28:
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in the region responsible for the absorption. At cooler stellar temperatures, the density most strongly affects the strength of the discontinuity and this can be used to classify stars on the basis of their
121:, usually when the Balmer lines themselves are strongly in emission. Other hydrogen spectral series also show bound-free absorption and hence a continuum discontinuity, but the Balmer jump in the near
218:
Slettebak, A.; Stock, J. (1957). "Classification of Early Type Stars of High
Luminosity with Objective Prism Spectra of Low Dispersion. With 7 figures".
245:
Knigge, Christian; Long, Knox S.; Wade, Richard A.; Baptista, Raymundo; Horne, Keith; Hubeny, Ivan; Rutten, Rene G. M. (1998). "Hubble Space
Telescope
145:. This effect is strongest in A class stars, but in hotter stars temperature has a much larger effect on the Balmer jump than surface gravity.
107:
118:
44:
335:
Scargle, J. D.; Erickson, E. F.; Witteborn, F. C.; Strecker, D. W. (1978). "Infrared excesses in early-type stars - Gamma
Cassiopeiae".
296:"Electron temperature determination from nebular continuum emission in planetary nebulae and the importance of temperature fluctuations"
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27:
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35:. The jump in this plot appears around 920 nm (instead of the intrinsic 364.5 nm) due to cosmological
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370:
Bessell, Michael S. (2007). "Measuring the Balmer Jump and the
Effective Gravity in FGK Stars".
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The strength of the continuum absorption, and hence the size of the Balmer jump, depends on
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55:(B7 III) on the bottom. The vertical blue line represents the limit of the Balmer series.
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393:
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176:"Statistical-Equilibrium Model Atmospheres for Early-Type Stars. I. Hydrogen Continua"
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Observations of the Nova‐like
Cataclysmic Variable UX Ursae Majoris".
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of a hydrogen atom (bound-free absorption), which creates a continuum
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384:
42:
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Balmer discontinuity on the observational spectrum of the star
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In some cases the Balmer discontinuity can show continuum
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300:Monthly Notices of the Royal Astronomical Society
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421:International Astronomical Union Symposium
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417:"The effective temperatures of hot stars"
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7:
82:on either side of the limit of the
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294:Liu, X.-W.; Danziger, J. (1993).
1:
125:has been the most observed.
114:shorter than 364.5 nm.
220:Zeitschrift für Astrophysik
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47:Balmer jump of two stars:
468:Astronomical spectroscopy
442:10.1017/S0074180900116614
251:The Astrophysical Journal
174:Mihalas, Dimitri (1967).
102:directly from the second
90:, at approximately 364.5
415:Crowther, P. A. (1997).
51:(O9.7 V) on the top and
321:10.1093/mnras/263.1.256
56:
40:
337:Astrophysical Journal
180:Astrophysical Journal
71:is the difference of
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30:
65:Balmer discontinuity
18:Balmer discontinuity
433:1997IAUS..189..137C
394:2007PASP..119..605B
349:1978ApJ...224..527S
312:1993MNRAS.263..256L
273:1998ApJ...499..414K
232:1957ZA.....42...67S
192:1967ApJ...149..169M
155:Lyman-break galaxy
94:. It is caused by
80:continuum spectrum
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98:being completely
16:(Redirected from
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463:Hydrogen physics
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378:(856): 605–615.
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264:astro-ph/9801206
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139:surface gravity
49:Epsilon Orionis
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281:10.1086/305617
257:(1): 414–428.
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104:energy level
69:Balmer break
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427:: 137–146.
306:: 256–266.
130:temperature
112:wavelengths
61:Balmer jump
457:Categories
161:References
143:luminosity
141:and hence
108:absorption
53:Beta Tauri
385:0706.2739
96:electrons
73:intensity
149:See also
119:emission
88:hydrogen
37:redshift
429:Bibcode
390:Bibcode
345:Bibcode
343:: 527.
308:Bibcode
269:Bibcode
247:Eclipse
228:Bibcode
188:Bibcode
186:: 169.
134:density
100:ionized
77:stellar
75:of the
226:: 67.
33:Icarus
380:arXiv
259:arXiv
67:, or
132:and
59:The
437:doi
425:189
398:doi
376:119
353:doi
341:224
316:doi
304:263
277:doi
255:499
196:doi
184:149
110:at
86:of
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123:UV
92:nm
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20:)
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