2001A&A...377..161O


Query : 2001A&A...377..161O

2001A&A...377..161O - Astronomy and Astrophysics, volume 377, 161-174 (2001/10-1)

A natural explanation for periodic X-ray outbursts in Be/X-ray binaries.

OKAZAKI A.T. and NEGUERUELA I.

Abstract (from CDS):

When applied to Be/X-ray binaries, the viscous decretion disc model, which can successfully account for most properties of Be stars, naturally predicts the truncation of the circumstellar disc. The distance at which the circumstellar disc is truncated depends mainly on the orbital parameters and the viscosity. In systems with low eccentricity, the disc is expected to be truncated at the 3:1 resonance radius, for which the gap between the disc outer radius and the critical lobe radius of the Be star is so wide that, under normal conditions, the neutron star cannot accrete enough gas at periastron passage to show periodic X-ray outbursts (type I outbursts). These systems will display only occasional giant X-ray outbursts (type II outbursts). On the other hand, in systems with high orbital eccentricity, the disc truncation occurs at a much higher resonance radius, which is very close to or slightly beyond the critical lobe radius at periastron unless the viscosity is very low. In these systems, disc truncation cannot be efficient, allowing the neutron star to capture gas from the disc at every periastron passage and display type I outbursts regularly. In contrast to the rather robust results for systems with low eccentricity and high eccentricity, the result for systems with moderate eccentricity depends on rather subtle details. Systems in which the disc is truncated in the vicinity of the critical lobe will regularly display type I outbursts, whereas those with the disc significantly smaller than the critical lobe will show only type II outbursts under normal conditions and temporary type I outbursts when the disc is strongly disturbed. In Be/X-ray binaries, material will be accreted via the first Lagrangian point with low velocities relative to the neutron star and carrying high angular momentum. This may result in the temporary formation of accretion discs during type I outbursts, something that seems to be confirmed by observations.

Abstract Copyright:

Journal keyword(s): stars: circumstellar matter - emission-line, Be - binaries: close - neutron - X-ray: stars, bursts

Simbad objects: 25

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Number of rows : 25
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 V* V635 Cas HXB 01 18 31.9704955824 +63 44 33.072603144 17.05 16.64 15.19 14.34 13.22 B0.2Ve 691 0
2 V* BQ Cam HXB 03 34 59.9116110096 +53 10 23.296879776   17.16 15.42 14.26 13.04 O8.5Ve 431 1
3 V* X Per HXB 03 55 23.0777456088 +31 02 45.039836148 6.090 6.840 6.720     O9.5III 940 0
4 RX J0531.2-6609 HXB 05 31 13.3008 -66 07 05.006     14.4     B0.7Ve 53 1
5 RX J0535.6-6651 HXB 05 35 40.9970566152 -66 51 53.547559416   13.7 13.8     B0.5IIIe 281 0
6 HD 245770 HXB 05 38 54.5748918624 +26 18 56.836952784 9.30 9.84 9.39 8.77 8.30 O9/B0III/Ve 927 0
7 V* V441 Pup HXB 07 28 53.5788273168 -26 06 28.897118208 11.27 12.29 11.83 11.53   O5Ve 74 0
8 V* V572 Pup HXB 08 12 28.3575205680 -31 14 52.138451400 12.14 13.03 12.74 12.44   B0.2IVe 63 0
9 Ginga 0834-430 HXB 08 35 54.9956514920 -43 11 17.497095048     20.4     B0-2III-Ve 95 0
10 GRO J1008-571 HXB 10 09 46.9642314696 -58 17 35.603851848       14.63   B0e 204 0
11 WRAY 15-793 HXB 11 20 57.1736884968 -61 55 00.166078020 12.81 13.06 12.12     O9.5III/Ve 184 0
12 HD 102567 Be* 11 48 00.0214464120 -62 12 24.902384760 8.24 9.06 9.00 9.62   O/Bne 300 0
13 V* BP Cru HXB 12 26 37.5605188992 -62 46 13.261044684   12.70 10.66     B1.5Iaeq 641 0
14 V* V850 Cen HXB 13 01 17.0968941216 -61 36 06.637549788   15.6 14.40     B2Vne 302 0
15 4U 1416-62 HXB 14 21 12.8 -62 41 54   17.9 17.2     B1Ve 133 0
16 [KRL2007b] 171 HXB 15 44 02 -56 42.7           Be? 51 0
17 GRO J1750-27 HXB 17 49 12.969 -26 38 38.93           Be? 59 1
18 4U 1850-03 HXB 18 48 17.7 -02 25 13           Be? 103 1
19 XTE J1946+274 HXB 19 45 39.3568693200 +27 21 55.501637040   18.76 16.92 15.62 14.38 B0-1IV-Ve 109 0
20 2MASS J19493548+3012317 HXB 19 49 35.4841147968 +30 12 31.775979852   15.16 14.22 13.53 12.88 B0Ve 149 1
21 GRO J2014+34 XB* 19 54 +30.1           ~ 32 1
22 V* V2246 Cyg HXB 20 32 15.2749858128 +37 38 14.843024844   22.16 19.41 17.32 15.18 B0Ve 401 0
23 GRO J2058+42 HXB 20 58 47.5371521256 +41 46 37.180486128   15.97 14.74 14.74 13.35 O9.5-B0IV-Ve 71 0
24 V* V490 Cep HXB 21 39 30.6903047304 +56 59 10.421969280   15.2       B1.5Ve 144 1
25 4U 2238+60 HXB 22 39 20.8443538152 +61 16 26.607472284   16.26 14.80 13.89 12.92 Be 47 0

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2022.08.10-06:39:33

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