2015A&A...579A.111K


C.D.S. - SIMBAD4 rel 1.7 - 2020.07.10CEST02:28:54

2015A&A...579A.111K - Astronomy and Astrophysics, volume 579A, 111-111 (2015/7-1)

X-ray irradiation of the winds in binaries with massive components.

KRTICKA J., KUBAT J. and KRTICKOVA I.

Abstract (from CDS):

Binaries with hot massive components are strong X-ray sources. Besides the intrinsic X-ray emission of individual binary members originating in their winds, X-ray emission stems from the accretion on the compact companion or from wind collision. Since hot star winds are driven by the light absorption in the lines of heavier elements, wind acceleration is sensitive to the ionization state. Therefore, the over-ionization induced by external X-ray source strongly influences the winds of individual components. We studied the effect of external X-ray irradiation on hot star winds. We used our kinetic equilibrium (NLTE) wind models to estimate the influence of external X-ray ionization for different X-ray luminosities and source distances. The models are calculated for parameters typical of O stars. The influence of X-rays is given by the X-ray luminosity, by the optical depth between a given point and the X-ray source, and by a distance to the X-ray source. Therefore, the results can be interpreted in the diagrams of X-ray luminosity vs. the optical depth parameter. X-rays are negligible in binaries with low X-ray luminosities or at large distances from the X-ray source. The influence of X-rays is stronger for higher X-ray luminosities and in closer proximity of the X-ray source. There is a forbidden area with high X-ray luminosities and low optical depth parameters, where the X-ray ionization leads to wind inhibition. There is excellent agreement between the positions of observed stars in these diagrams and our predictions. All wind-powered high-mass X-ray binary primaries lie outside the forbidden area. Many of them lie close to the border of the forbidden area, indicating that their X-ray luminosities are self-regulated. We discuss the implications of our work for other binary types. X-rays have a strong effect on the winds in binaries with hot components. The magnitude of the influence of X-rays can be estimated from the position of a star in the diagram of X-ray luminosity vs. the optical depth parameter.

Abstract Copyright:

