2011A&A...532A.126K


C.D.S. - SIMBAD4 rel 1.7 - 2020.07.04CEST14:46:06

2011A&A...532A.126K - Astronomy and Astrophysics, volume 532A, 126-126 (2011/8-1)

Pulse-amplitude-resolved spectroscopy of bright accreting pulsars: indication of two accretion regimes.

KLOCHKOV D., STAUBERT R., SANTANGELO A., ROTHSCHILD R.E. and FERRIGNO C.

Abstract (from CDS):

In addition to coherent pulsation, many accreting neutron stars exhibit flaring activity and strong aperiodic variability on time scales comparable to or shorter than their pulsation period. This behavior shows that the accretion flow in the vicinity of the accretor must be highly non-stationary. Observational study of this phenomenon is often problematic because it requires very high statistics of X-ray data and a specific analysis technique. In our research we used high-resolution data taken with RXTE and INTEGRAL on a sample of bright transient and persistent pulsars to perform an in-depth study of their variability on time scales comparable to the pulsation period - ''pulse-to-pulse variability''. The high-quality data allowed us to collect individual pulses of different amplitude and explore their X-ray spectrum as a function of pulse amplitude. The described approach allowed us for the first time to study the luminosity dependence of pulsars' X-ray spectra in observations where the averaged (over many pulse cycles) luminosity of the source remains constant. In all studied pulsars we reveal significant spectral changes as a function of the pulse height both in the continuum and in the cyclotron absorption features. The sources appear to form two groups that show different dependencies of the spectrum on pulse height. We interpret this division as a manifestation of two distinct accretion regimes that are at work in different pulsars.

Abstract Copyright:

Journal keyword(s): X-rays: binaries - stars: neutron - accretion, accretion disks

Simbad objects: 9

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Number of rows : 9

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 661 0
2 V* BQ Cam HXB 03 34 59.9116460415 +53 10 23.296351781   17.16 15.42 14.26 13.04 O8.5Ve 398 1
3 V* CM Tau Psr 05 34 31.93830 +22 00 52.1758           ~ 4803 1
4 M 1 SNR 05 34 31.94 +22 00 52.2           ~ 5594 4
5 HD 245770 HXB 05 38 54.5749436467 +26 18 56.839215267 9.30 9.84 9.39 8.77 8.30 O9/B0III/Ve 870 0
6 V* GP Vel HXB 09 02 06.8610736194 -40 33 16.896402010 6.85 7.37 6.87 6.31 6.05 B0.5Ia 1373 0
7 NAME Centaurus A Sy2 13 25 27.61509104 -43 01 08.8056025   8.18 6.84 6.66   ~ 3995 3
8 V* HZ Her LXB 16 57 49.8110797681 +35 20 32.487435684 11.90 14.89 13.63 13.88   B3/6ep 1920 0
9 HD 226868 HXB 19 58 21.6758193269 +35 12 05.782512305 9.38 9.72 8.91 8.42   O9.7Iabpvar 3923 0

    Equat.    Gal    SGal    Ecl

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2020.07.04-14:46:07

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