2016ApJ...824..143L


Query : 2016ApJ...824..143L

2016ApJ...824..143L - Astrophys. J., 824, 143-143 (2016/June-3)

Can the subsonic accretion model explain the spin period distribution of wind-fed X-ray pulsars?

LI T., SHAO Y. and LI X.-D.

Abstract (from CDS):

Neutron stars in high-mass X-ray binaries (HMXBs) generally accrete from the wind matter of their massive companion stars. Recently, Shakura et al. suggested a subsonic accretion model for low-luminosity (

Abstract Copyright: © 2016. The American Astronomical Society. All rights reserved.

Journal keyword(s): stars: early-type - stars: evolution - stars: neutron - X-rays: binaries

Simbad objects: 13

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Number of rows : 13
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 SK 160 HXB 01 17 05.1457288392 -73 26 36.014808156 12.23 13.00 13.15   13.17 O9.7Ia+ 918 0
2 SXP 1062 HXB 01 27 45.9424650912 -73 32 56.376382920   14.32 14.36     B0.5(III)e 95 1
3 V* X Per HXB 03 55 23.0777456088 +31 02 45.039836148 6.090 6.840 6.720     O9.5III 1037 0
4 X LMC X-4 HXB 05 32 49.5556042296 -66 22 13.202721768   13.9 14.0 14.290   O8III 714 0
5 V* GP Vel HXB 09 02 06.8608812864 -40 33 16.899168060 6.85 7.37 6.87 6.31 6.05 B0.5Ia 1588 0
6 V* BP Cru HXB 12 26 37.5605188992 -62 46 13.261044684   12.482 10.803 10.304   B1Ia+ 731 0
7 HD 153919 HXB 17 03 56.7725629224 -37 50 38.913331452 6.06 6.78 6.51 6.08 5.90 O6Iafcp 851 0
8 V* V2116 Oph Sy* 17 32 02.1532435416 -24 44 44.129169096   20.78 18.4     M6IIIe 719 1
9 IGR J17544-2619 HXB 17 54 25.2722906112 -26 19 52.576928292   14.71 12.94 12.10 10.38 O9Ib 207 0
10 4U 1907+09 HXB 19 09 38.0514267264 +09 49 47.270139132   19.41 16.35 15.570 12.53 O9.5Iab 362 0
11 4U 1908+075 HXB 19 10 48.2133201408 +07 35 51.707133960           O7.5/9.5If 139 0
12 DO 18341 HXB 19 55 42.3383143920 +32 05 49.046285472   12.02 9.97     M4/5III 145 0
13 BD+53 2790 HXB 22 07 56.2366802328 +54 31 06.408879888 9.4 10.11 9.84 9.64 9.43 O9.5Vep 233 0

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