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

Simbad objects: 55

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Number of rows : 55

N Identifier Otype ICRS (J2000)
RA
ICRS (J2000)
DEC
Mag U Mag B Mag V Mag R Mag I Sp type #ref
1850 - 2020
#notes
1 V* AO Cas WU* 00 17 43.0629024684 +51 25 59.115602831 5.04 6.01 6.14     O9.2II+O8V((f)) 317 0
2 BD+60 73 HXB 00 37 09.6358465128 +61 21 36.485521705 9.79 10.14 9.66     B1Ib 62 0
3 NAME SMC G 00 52 38.0 -72 48 01   2.79 2.2     ~ 9446 1
4 SK 160 HXB 01 17 05.1447530244 -73 26 36.015353425 12.23 13.00 13.15   13.17 O9.7Ia+ 798 0
5 V* V662 Cas HXB 01 18 02.6973905772 +65 17 29.829417242 12.27 11.99 11.14 10.33 9.58 B1Iae 231 0
6 NAME Magellanic Clouds GrG 03 00 -71.0           ~ 5669 1
7 V* X Per HXB 03 55 23.0778791365 +31 02 45.045745259 6.090 6.840 6.720     O9.5III 902 0
8 NAME LMC G 05 23 34.6 -69 45 22     0.4     ~ 14832 1
9 * del Ori Al* 05 32 00.40009 -00 17 56.7424 0.96 2.02 2.41 2.32 2.54 B0III+O9V 742 0
10 X LMC X-4 HXB 05 32 49.5558669817 -66 22 13.202534152   13.9 14.0     O8III 609 0
11 * iot Ori SB* 05 35 25.9819073 -05 54 35.643537 1.45 2.53 2.77     O9IIIvar 729 0
12 * sig Ori Y*O 05 38 44.7665260139 -02 36 00.284709290 2.54 3.58 3.79 3.87 4.11 O9.5V 738 0
13 X LMC X-1 HXB 05 39 38.8285930597 -69 44 35.533031148   14.8 14.5     O8(f)p 560 2
14 * zet Ori A ** 05 40 45.527 -01 56 33.26 0.50 1.77 1.88 1.84 2.04 O9.2IbvarNwk 643 0
15 HD 47129 SB* 06 37 24.0417003671 +06 08 07.376246443 5.23 6.11 6.06     O8I+O7.5III 368 0
16 V* GP Vel HXB 09 02 06.8610736194 -40 33 16.896402010 6.85 7.37 6.87 6.31 6.05 B0.5Ia 1373 0
17 V* V712 Car bL* 10 23 58.0120989646 -57 45 48.938103165 15.466 15.473 13.5 12.6   O3If*/WN6+O3If*/WN6 147 1
18 2MASS J10442207-5959351 * 10 44 21.9762241786 -59 59 35.070567231           ~ 3 1
19 HD 93206 bL* 10 44 22.9117286732 -59 59 35.978252992 5.53 6.37 6.24 7.42   O9.7Ibn 192 0
20 V* V560 Car SB* 10 44 33.7392630703 -59 44 15.434160993 6.89 7.80 7.75 7.56 7.46 O3.5V((f))+O8V 278 0
21 V* V779 Cen HXB 11 21 15.0920367078 -60 37 25.627505233   14.4       O9III/Veq 994 0
22 HD 306414 s*b 11 21 46.8237210288 -59 51 47.969821291 10.12 10.69 10.23 10.00   B1Ia 133 0
23 CPD-63 2495 HXB 13 02 47.6541729595 -63 50 08.625922862 10.34 10.72 9.98 10.03   O9.5Ve 674 1
24 * del Cir SB* 15 16 56.8969460249 -60 57 26.100998940 4.11 5.03 5.09 6.68   O8V 146 0
25 CXOU J162046.2-513006 HXB 16 20 46.2655398336 -51 30 06.046848280   18.9   16.28 13.4 B8IIIe 56 0
26 IGR J16318-4848 HXB 16 31 48.3102815892 -48 49 00.664215918           ~ 157 0
27 HD 149404 s*b 16 36 22.5628576926 -42 51 31.909559692 5.23 5.88 5.52 6.90   O8.5Iab(f)p 224 1
28 HD 150136 SB* 16 41 20.4156742370 -48 45 46.728092318 4.98 5.78 5.65 6.93   O3.5-4III(f*)+O6IV 171 0
29 2MASS J16415078-4532253 HXB 16 41 50.7854893198 -45 32 25.452141297           O8.5(sg?) 92 2
30 2MASS J16463526-4507045 HXB 16 46 35.2592332854 -45 07 04.609816032   15.2       O9.5Ia 87 1
31 2MASS J16480656-4512068 HXB 16 48 06.56 -45 12 06.8           O8.5Iab 119 2
32 HD 152219 Al* 16 53 55.6076307131 -41 52 51.497348038 6.950 7.705 7.569   7.267 O9.5III(n) 89 0
33 HD 152218 Al* 16 53 59.9903922189 -41 42 52.819620538 7.02 7.78 7.570   7.243 O9IV+B0:V: 131 0
34 HD 152248 bL* 16 54 10.0614779606 -41 49 30.143138696 5.56 6.15 6.088     O7Iabf+O7Ib(f) 228 0
35 CD-41 11042 Al* 16 54 19.8364088142 -41 50 09.384765116 7.733 9.02 8.80 9.23 7.859 O9.5IV 92 0
36 NAME OAO 1657-41 HXB 17 00 48.884 -41 39 21.46           Ofpe/WN9 211 0
37 HD 153919 HXB 17 03 56.7728262865 -37 50 38.912077679 6.06 6.78 6.51 6.08 5.90 O6Iafcp 756 1
38 2XMM J172511.3-361658 HXB 17 25 11.392 -36 16 57.53           B0-1Ia 109 2
39 HD 159176 SB* 17 34 42.4926595872 -32 34 53.964439199 4.88 5.74 5.70 7.19   O7V((f))+O7V((f)) 240 0
40 IGR J17354-3255 HX? 17 35 27.6078770673 -32 55 54.407937802           O9Iab 43 2
41 AX J1739.1-3020 HXB 17 39 11.5521531365 -30 20 37.783172824       13.91   O8.5Iab(f) 141 1
42 IGR J17544-2619 HXB 17 54 25.2724584579 -26 19 52.578788584   14.71 12.94 12.10 10.38 O9Ib 164 0
43 IGR J18029-2016 HXB 18 02 39.9 -20 17 13           B1b 71 1
44 * 9 Sgr Em* 18 03 52.4455370104 -24 21 38.639393923 5.08 5.97 5.97 5.72 5.70 O4V((f))z 517 0
45 V* V479 Sct HXB 18 26 15.0561532140 -14 50 54.249464136 12.02 12.23 11.27 11.04   ON6V((f))z 492 2
46 [KRL2007b] 335 HXB 18 45 01.5 -04 33 58   16.24 14.06 12.71 11.42 O9Ia 77 0
47 IGR J18483-0311 HXB 18 48 17.2064881183 -03 10 16.876608322 23.702 25.162 21.884 17.888 15.88 B0.5Ia 109 0
48 4U 1907+09 HXB 19 09 37.9 +09 49 49   19.41 16.35 14.40 12.53 O8.5Iab 307 1
49 INTEGRAL1 111 HXB 19 14 04.2269997048 +09 52 58.398334234   18.6 16.4     B0.5I 88 0
50 HD 226868 HXB 19 58 21.6758193269 +35 12 05.782512305 9.38 9.72 8.91 8.42   O9.7Iabpvar 3924 0
51 HD 193322 ** 20 18 06.98820 +40 43 55.5001 5.17 5.94 5.84 5.69 5.68 O9IV(n)+B1.5V 265 0
52 HD 206267 SB* 21 38 57.6182747705 +57 29 20.557311013 5.09 5.83 5.62   5.56 O6.0V((f))+O9:V 452 0
53 * 14 Cep SB* 22 02 04.5726568485 +58 00 01.308560227 4.77 5.551 5.542     O9IV(n)var+B1:V: 240 0
54 BD+53 2790 HXB 22 07 56.2368407539 +54 31 06.405811141 9.4 10.11 9.84 9.64 9.43 O9.5Vep 173 0
55 HD 215835 SB* 22 46 54.1108577770 +58 05 03.531709415 8.24 8.85 8.629   8.049 O5.5V((f))+O6V((f)) 237 0

    Equat.    Gal    SGal    Ecl

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2020.07.10-02:28:54

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