2002A&A...386L...5L


Query : 2002A&A...386L...5L

2002A&A...386L...5L - Astronomy and Astrophysics, volume 386, L5-8 (2002/4-4)

Hydrogen infrared recombination lines as a diagnostic tool for the geometry of the circumstellar material of hot stars.

LENORZER A., DE KOTER A. and WATERS L.B.F.M.

Abstract (from CDS):

We have analysed the infrared hydrogen recombination lines of a sample of well studied hot massive stars observed with the Infrared Space Observatory. Our sample contains stars from several classes of objects, whose circumstellar environment is believed to be dominated by an ionized stellar wind (the Luminous Blue Variables) or by a dense disk-like geometry (Be stars and B[e] stars). We show that hydrogen infrared recombination lines can be used as a diagnostic tool to constrain the geometry of the ionized circumstellar material. The line strengths are sensitive to the density of the emitting gas. High densities result in optically thick lines for which line strengths are only dependent on the emitting surface. Low density gas produces optically thin lines which may be characterized by Menzel case B recombination. The ISO observations show that stellar winds are dominated by optically thin HI recombination lines, while disks are dominated by optically thick lines. Disks and winds are well separated in a diagnostic diagram using the Hu(14-6)/Brα and the Hu(14-6)/Pfγ line flux ratios. This diagnostic tool is useful to constrain the nature of hot star environments in case they are highly obscured, for instance while they are still embedded in their natal molecular cloud.

Abstract Copyright:

Journal keyword(s): stars: circumstellar matter - early-type - emission-line - mass loss - winds

Simbad objects: 18

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Number of rows : 18
N Identifier Otype ICRS (J2000)
RA
ICRS (J2000)
DEC
Mag U Mag B Mag V Mag R Mag I Sp type #ref
1850 - 2022
#notes
1 * gam Cas Be* 00 56 42.5317 +60 43 00.265 1.18 2.29 2.39 2.32 2.40 B0.5IVpe 1170 2
2 HD 45677 Be* 06 28 17.4219710352 -13 03 11.128860972 7.86 8.52 8.50 8.11 8.01 B2IV/V[e] 318 0
3 * kap CMa Be* 06 49 50.4593263 -32 30 30.522482 2.73 3.68 3.89 3.91 4.05 B1.5Ve 277 0
4 V* HZ CMa Be* 06 50 23.3482557912 -31 42 21.808309320   5.829 5.747     B6IVe+A 85 0
5 * ome CMa Be* 07 14 48.6538664 -26 46 21.609714 2.90 3.64 3.82 3.80 3.90 B2.5Ve 341 0
6 * eta Car Em* 10 45 03.5377808928 -59 41 04.051599720 6.37 7.03 6.48 4.90 4.41 OBepec 2332 0
7 HD 94878 EB* 10 55 58.9149262296 -60 23 33.436864428 8.67 9.37 8.70 8.07   B0/2eq 150 0
8 V* AG Car WR* 10 56 11.5781414448 -60 27 12.810673260 7.00 7.57 6.96 7.73   WN11h 613 0
9 * del Cen Be* 12 08 21.4976373 -50 43 20.738614 1.51 2.39 2.52 2.48 2.62 B2Vne 301 0
10 EM* MWC 922 Be* 18 21 16.0519243728 -13 01 25.511760192     13.80 13.65   B[e] 86 0
11 * 12 Vul Be* 19 51 04.1083085616 +22 36 36.172997964 4.15 4.84 4.96 4.98 5.12 B2.5Ve 182 0
12 * b02 Cyg Be* 20 09 25.6190611128 +36 50 22.633958400 4.03 4.80 4.93     B2.5Ve 256 0
13 * P Cyg s*b 20 17 47.2020844 +38 01 58.552724 4.66 5.24 4.82 4.28 4.02 B1-2Ia-0ep 1154 1
14 EM* MWC 349 ** 20 32 45.499080 +40 39 36.74124   15.88 13.15 12.13   Bep 756 0
15 HD 200775 Ae* 21 01 36.9205762896 +68 09 47.789578836 7.34 7.754 7.427 8.13   B2Ve 531 0
16 * bet Cep bC* 21 28 39.5968513 +70 33 38.574681 2.05 3.01 3.23 3.33 3.55 B0.5IIIs 701 0
17 HD 206773 Be* 21 42 24.1853979312 +57 44 09.795762276 6.30 7.10 6.87     B0V:pe 159 0
18 * omi Aqr Be* 22 03 18.8440292 -02 09 19.306758 4.22 4.64 4.69 4.70 4.74 B5V 260 0

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2022.08.09-03:28:39

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