
628:
627:
622:
617:
616:
607:
575:
573:
572:
567:
562:
561:
552:
525:
523:
522:
517:
436:Gaussian profile
343:principal series
322:band designation
285:chemical element
167:, but sometimes
153:fluorescent lamp
87:in sunlight and
85:Fraunhofer lines
70:Absorption lines
62:
41:
27:
3407:
3406:
3402:
3401:
3400:
3398:
3397:
3396:
3377:
3376:
3365:
3359:
3342:
3336:
3323:
3320:
3318:Further reading
3315:
3314:
3305:
3303:
3269:
3268:
3264:
3255:
3253:
3244:
3243:
3239:
3201:
3199:
3195:
3188:
3167:
3166:
3162:
3150:
3146:
3103:
3102:
3098:
3090:
3088:
3080:
3079:
3075:
3070:
3065:
3064:
3035:
3031:
3026:
2987:Fraunhofer line
2953:
955:Spectral lines
925:
869:
864:
858:
848:, known as the
833:
808:
800:self-absorption
791:
783:
763:
734:
709:
708:
667:
642:
641:
636:occurs via the
608:
583:
582:
553:
528:
527:
508:
507:
502:occurs via the
444:
427:
421:
397:
392:
368:
258:Fraunhofer line
250:
200:absorption line
175:) and a single
141:
77:
76:
75:
74:
73:
63:
54:
53:
52:
42:
33:
32:
31:
28:
17:
12:
11:
5:
3405:
3403:
3395:
3394:
3389:
3379:
3378:
3375:
3374:
3363:
3357:
3349:Academic Press
3340:
3334:
3319:
3316:
3313:
3312:
3282:(3): 367–474.
3262:
3237:
3193:
3186:
3160:
3144:
3096:
3072:
3071:
3069:
3066:
3063:
3062:
3028:
3027:
3025:
3022:
3021:
3020:
3015:
3010:
3005:
3000:
2994:
2989:
2984:
2979:
2974:
2969:
2964:
2959:
2952:
2949:
2946:
2945:
2943:
2940:
2939:100–118
2937:
2927:
2926:
2919:
2916:
2913:
2907:
2906:
2899:
2896:
2893:
2887:
2886:
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2799:
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2759:
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2503:
2497:
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2489:
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2483:
2477:
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2303:
2297:
2296:
2289:
2286:
2283:
2277:
2276:
2269:
2266:
2263:
2257:
2256:
2249:
2246:
2243:
2237:
2236:
2229:
2226:
2223:
2217:
2216:
2209:
2206:
2203:
2197:
2196:
2189:
2186:
2183:
2177:
2176:
2169:
2166:
2163:
2157:
2156:
2149:
2146:
2143:
2137:
2136:
2129:
2126:
2123:
2117:
2116:
2109:
2106:
2103:
2097:
2096:
2089:
2086:
2083:
2077:
2076:
2069:
2066:
2063:
2057:
2056:
2049:
2046:
2043:
2037:
2036:
2029:
2026:
2023:
2017:
2016:
2009:
2006:
2003:
1997:
1996:
1989:
1986:
1983:
1977:
1976:
1969:
1966:
1963:
1957:
1956:
1949:
1946:
1943:
1937:
1936:
1929:
1926:
1923:
1917:
1916:
1909:
1906:
1903:
1897:
1896:
1889:
1886:
1883:
1877:
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1869:
1866:
1863:
1857:
1856:
1849:
1846:
1843:
1837:
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1809:
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1803:
1797:
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1769:
1766:
1763:
1757:
1756:
1749:
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1709:
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1697:
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1689:
1686:
1683:
1677:
1676:
1669:
1666:
1663:
1657:
1656:
1649:
1646:
1643:
1637:
1636:
1629:
1626:
1623:
1617:
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1609:
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1603:
1597:
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1577:
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1569:
1566:
1563:
1557:
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1549:
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1517:
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1509:
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1497:
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1469:
1466:
1463:
1457:
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1449:
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1437:
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1429:
1426:
1423:
