2011A&A...535A..32N


C.D.S. - SIMBAD4 rel 1.7 - 2019.08.24CEST10:27:35

2011A&A...535A..32N - Astronomy and Astrophysics, volume 535A, 32-32 (2011/11-1)

L-band spectroscopy of galactic OB-stars.

NAJARRO F., HANSON M.M. and PULS J.

Abstract (from CDS):

Mass-loss, occurring through radiation driven supersonic winds, is a key issue throughout the evolution of massive stars. Two outstanding problems are currently challenging the theory of radiation-driven winds: wind clumping and the weak-wind problem. We seek to obtain accurate mass-loss rates of OB stars at different evolutionary stages to constrain the impact of both problems in our current understanding of massive star winds. We perform a multi-wavelength quantitative analysis of a sample of ten Galactic OB-stars by means of the atmospheric code cmfgen, with special emphasis on the L-band window. A detailed investigation is carried out on the potential of Brα and Pfγ as mass-loss and clumping diagnostics. For objects with dense winds, Brα samples the intermediate wind while Pfγ maps the inner one. In combination with other indicators (UV, Hα, Brγ) these lines enable us to constrain the wind clumping structure and to obtain ``true'' mass-loss rates. For objects with weak winds, Brα emerges as a reliable diagnostic tool to constrain {dot}(M). The emission component at the line Doppler-core superimposed on the rather shallow Stark absorption wings reacts very sensitively to mass loss already at very low {dot}(M) values. On the other hand, the line wings display similar sensitivity to mass loss as Hα, the classical optical mass loss diagnostics. Our investigation reveals the great diagnostic potential of L-band spectroscopy to derive clumping properties and mass-loss rates of hot star winds. We are confident that Brα will become the primary diagnostic tool to measure very low mass-loss rates with unprecedented accuracy.

Abstract Copyright:

Journal keyword(s): infrared: stars - stars: early-type - stars: winds, outflows - stars: mass-loss

Simbad objects: 22

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Number of rows : 22

N Identifier Otype ICRS (J2000)
RA
ICRS (J2000)
DEC
Mag U Mag B Mag V Mag R Mag I Sp type #ref
1850 - 2019
#notes
1 NAME SMC G 00 52 38.0 -72 48 01   2.79 2.2     ~ 9018 1
2 HD 7113 Em* 01 09 13.066 -73 11 38.92     11.7     ~ 114 0
3 * alf Cam s*b 04 54 03.0103983 +66 20 33.636467 3.47 4.34 4.29 4.18 4.18 O9Ia 632 1
4 HD 33654 * 05 14 44.2726775919 +53 12 50.211652923 6.280 6.240 6.160     A0V 41 0
5 Cl Collinder 69 OpC 05 35 06 +09 56.0     2.8     ~ 209 0
6 * lam Ori A Em* 05 35 08.277 +09 56 02.96 2.17 3.48 3.47     O8III((f)) 478 0
7 * eps Ori s*b 05 36 12.81335 -01 12 06.9089 0.48 1.51 1.69 1.76 1.93 B0Ia 852 0
8 * sig Ori Y*O 05 38 44.7665260139 -02 36 00.284709290 2.54 3.58 3.79 3.87 4.11 O9.5V 729 0
9 * zet Pup BY* 08 03 35.04754 -40 00 11.3321 0.89 1.98 2.25 2.36 2.58 O4I(n)fp 1082 1
10 HD 76341 Em* 08 54 00.6139143219 -42 29 08.767038173 6.88 7.392 7.163 8.08   O9.2IV 87 1
11 HD 93129A SB* 10 43 57.4584179931 -59 32 51.395115271 6.46 7.478 7.310 7.84   O2If* 140 0
12 * tau Sco * 16 35 52.9528530 -28 12 57.661515 1.55 2.56 2.81 2.93 3.18 B0.2V 839 0
13 NAME Arches Cluster Cl* 17 45 50.5 -28 49 28           ~ 607 0
14 * alf Lyr dS* 18 36 56.33635 +38 47 01.2802 0.03 0.03 0.03 0.07 0.10 A0Va 2467 0
15 Ass Cyg OB 2 As* 20 33.2 +41 19           ~ 745 0
16 Schulte 7 *iA 20 33 14.1095790591 +41 20 21.903381641 12.24 12.00 10.55     O3If* 124 0
17 BD+40 4227A ** 20 33 15.0780900764 +41 18 50.478859468 10.42 10.27 8.98 8.03 6.83 O6Ib(fc)+O4.5:III:(fc) 210 0
18 Schulte 8C *iA 20 33 17.9821559015 +41 18 31.192311433 12.2 11.43 10.19     O4.5III(fc) 72 0
19 * lam Cep s*b 22 11 30.5750839949 +59 24 52.147736074 4.55 5.29 5.05 4.77 4.62 O6.5I(n)fp 639 1
20 * 10 Lac ** 22 39 15.6786372 +39 03 00.971152 3.650 4.670 4.880 4.98 5.19 O9V 713 0
21 HD 217086 Y*O 22 56 47.19030 +62 43 37.6487 7.88 8.30 7.66     O7Vnn((f))z 236 0
22 HD 219190 PM* 23 14 07.8749880491 -08 23 14.127267286   9.19 8.47     G3IV 16 0

    Equat.    Gal    SGal    Ecl

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2019.08.24-10:27:35

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