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


C.D.S. - SIMBAD4 rel 1.7 - 2020.05.26CEST12:14:50

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

Status at CDS:  

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 - 2020
#notes
1 V* V635 Cas HXB 01 18 31.9704429246 +63 44 33.071137750 17.05 16.64 15.19 14.34 13.22 B0.2Ve 658 0
2 V* BQ Cam HXB 03 34 59.9116460415 +53 10 23.296351781   17.16 15.42 14.26 13.04 O8.5Ve 396 1
3 V* X Per HXB 03 55 23.0778791365 +31 02 45.045745259 6.090 6.840 6.720     O9.5III 900 0
4 RX J0531.2-6609 HXB 05 31 13.3008 -66 07 05.006     14.4     B0.7Ve 52 1
5 RX J0535.6-6651 HXB 05 35 40.9965654015 -66 51 53.522991468   13.7 13.8     B0.5IIIe 278 0
6 HD 245770 HXB 05 38 54.5749436467 +26 18 56.839215267 9.30 9.84 9.39 8.77 8.30 O9/B0III/Ve 867 0
7 V* V441 Pup HXB 07 28 53.5787769417 -26 06 28.895160996 11.27 12.29 11.83 11.53   O5Ve 68 0
8 V* V572 Pup HXB 08 12 28.3576629560 -31 14 52.138780764 12.14 13.03 12.74 12.44   B0.2IVe 60 0
9 Ginga 0834-430 HXB 08 35 55 -43 11.1     20.4     B0-2III-Ve 89 0
10 GRO J1008-571 HXB 10 09 46.9645132055 -58 17 35.603669270       14.63   B0e 170 0
11 WRAY 15-793 HXB 11 20 57.1736252056 -61 55 00.165172193 12.81 13.06 12.12     O9.5III/Ve 171 0
12 HD 102567 Be* 11 48 00.0214627917 -62 12 24.900348094 8.24 9.06 9.00 9.62   O/Bne 287 0
13 V* BP Cru HXB 12 26 37.5607088371 -62 46 13.259605389   12.70 10.66     B1.5Iaeq 601 0
14 V* V850 Cen HXB 13 01 17.0966951298 -61 36 06.636402972   15.6       B2Vne 271 0
15 4U 1416-62 HXB 14 21 12.8 -62 41 54   17.9 17.2     B1Ve 122 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? 52 1
18 4U 1850-03 HXB 18 48 17.7 -02 25 13           Be? 96 1
19 XTE J1946+274 HXB 19 45 39.3569004855 +27 21 55.502556930   18.76 16.92 15.62 14.38 B0-1IV-Ve 99 0
20 2MASS J19493548+3012317 HXB 19 49 35.4840244577 +30 12 31.775034731   15.16 14.22 13.53 12.88 B0Ve 131 1
21 GRO J2014+34 XB* 19 54 +30.1           ~ 31 1
22 V* V2246 Cyg HXB 20 32 15.2744631713 +37 38 14.839930326   22.16 19.41 17.32 15.18 B0Ve 374 0
23 GRO J2058+42 HXB 20 58 47.5371693693 +41 46 37.180557326   15.97 14.74 14.74 13.35 O9.5-B0IV-Ve 58 0
24 V* V490 Cep HXB 21 39 30.6903601561 +56 59 10.421972716   15.2       B1.5Ve 129 1
25 4U 2238+60 HXB 22 39 20.8444678371 +61 16 26.607919757   16.26 14.80 13.89 12.92 Be 42 0

    Equat.    Gal    SGal    Ecl

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2020.05.26-12:14:50

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