1417:
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1409:
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1403:
1397:
1396:
1389:
1386:
1383:
1377:
1376:
1369:
1366:
1363:
1357:
1356:
1349:
1346:
1343:
1337:
1336:
1329:
1326:
1323:
1317:
1316:
1309:
1306:
1303:
1297:
1296:
1289:
1286:
1283:
1277:
1276:
1269:
1266:
1263:
1257:
1256:
1249:
1246:
1243:
1237:
1236:
1229:
1226:
1223:
1217:
1216:
1209:
1206:
1203:
1197:
1196:
1189:
1186:
1183:
1177:
1176:
1169:
1166:
1163:
1157:
1156:
1149:
1146:
1143:
1137:
1136:
1129:
1126:
1123:
1117:
1116:
1109:
1106:
1103:
1097:
1096:
1089:
1086:
1083:
1077:
1076:
1069:
1066:
1063:
1057:
1056:
1049:
1046:
1043:
1037:
1036:
1029:
1026:
1023:
1017:
1016:
1009:
1006:
1003:
997:
996:
989:
986:
983:
977:
976:
969:
966:
963:
957:
956:
953:
950:
947:
936:Spectral lines
924:
921:
909:radio spectrum
905:Paschen series
868:
865:
857:
854:
832:
829:
807:
804:
790:
787:
782:
779:
762:
759:
758:
757:
746:
741:
737:
732:
728:
725:
722:
719:
716:
690:
679:
674:
670:
665:
661:
658:
655:
652:
649:
631:
620:
615:
611:
606:
602:
599:
596:
593:
590:
576:
565:
560:
556:
551:
547:
544:
541:
538:
535:
515:
493:
492:
470:
443:
440:
431:Doppler effect
423:Main article:
420:
417:
396:
393:
391:
388:
380:spectral width
367:
364:
355:diffuse series
332:, such as the
249:
246:
161:quantum system
140:
137:
64:
57:
56:
55:
45:Emission lines
43:
36:
35:
34:
29:
22:
21:
20:
19:
18:
15:
13:
10:
9:
6:
4:
3:
2:
3404:
3393:
3390:
3388:
3385:
3384:
3382:
3371:
3370:
3364:
3360:
3358:0-12-302850-7
3354:
3350:
3346:
3341:
3337:
3335:0-521-45504-9
3331:
3327:
3322:
3321:
3317:
3302:on 2013-01-14
3301:
3297:
3293:
3289:
3285:
3281:
3277:
3273:
3266:
3263:
3252:on 2015-09-24
3251:
3247:
3241:
3238:
3233:
3229:
3225:
3221:
3217:
3213:
3209:
3205:
3197:
3194:
3189:
3183:
3179:
3175:
3171:
3164:
3161:
3157:
3153:
3148:
3145:
3140:
3136:
3132:
3128:
3124:
3120:
3116:
3112:
3108:
3100:
3097:
3086:
3085:
3077:
3074:
3067:
3059:
3055:
3051:
3047:
3046:0-471-27663-4
3043:
3039:
3033:
3030:
3023:
3019:
3016:
3014:
3011:
3009:
3008:Spectral band
3006:
3004:
3001:
2998:
2997:Hydrogen line
2995:
2993:
2990:
2988:
2985:
2983:
2980:
2978:
2975:
2973:
2970:
2968:
2965:
2963:
2960:
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2936:
2932:
2929:
2928:
2924:
2920:
2917:
2914:
2912:
2909:
2908:
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2900:
2897:
2894:
2892:
2889:
2888:
2884:
2880:
2877:
2874:
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2869:
2868:
2864:
2860:
2857:
2854:
2852:
2849:
2848:
2844:
2840:
2837:
2834:
2832:
2829:
2828:
2824:
2820:
2817:
2814:
2812:
2809:
2808:
2804:
2800:
2797:
2794:
2792:
2789:
2788:
2784:
2780:
2777:
2774:
2772:
2769:
2768:
2764:
2760:
2757:
2754:
2752:
2749:
2748:
2744:
2740:
2737:
2734:
2732:
2729:
2728:
2724:
2720:
2717:
2714:
2712:
2709:
2708:
2704:
2700:
2697:
2694:
2692:
2689:
2688:
2685:
2682:
2679:
2677:
2674:
2673:
2669:
2665:
2662:
2659:
2657:
2654:
2653:
2650:
2647:
2644:
2642:
2639:
2638:
2634:
2630:
2627:
2624:
2622:
2619:
2618:
2614:
2610:
2607:
2604:
2602:
2599:
2598:
2594:
2590:
2587:
2584:
2582:
2579:
2578:
2574:
2570:
2567:
2564:
2562:
2559:
2558:
2554:
2550:
2547:
2544:
2542:
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2538:
2534:
2530:
2527:
2524:
2522:
2519:
2518:
2514:
2510:
2507:
2504:
2502:
2499:
2498:
2494:
2490:
2487:
2484:
2482:
2479:
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2434:
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2427:
2424:
2422:
2419:
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2414:
2410:
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2379:
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2359:
2358:
2354:
2350:
2347:
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2342:
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2338:
2334:
