2016A&A...593A.101K

Query : 2016A&A...593A.101K

2016A&A...593A.101K - Astronomy and Astrophysics, volume 593A101-101 (2016/9-1)

Stellar wind models of subluminous hot stars.

KRTICKA J., KUBAT J. and KRTICKOVA I.

Abstract (from CDS):

Context. Mass-loss rate is one of the most important stellar parameters. Mass loss via stellar winds may influence stellar evolution and modifies stellar spectrum. Stellar winds of subluminous hot stars, especially subdwarfs, have not been studied thoroughly.
Aims. We aim to provide mass-loss rates as a function of subdwarf parameters and to apply the formula for individual subdwarfs, to predict the wind terminal velocities, to estimate the influence of the magnetic field and X-ray ionization on the stellar wind, and to study the interaction of subdwarf wind with mass loss from Be and cool companions.
Methods. We used our kinetic equilibrium (NLTE) wind models with the radiative force determined from the radiative transfer equation in the comoving frame (CMF) to predict the wind structure of subluminous hot stars. Our models solve stationary hydrodynamical equations, that is the equation of continuity, equation of motion, and energy equation and predict basic wind parameters.
Results. We predicted the wind mass-loss rate as a function of stellar parameters, namely the stellar luminosity, effective temperature, and metallicity. The derived wind parameters (mass-loss rates and terminal velocities) agree with the values derived from the observations. The radiative force is not able to accelerate the homogeneous wind for stars with low effective temperatures and high surface gravities. We discussed the properties of winds of individual subdwarfs. The X-ray irradiation may inhibit the flow in binaries with compact components. In binaries with Be components, the winds interact with the disk of the Be star.
Conclusions. Stellar winds exist in subluminous stars with low gravities or high effective temperatures. Despite their low mass-loss rates, they are detectable in the ultraviolet spectrum and cause X-ray emission. Subdwarf stars may lose a significant part of their mass during the evolution. The angular momentum loss in magnetic subdwarfs with wind may explain their low rotational velocities. Stellar winds are especially important in binaries, where they may be accreted on a compact or cool companion.

