2001A&A...378..847B


C.D.S. - SIMBAD4 rel 1.7 - 2020.07.13CEST23:29:05

2001A&A...378..847B - Astronomy and Astrophysics, volume 378, 847-860 (2001/11-2)

Neutron star blackbody contraction during flaring in X 1624-490.

BALUCINSKA-CHURCH M., BARNARD R., CHURCH M.J. and SMALE A.P.

Abstract (from CDS):

We present results of an extensive investigation of the physical changes taking place in the emission regions of the LMXB X 1624-490 during strong flaring in observations made using RXTE in 1997 and 1999. Based on the detailed light curve, we propose that the flaring consists of a superposition of X-ray bursts. It is shown that major changes take place in the blackbody emission component, the temperature kTBB increasing to ∼2.2keV in flaring. Remarkably, the blackbody area decreases by a factor of ∼5 in flaring. During flare evolution, the blackbody luminosity remains approximately constant, constituting a previously unknown Eddington limiting effect which we propose is due to radiation pressure of the blackbody as kTBB increases affecting the inner disk or accretion flow resulting in a decreased emitting area on the star. We argue that the large decrease in area cannot be explained in terms of modification of the blackbody spectrum by electron scattering in the atmosphere of the neutron star. The height of the emitting region on the non-flaring neutron star is shown to agree with the height of the inner radiatively-supported accretion disk as found for sources in the ASCA survey of LMXB of Church & Balucinska-Church (2001A&A...369..915C). The decrease in height during flaring is discussed in terms of possible models, including radial accretion flow onto the stellar surface and the theory of accretion flow spreading on the neutron star surface of Inogamov & Sunyaev (1999AstL...25..269I). We demonstrate that the intensity of the broad iron line at 6.4keV is strongly correlated with the luminosity of the blackbody emission from the neutron star, and discuss the probable origin of this line in the ADC. Finally, possible reasons for non-detection of a reflection component in this source, and LMXB in general, are discussed.

Abstract Copyright:

Journal keyword(s): X rays: stars - stars: individual: X 1624-490 - stars: neutron - binaries: close - accretion: accretion disks

Simbad objects: 8

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Number of rows : 8

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* QX Nor LXB 16 12 43.0 -52 25 23           ~ 827 1
2 V* V818 Sco LXB 16 19 55.0688745859 -15 38 25.019920749 11.60 12.40 11.1     Oev 1525 0
3 NAME Big Dipper LXB 16 28 05.5318316228 -49 12 40.011030945           ~ 208 0
4 V* V801 Ara LXB 16 40 55.5979962948 -53 45 04.953475039 17.50 18.20 17.5   17.07 ~ 786 1
5 NAME Slow Burster LXB 17 31 57.73 -33 50 02.5           ~ 758 1
6 1ES 1735-26.9 LXB 17 38 17.12 -26 59 38.6           ~ 149 0
7 V* V4634 Sgr LXB 18 29 28.2 -23 47 49 18.90 19.40 19     ~ 287 0
8 HD 226868 HXB 19 58 21.6758193269 +35 12 05.782512305 9.38 9.72 8.91 8.42   O9.7Iabpvar 3925 0

    Equat.    Gal    SGal    Ecl

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2020.07.13-23:29:05

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