2330:
2327:
2324:
2322:
2319:
2318:
2314:
2310:
2307:
2304:
2302:
2299:
2298:
2294:
2290:
2287:
2284:
2282:
2279:
2278:
2274:
2270:
2267:
2264:
2262:
2259:
2258:
2254:
2250:
2247:
2244:
2242:
2239:
2238:
2234:
2230:
2227:
2224:
2222:
2219:
2218:
2214:
2210:
2207:
2204:
2202:
2199:
2198:
2194:
2190:
2187:
2184:
2182:
2179:
2178:
2174:
2170:
2167:
2164:
2162:
2159:
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2154:
2150:
2147:
2144:
2142:
2139:
2138:
2134:
2130:
2127:
2124:
2122:
2119:
2118:
2114:
2110:
2107:
2104:
2102:
2099:
2098:
2094:
2090:
2087:
2084:
2082:
2079:
2078:
2074:
2070:
2067:
2064:
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2054:
2050:
2047:
2044:
2042:
2039:
2038:
2034:
2030:
2027:
2024:
2022:
2019:
2018:
2014:
2010:
2007:
2004:
2002:
1999:
1998:
1994:
1990:
1987:
1984:
1982:
1979:
1978:
1974:
1970:
1967:
1964:
1962:
1959:
1958:
1954:
1950:
1947:
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1938:
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1927:
1924:
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1918:
1914:
1910:
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1902:
1899:
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1482:
1479:
1478:
1474:
1470:
1467:
1464:
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1434:
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1427:
1424:
1422:
1419:
1418:
1414:
1410:
1407:
1404:
1402:
1399:
1398:
1394:
1390:
1387:
1384:
1382:
1379:
1378:
1374:
1370:
1367:
1364:
1362:
1359:
1358:
1354:
1350:
1347:
1344:
1342:
1339:
1338:
1334:
1330:
1327:
1324:
1322:
1319:
1318:
1314:
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1302:
1299:
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1294:
1290:
1287:
1284:
1282:
1279:
1278:
1274:
1270:
1267:
1264:
1262:
1259:
1258:
1254:
1250:
1247:
1244:
1242:
1239:
1238:
1234:
1230:
1227:
1224:
1222:
1219:
1218:
1214:
1210:
1207:
1204:
1202:
1199:
1198:
1194:
1190:
1187:
1184:
1182:
1179:
1178:
1174:
1170:
1167:
1164:
1162:
1159:
1158:
1154:
1150:
1147:
1144:
1142:
1139:
1138:
1134:
1130:
1127:
1124:
1122:
1119:
1118:
1114:
1110:
1107:
1104:
1102:
1099:
1098:
1094:
1090:
1087:
1084:
1082:
1079:
1078:
1074:
1070:
1067:
1064:
1062:
1059:
1058:
1054:
1050:
1047:
1044:
1042:
1039:
1038:
1034:
1030:
1027:
1024:
1022:
1019:
1018:
1014:
1010:
1007:
1004:
1002:
999:
998:
994:
990:
987:
984:
982:
979:
978:
974:
970:
967:
964:
962:
959:
958:
951:
948:
945:
944:
941:
937:
932:
930:
923:Visible light
922:
920:
918:
914:
911:includes the
910:
906:
902:
898:
894:
890:
886:
882:
878:
874:
866:
863:
855:
853:
851:
847:
841:
839:
838:Voigt profile
830:
828:
826:
822:
818:
813:
812:Doppler shift
805:
803:
801:
797:
796:self reversal
788:
786:
780:
778:
776:
775:
769:
768:
760:
739:
735:
730:
726:
723:
720:
706:
702:
698:
694:
691:
672:
668:
663:
659:
656:
653:
639:
635:
632:
613:
609:
604:
600:
597:
594:
580:
577:
558:
554:
549:
545:
542:
539:
513:
505:
501:
498:
497:
496:
490:
486:
482:
478:
477:spectral band
474:
471:
468:
464:
460:
456:
452:
449:
448:
447:
441:
439:
437:
432:
426:
418:
416:
414:
410:
409:Auger process
406:
402:
394:
389:
387:
385:
381:
377:
376:spectral band
373:
365:
363:
361:
357:
356:
351:
350:
345:
344:
339:
338:Balmer series
335:
331:
327:
323:
319:
315:
310:
309:
305:
301:
300:
296:
292:
290:
289:Roman numeral
286:
282:
281:Roman numeral
278:
273:
271:
267:
263:
259:
255:
247:
245:
243:
239:
235:
230:
228:
224:
220:
216:
212:
208:
203:
201:
197:
196:emission line
192:
190:
186:
182:
178:
174:
173:atomic nuclei
170:
166:
162:
154:
150:
145:
138:
136:
134:
130:
126:
122:
118:
114:
110:
106:
102:
98:
97:spectral line
90:
86:
81:
71:
67:
61:
50:
46:
40:
26:
3387:Spectroscopy
3368:
3347:. New York:
3344:
3325:
3304:. Retrieved
3300:the original
3279:
3275:
3265:
3254:. Retrieved
3250:the original
3240:
3210:(1): 67–70.