Abstract Copyright: © ESO, 2016

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

Simbad objects: 78

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Number of rows : 78
N Identifier Otype ICRS (J2000)
RA 		ICRS (J2000)
DEC 		Mag U Mag B Mag V Mag R Mag I Sp type #ref
1850 - 2026 		#notes
1 Feige 11 HS* 01 04 21.6747168600 +04 13 37.054495956 10.847 11.826 12.065 12.183 12.324 sdB2VIHe4 136 0
2 GD 687 HS* 01 10 18.6196714608 -34 00 25.710906636   13.89 14.08 14.39   sdBHe1 40 0
3 * phi Per Be* 01 43 39.6379691568 +50 41 19.433124998 3.10 4.02 4.06 3.90 3.88 B1.5V:e-shell 594 0
4 BD+37 442 HS* 01 58 33.4346638392 +38 34 23.842803324   9.69 9.92     sdOHe 73 0
5 PG 0217+155 HS* 02 20 35.6035638816 +15 44 06.919456488   15.08       sdOB 16 0
6 CPD-71 172 ** 02 53 30.6948092520 -71 22 31.730091240   10.82 10.63     F2.5IV+sdOHe-wk 27 0
7 PN HFG 1 PN 03 03 47.0096763024 +64 54 35.517676320     14.56 13.99   ~ 114 0
8 LS I +63 198 HS* 03 29 05.6683420320 +64 04 42.157890228 11.71 13.18 13.20 12.96 13.2 sdOB 22 0
9 V* IQ Cam HS* 04 26 06.8650883976 +54 28 17.101122600 14.21 14.86 14.66     sdB 66 0
10 KUV 04421+1416 HS* 04 44 56.8983457992 +14 21 50.176351836   15.28       sdB 46 0
11 LB 1766 HS* 04 59 18.7820628456 -53 52 54.594838668 10.88 12.25 12.91     sdBHe 20 0
12 HD 269696 HS* 05 31 40.3594532592 -69 53 02.153902236 9.74 10.92 11.15     sdB+dM 202 0
13 CPD-20 1123 HS* 06 06 13.3951675848 -20 21 07.275405420   11.75 11.80 11.84 11.90 sdB3VHe15 37 0
14 HD 49798 HXB 06 48 04.7001531360 -44 18 58.436036028 6.758 8.017 8.287 8.391 8.543 sdO6 339 0
15 BD+34 1543 HS* 07 10 07.7039318016 +34 24 53.808705504   10.29 10.17     sdB+F? 34 0
16 V* V470 Cam HS* 07 10 42.0513241680 +66 55 43.521505680           sdB+dM 118 0
17 HD 58978 Be* 07 26 59.4826856664 -23 05 09.689679528 4.51 5.45 5.56 7.05   B0.5IVe 248 0
18 CD-31 4800 HS* 07 36 30.1950207312 -32 12 43.685045964 9 10.26 10.48 10.81   sdO8p 75 0
19 BD-03 2179 HS* 08 02 14.8870205088 -03 58 16.343922324 8.8 10.044 10.29 10.64 10.60 sdO 56 0
20 BD+75 325 HS* 08 10 49.4903003712 +74 57 57.931973676 8.002 9.23 9.50 9.698 9.884 sdO5 267 0
21 GALEX J082053.6+000843 HS* 08 20 53.5359673248 +00 08 43.502407800   15.03 15.17 15.54 15.91 sdB 48 0
22 V* DT Lyn HS* 09 14 55.3780066224 +45 23 41.396157600   14.92       sdBO 34 0
23 CD-45 5058 HS* 09 20 10.1317907208 -45 31 54.942917700 9.81 11.03 11.33 11.62   sdO 62 0
24 BD+37 1977 HS* 09 24 26.3929652664 +36 42 53.295009624   9.86 10.15     sdO 52 0
25 US 708 HS* 09 33 20.8631859264 +44 17 05.495440452   18.5 18.8     sdOHe 103 0
26 PG 0958-116 HS* 10 00 41.8235310624 -11 51 34.585561008   15.01 15.26     sdB 27 0
27 ASAS J102322-3737.0 HS* 10 23 21.8946607008 -37 36 59.909184792   11.43 11.51     sdB+dM 30 0
28 EC 10246-2707 HS* 10 26 56.4747793032 -27 22 57.097779564   14.56 14.77 14.85   sdB+dM 31 0
29 V* DN Leo Pu* 10 38 55.2343433712 +10 03 48.486337812   9.76 9.93     Bp 150 0
30 Feige 34 HS* 10 39 36.7358839104 +43 06 09.212615280 9.613 10.91 11.14 11.319 11.464 sdOp 731 0
31 CD-48 6027 HS* 10 54 40.5601100160 -48 47 02.815818036 10.92 11.99 12.12 12.39   sdO 127 0
32 Feige 36 HS* 11 04 31.6443383808 +24 39 42.687580896   12.87 12.78     sdB 59 0
33 PG 1104+243 HS* 11 07 26.2324234560 +24 03 11.108174724   11.49 11.39     sdOB+G2V 36 0
34 Feige 48 HS* 11 47 14.4978515760 +61 15 31.789400364   13.12 13.28     sdB 125 0
35 PG 1219+534 HS* 12 21 29.0914917288 +53 04 36.796062144   12.41       sdB 90 1
36 PG 1232-136 HS* 12 35 18.7430526168 -13 55 08.879064096   13.06 13.27     sdB 34 0
37 BD+18 2647 HS* 12 41 51.7899961800 +17 31 19.750566756 10.261 11.70 11.63 11.969 12.159 sdOpec 185 1
38 BD-07 3477 HS* 12 44 20.2386233232 -08 40 16.846099536   10.46 10.594 10.895   sdB2VIIHe3 303 1
