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In most situations, the total emission by the free-free process far exceeds the recombination radiation, but the recombination radiation can introduce characteristic spectral features at ionisation thresholds in the continuum radiation. For
Hydrogen, the highest ionisation threshold, called the Lyman
301:
In a preliminary paper the author has given the wave-length of more than one hundred and thirty lines in the region of the spectrum lying between the values 1850 and 1030 tenth metres. It is the object of the present paper to compare the results obtained by the author with those given by
Schumann; to
404:
Flury, Sophia R.; Jaskot, Anne E.; Ferguson, Harry C.; Worseck, Gábor; Makan, Kirill; Chisholm, John; Saldana-Lopez, Alberto; Schaerer, Daniel; McCandliss, Stephan; Wang, Bingjie; Ford, N. M.; Heckman, Timothy; Ji, Zhiyuan; Giavalisco, Mauro; Amorin, Ricardo (2022-05-01).
472:
Flury, Sophia R.; Jaskot, Anne E.; Ferguson, Harry C.; Worseck, Gábor; Makan, Kirill; Chisholm, John; Saldana-Lopez, Alberto; Schaerer, Daniel; McCandliss, Stephan R.; Xu, Xinfeng; Wang, Bingjie; Oey, M. S.; Ford, N. M.; Heckman, Timothy; Ji, Zhiyuan (2022-05-01).
168:—LyC are predominantly UV-C. The photon absorption process leading to the ionization of atomic hydrogen can occur in reverse: an electron and a proton can collide and form atomic hydrogen. If the two particles were traveling slowly (so that
172:
can be ignored), then the photon the atom emits upon its creation will theoretically be 13.6 eV (in reality, the energy will be less if the atom is formed in an excited state). At faster speeds, the excess (kinetic) energy is radiated (but
391:
Lyman limit The short-wavelength end of the hydrogen Lyman series, at 91.2 nm. It corresponds to the energy required for an electron in the hydrogen ground state to jump completely out of the atom, leaving the atom
181:) as photons of lower wavelength (higher energy). Therefore, photons with energies above 13.6 eV are emitted by the combination of energetic protons and electrons forming atomic hydrogen, and emission from
113:
wavelengths of light may be absorbed. This forms a continuum in the energy spectrum; the spectrum is continuous rather than composed of many discrete lines, which are seen at lower energies.
101:. In the case of neutral atomic hydrogen, the minimum ionization energy is equal to the Lyman limit, where the photon has enough energy to completely ionize the atom, resulting in a free
97:
is thus named after him. All the wavelengths in the Lyman series are in the ultraviolet band. This quantized absorption behavior occurs only up to an energy limit, known as the
370:
Limit, corresponds to an energy of 13.6 eV or an wavelength of 912Ă…. Recombination radiation from
Hydrogen at wavelengths shorter than this is called the "Lyman continuum".
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describe the apparatus used in this research and to call attention to some new facts which have come to light since the publication of the first notice.
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367:. Fundamentals of Astrophysics. India: Inter-University Centre for Astronomy and Astrophysics.
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407:"The Low-redshift Lyman Continuum Survey. I. New, Diverse Local Lyman Continuum Emitters"
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222:- One of the two galaxies in the local universe that 'leaks' Lyman continuum photons.
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will also ionize a hydrogen atom, there are far fewer of them emitted from a star's
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259:(1906), "The Spectrum of Hydrogen in the Region of Extremely Short Wave-Length",
475:"The Low-redshift Lyman Continuum Survey. II. New Insights into LyC Diagnostics"
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228:- The second galaxy in the local universe that 'leaks' Lyman continuum photons.
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Photons emitted from stars at photon energies above the Lyman limit
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319:"An Extension of the Spectrum in the Extreme Ultra-Violet"
234:- Many nearby Green Peas are confirmed LyC 'leakers'.
261:
Memoirs of the
American Academy of Arts and Sciences
124:The Lyman limit is at the wavelength of 91.2
385:. A Dictionary of Astronomy. 1997. Archived from
132:), corresponding to a frequency of 3.29 million
360:Dipankar Bhattacharya (August–December 2003).
355:
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109:. Above this energy (below this wavelength),
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411:The Astrophysical Journal Supplement Series
19:"LyC" redirects here. For other uses, see
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144:. LyC energies are mostly in the
85:absorbs light only at specific
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29:(abbrev. LyC), shortened to
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18:
479:The Astrophysical Journal
510:10.3847/1538-4357/ac61e4
442:10.3847/1538-4365/ac5331
150:electromagnetic spectrum
27:Lyman continuum photons
362:"Matter and Radiation"
121:
47:active galactic nuclei
546:Emission spectroscopy
119:
77:, from 1906 to 1914,
31:Ly continuum photons
21:LYC (disambiguation)
501:2022ApJ...930..126F
433:2022ApJS..260....1F
335:1914Natur..93..241L
273:1906MAAAS..13..125L
210:Lyman-break galaxy
205:Lyman-alpha forest
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69:LyC. Working from
389:on May 23, 2011.
99:ionization energy
75:ultraviolet light
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551:Hydrogen physics
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344:10.1038/093241a0
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281:10.2307/25058084
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200:Lyman-alpha blob
120:The Lyman Series
73:'s discovery of
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315:Lyman, Theodore
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257:Lyman, Theodore
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226:Tololo-1247-232
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148:portion of the
83:atomic hydrogen
71:Victor Schumann
51:photon energies
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267:(3): 125–146,
263:, New Series,
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170:kinetic energy
81:observed that
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146:ultraviolet C
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138:photon energy
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41:emitted from
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387:the original
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238:Reionization
215:Lyman series
195:Balmer limit
183:photoionized
156:). Although
154:Lyman series
123:
110:
95:Lyman series
34:
30:
26:
25:
166:photosphere
105:and a free
91:wavelengths
87:frequencies
55:Lyman limit
35:Lyc photons
540:Categories
492:2203.15649
485:(2): 126.
424:2201.11716
244:References
232:Pea galaxy
185:hydrogen.
162:gamma-rays
128:(912
93:) and the
53:above the
37:, are the
527:247778972
519:0004-637X
459:246294865
451:0067-0049
289:0096-6134
179:conserved
67:absorbing
417:(1): 1.
392:ionized.
317:(1914),
297:25058084
189:See also
177:must be
175:momentum
140:of 13.6
107:electron
59:Hydrogen
497:Bibcode
429:Bibcode
331:Bibcode
269:Bibcode
220:Haro 11
63:ionized
39:photons
525:
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457:
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323:Nature
295:
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158:X-rays
136:and a
103:proton
523:S2CID
487:arXiv
455:S2CID
419:arXiv
365:(PDF)
293:JSTOR
152:(see
43:stars
515:ISSN
447:ISSN
285:ISSN
160:and
89:(or
505:doi
483:930
437:doi
415:260
339:doi
277:doi
134:GHz
111:all
65:by
61:is
49:at
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352:^
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327:93
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265:13
142:eV
126:nm
57:.
529:.
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130:Ă…
23:.
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