3207:
3203:
3196:
3169:
3163:
3147:
3114:
3110:
3099:
3089:, retrieved
3083:
3076:
3032:
3013:Spectroscopy
2999:(21-cm line)
2942:Fm–Og
2751:protactinium
2121:praseodymium
935:
926:
885:Lyman series
875:of the full
873:visible band
870:
850:Dicke effect
845:
842:
834:
809:
799:
795:
792:
784:
772:
765:
764:
692:
633:
578:
499:
494:
472:
454:
450:
445:
428:
398:
369:
353:
349:sharp series
347:
341:
334:Lyman series
311:
307:
303:
302:
298:
294:
293:
279:by adding a
274:
265:
261:
251:
248:Nomenclature
231:
204:
199:
195:
193:
158:
115:in a narrow
96:
94:
3018:Splatalogue
2911:einsteinium
2891:californium
881:ultraviolet
823:shell in a
485:temperature
463:temperature
238:radio waves
219:temperature
3381:Categories
3306:2005-12-09
3256:2015-09-24
3091:2021-06-27
3068:References
2967:Bohr model
2261:dysprosium
2221:gadolinium
2161:promethium
1801:technetium
1781:molybdenum
1241:phosphorus
913:21-cm line
860:See also:
314:wavelength
277:ionization
242:gamma rays
109:absorption
3172:. Wiley.
3154:(1905). "
3139:0022-4073
3056:; and in
2935:oganesson
2871:berkelium
2831:americium
2811:plutonium
2791:neptunium
2341:ytterbium
2141:neodymium
2081:lanthanum
1981:tellurium
1861:palladium
1821:ruthenium
1741:zirconium
1701:strontium
1581:germanium
1441:manganese
1321:potassium
1201:aluminium
1181:magnesium
1021:beryllium
846:narrowing
724:∼
718:Δ
657:∼
651:Δ
598:∼
592:Δ
543:∼
537:Δ
318:multiplet
187:changing
169:molecules
163:(usually
125:molecules
117:frequency
3232:10031682
3117:: 4–50.
2951:See also
2711:actinium
2676:francium
2641:astatine
2621:polonium
2561:thallium
2501:platinum
2421:tungsten
2401:tantalum
2361:lutetium
2201:europium
2181:samarium
1961:antimony
1681:rubidium
1621:selenium
1421:chromium
1401:vanadium
1381:titanium
1361:scandium
1281:chlorine
1121:fluorine
1081:nitrogen
961:hydrogen
946:Element
901:infrared
889:hydrogen
461:and the
326:hydrogen
211:thallium
189:orbitals
185:electron
155:(bottom)
105:emission
3284:Bibcode
3212:Bibcode
3119:Bibcode
2933:–
2931:fermium
2771:uranium
2731:thorium
2601:bismuth
2541:mercury
2481:iridium
2441:rhenium
2381:hafnium
2321:thulium
2281:holmium
2241:terbium
2041:caesium
1901:cadmium
1841:rhodium
1761:niobium
1721:yttrium
1661:krypton
1641:bromine
1601:arsenic
1561:gallium
1341:calcium
1221:silicon
1001:lithium
952:Symbol
938:of the
825:Z-pinch
481:density
459:density
407:or the
270:species
236:, from
223:density
215:caesium
133:planets
3355:
3332:
3230:
3184:
3137:
3052:
3044:
2851:curium
2691:radium
2461:osmium
2301:erbium
2101:cerium
2061:barium
2001:iodine
1921:indium
1881:silver
1521:copper
1501:nickel
1481:cobalt
1261:sulfur
1161:sodium
1101:oxygen