39 [RWW88] CS 124636.2-631549 HS* 12 49 37.6226470128 -63 32 09.899403252   14.87 14.59 14.80 14.11 sdB6 27 0
40 Feige 80 HS* 13 19 53.6033701512 +12 03 58.272912072   11.281 11.410 11.496   sdO+G1V 32 0
41 PG 1325+102 HS* 13 27 48.5600155368 +09 54 51.049107756   13.73 13.98 14.29   sdBO 60 1
42 V* NY Vir HS* 13 38 48.1466908176 -02 01 49.207286748   13.43 13.66 13.75   sdB1VIIHe1 237 1
43 Feige 87 HS* 13 40 14.6950103088 +60 52 47.566392996   11.56 11.71     sdB+G4V 49 0
44 M 3 GlC 13 42 11.62 +28 22 38.2     6.39     ~ 2593 0
45 NAME vZ 1128 pA* 13 42 16.7509672392 +28 26 00.616904988   14.77 15.04 15.50   O8p 80 0
46 CD-46 8926 HS* 13 53 08.2139106408 -46 43 42.314548008   11.04 11.30     sdO 51 0
47 CD-30 11223 HS* 14 11 16.1541452856 -30 53 03.700889340   12.101 12.296 12.659 12.541 sdB+DA 78 0
48 HD 127493 HS* 14 32 21.4926471192 -22 39 25.646693688 8.64 9.74 10.08     sdOHe 110 0
49 HD 128220 SB* 14 35 15.7845026736 +19 12 54.526317408   8.724 8.503     G0IIIn+sdO 125 0
50 PG 1432+159 HS* 14 35 18.9439382472 +15 40 14.376188748   13.63       sdB 36 1
51 FBS 1531+381 HS* 15 33 49.4441301600 +37 59 28.095378720     13.08     sdB+dM 52 0
52 PG 1605+072 HS* 16 08 03.6872637792 +07 04 28.748468964   12.53 12.83 13.18   sdB0.2VIHe3 136 0
53 HD 144941 pA* 16 09 24.5513020968 -27 13 38.184011148 9.45 10.17 10.02     B8 96 1
54 PG 1621+476 HS* 16 22 56.6652852936 +47 30 51.128501040   16.07 16.19     sdB+dM 61 0
55 LS IV -12 1 HS* 16 23 43.9896591936 -12 12 33.642833328 10.06 11.14 11.17     sdO 39 0
56 HD 149382 HS* 16 34 23.3333693424 -04 00 52.030152000 7.518 8.661 8.943 9.070 9.205 sdB 149 1
57 PG 1718+519 HS* 17 19 45.3514315416 +51 52 10.717011948   13.86 13.75 13.81   sdB+G4V 20 0
58 PN A66 41 PN 17 29 02.0258857104 -15 13 04.482114960   16.06 15.95     sdO 146 1
59 BD+29 3070 HS* 17 38 21.2004399672 +29 08 47.348080656   10.55 10.45     sdOB+F/G 35 0
60 BD+39 3226 HS* 17 46 31.9115217336 +39 19 09.070120164   9.89 10.18     sdOHe 47 0
61 PN A66 46 PN 18 31 18.5910709560 +26 56 12.110750088       15.050   O9k 190 0
62 CD-51 11879 HS* 19 02 11.7428660328 -51 30 09.561616380   11.44 11.55     sdO 43 0
63 UCAC4 698-068637 HS* 19 26 34.1086958928 +49 30 29.555956908   14.548 14.859 15.096   sdB 44 1
64 KPD 1930+2752 HS* 19 32 14.8088063952 +27 58 35.445679608 12.80 13.75 13.82     sdB 167 0
65 Kepler-451 HS* 19 38 32.6123816016 +46 03 59.135231952   12.17 12.69 12.46 12.399 sdB+dM 103 0
66 Kepler-70 HS* 19 45 25.4745687168 +41 05 33.882248544 13.80 14.71 14.87 15.43 15.72 sdB 81 1
67 KPD 1946+4340 HS* 19 47 42.8876526504 +43 47 30.754543092 13.05 14.06 14.23 14.92   sdOB+D 62 0
68 DENIS J200816.4-175310 HS? 20 08 16.3426899768 -17 53 10.633167564   16.8   17.1 17.07 ~ 19 0
69 V* V1828 Aql HS* 20 20 00.4587151080 +04 37 56.517736296   12.9   13.34   sdOB+dM 77 1
70 LS IV +10 9 HS* 20 43 02.4781026312 +10 34 21.001039644 10.51 11.71 12.06     sdO 39 0
71 LS IV -14 116 HS* 20 57 38.8746228912 -14 25 43.991016852 11.63 12.73 13.02 13.28   sdB0.5VIIHe18 89 0
72 * f01 Cyg Be* 20 59 49.5541247496 +47 31 15.363746436 3.77 4.71 4.75 4.62 4.63 B1.5Vnne 514 0
73 KPD 2109+4401 HS* 21 11 47.6445824136 +44 13 50.620755936 12.14 13.11 13.30 13.64   sdB 72 0
74 BD+28 4211 HS* 21 51 11.0221915656 +28 51 50.367627468 8.922 10.25 10.58 10.656 10.831 sdO2VIIIHe5 837 0
75 BD+25 4655 HS* 21 59 41.9748629928 +26 25 57.403455672 8.27 9.39 9.68     sdO6 130 0
76 HS 2231+2441 HS* 22 34 21.4832585640 +24 56 57.392918196     14.20     sdB+dM 58 0
77 Feige 110 HS* 23 19 58.3996844256 -05 09 56.171142864 10.360 11.45 11.50 11.970 12.145 sdO8VIIIHe5 673 1
78 HS 2333+3927 HS* 23 35 42.5025647712 +39 44 27.064626936     14.53     sdOB 48 0

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