2009A&A...494.1059J


Query : 2009A&A...494.1059J

2009A&A...494.1059J - Astronomy and Astrophysics, volume 494, 1059-1071 (2009/2-2)

A model for the Z-track phenomenon in GX 5-1 and observational evidence for the physical origins of the kHz QPO.

JACKSON N.K., CHURCH M.J. and BALUCINSKA-CHURCH M.

Abstract (from CDS):

We present the results of a combined investigation of the spectral and kHz QPO evolution around the Z-track in GX 5-1 based on high-quality Rossi-XTE data. In spectral analysis, we find that the Extended ADC emission model provides very good fits to all of the spectra, and the results point clearly to a model for the nature of the Z-track in this source, in agreement with previous results for the similar source GX 340+0. In this model, at the soft apex of the Z-track, the mass accretion rate {dot}(M) is at its minimum and the neutron star has its lowest temperature; but as the source moves along the normal branch, the luminosity of the Comptonized emission increases, indicating that {dot}(M) increases and the neutron star gets hotter. The measured flux f of the neutron star emission increases by a factor of ten becoming super-Eddington, and we propose that this causes disruption of the inner disk and the formation of jets. In flaring, the luminosity of the dominant Comptonized emission from the accretion disk corona is constant, while the neutron star emission increases, and we propose for the first time that flaring consists of unstable nuclear burning on the neutron star, supported by the agreement between the measured mass accretion rate per unit area {dot}(m) at the onset of flaring and the theoretical critical value at which burning becomes unstable. There is a striking correlation between the frequencies of the kHz QPO and the ratio of the flux to the Eddington value: f/fEdd, suggesting an explanation of the higher frequency QPO and of its variation along the Z-track. It is well known that a Keplerian orbit in the disk at this frequency corresponds to a position some distance from the neutron star; we propose that the oscillation always occurs at the inner disk edge, which moves radially outwards on the upper normal and horizontal branches as the measured increasing radiation pressure increasingly disrupts the inner disk.

Abstract Copyright:

Journal keyword(s): accretion, accretion disks - stars: binaries: close - stars: neutron - X-rays: binaries - X-rays: individual: GX 5-1

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 - 2022
#notes
1 V* V818 Sco LXB 16 19 55.0692669024 -15 38 25.017666540 11.60 12.40 11.1     Oev 1577 0
2 4U 1642-45 LXB 16 45 47.7 -45 36 40     14.30     ~ 394 1
3 V* V1033 Sco HXB 16 54 00.137 -39 50 44.90   15.20 14.2 16.14   F5IV 1793 1
4 V* V1101 Sco LXB 17 05 44.4916006152 -36 25 23.049324480   20.10 18.6     ~ 420 0
5 4U 1758-25 LXB 18 01 09.7308060816 -25 04 44.120221284     11.08     ~ 631 1
6 V* V4580 Sgr LXB 18 08 27.54 -36 58 44.3   16.81 16.51     ~ 926 0
7 V* NP Ser LXB 18 16 01.389 -14 02 10.62   18.8       K 619 2
8 V* V1341 Cyg LXB 21 44 41.1544345272 +38 19 17.066570988 15.00 15.13 14.68 15.00   A9III 1108 1

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2022.08.18-03:14:26

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