1061:carbon
981:helium
917:cosmos
893:X-rays
821:plasma
352:, and
330:series
304:Fe III
213:, and
207:helium
198:or an
181:energy
177:photon
3024:Notes
2656:radon
2021:xenon
1301:argon
1041:boron
867:Bands
295:Cu II
227:stars
165:atoms
129:stars
121:atoms
113:light
68:with
3353:ISBN
3330:ISBN
3228:PMID
3182:ISBN
3135:ISSN
3050:ISBN
3042:ISBN
2581:lead
2521:gold
1541:zinc
1461:iron
1141:neon
817:star
221:and
131:and
123:and
3292:doi
3220:doi
3174:doi
3127:doi
3115:130
2918:Es
2915:99
2898:Cf
2895:98
2878:Bk
2875:97
2858:Cm
2855:96
2838:Am
2835:95
2818:Pu
2815:94
2798:Np
2795:93
2775:92
2758:Pa
2755:91
2738:Th
2735:90
2718:Ac
2715:89
2698:Ra
2695:88
2683:Fr
2680:87
2663:Rn
2660:86
2648:At
2645:85
2628:Po
2625:84
2608:Bi
2605:83
2588:Pb
2585:82
2568:Tl
2565:81
2548:Hg
2545:80
2528:Au
2525:79
2508:Pt
2505:78
2488:Ir
2485:77
2468:Os
2465:76
2448:Re
2445:75
2425:74
2408:Ta
2405:73
2388:Hf
2385:72
2368:Lu
2365:71
2348:Yb
2345:70
2328:Tm
2325:69
2308:Er
2305:68
2288:Ho
2285:67
2268:Dy
2265:66
2248:Tb
2245:65
2228:Gd
2225:64
2208:Eu
2205:63
2188:Sm
2185:62
2168:Pm
2165:61
2148:Nd
2145:60
2128:Pr
2125:59
2108:Ce
2105:58
2088:La
2085:57
2068:Ba
2065:56
2048:Cs
2045:55
2028:Xe
2025:54
2005:53
1988:Te
1985:52
1968:Sb
1965:51
1948:Sn
1945:50
1941:tin
1928:In
1925:49
1908:Cd
1905:48
1888:Ag
1885:47
1868:Pd
1865:46
1848:Rh
1845:45
1828:Ru
1825:44
1808:Tc
1805:43
1788:Mo
1785:42
1768:Nb
1765:41
1748:Zr
1745:40
1725:39
1708:Sr
1705:38
1688:Rb
1685:37
1668:Kr
1665:36
1648:Br
1645:35
1628:Se
1625:34
1608:As
1605:33
1588:Ge
1585:32
1568:Ga
1565:31
1548:Zn
1545:30
1528:Cu
1525:29
1508:Ni
1505:28
1488:Co
1485:27
1468:Fe
1465:26
1448:Mn
1445:25
1428:Cr
1425:24
1405:23
1388:Ti
1385:22
1368:Sc
1365:21
1348:Ca
1345:20
1325:19
1308:Ar
1305:18
1288:Cl
1285:17
1265:16
1245:15
1228:Si
1225:14
1208:Al
1205:13
1188:Mg
1185:12
1168:Na
1165:11
1148:Ne
1145:10
1028:Be
1008:Li
988:He
887:of
453:or
336:or
240:to
171:or
111:of
107:or
3383::
3351:.
3290:.
3280:30
3278:.
3274:.
3226:.
3218:.
3208:55
3206:.
3180:.
3158:".
3133:.
3125:.
3113:.
3109:.
3048:,
2778:U
2428:W
2008:I
1728:Y
1408:V
1328:K
1268:S
1248:P
1128:F
1125:9
1108:O
1105:8
1088:N
1085:7
1068:C
1065:6
1048:B
1045:5
1025:4
1005:3
985:2
968:H
965:1
949:Z
919:.
852:.
840:.
827:.
802:.
777:.
707:.
346:,
308:Fe
299:Cu
272:.
266:Ca
244:.
209:,
95:A
3361:.
3338:.
3309:.
3294::
3286::
3259:.
3234:.
3222::
3214::
3190:.
3176::
3141:.
3129::
3121::
745:)
740:6
736:r
731:/
727:1
721:E
715:(
678:)
673:4
669:r
664:/
660:1
654:E
648:(
619:)
614:3
610:r
605:/
601:1
595:E
589:(
564:)
559:2
555:r
550:/
546:1
540:E
534:(
514:r
491:.
262:K
51:)
47:(
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