2016A&A...594A..45R


Query : 2016A&A...594A..45R

2016A&A...594A..45R - Astronomy and Astrophysics, volume 594A, 45-45 (2016/10-1)

Accretion regimes in the X-ray pulsar 4U 1901+03.

REIG P. and MILONAKI F.

Abstract (from CDS):

Context. The source 4U 1901+03 is a high-mass X-ray pulsar than went into outburst in 2003. Observation performed with the Rossi X-ray Timing Explorer showed spectral and timing variability, including the detection of flares, quasi-periodic oscillations, complex changes in the pulse profiles, and pulse phase dependent spectral variability.
Aims. We re-analysed the data covering the 2003 X-ray outburst and focused on several aspects of the variability that have not been discussed so far. These are the 10 keV feature and the X-ray spectral states and their association with accretion regimes, including the transit to the propeller state at the end of the outburst.
Methods. We extracted light curves and spectra using data from the Rossi X-ray Timing Explorer. Low time resolution light curves were used to create hardness-intensity diagrams and study daily changes in flux. High time resolution light curves were used to create pulse profiles. An average spectrum per observation allowed us to investigate the evolution of the spectral parameters with time.
Results. We find that 4U 1901+03 went through three accretion regimes over the course of the X-ray outburst. At the peak of the outburst and for a very short time, the X-ray flux may have overcome the critical limit that marks the formation of a radiative shock at a certain distance above the neutron star surface. Most of the time, however, the source is in the subcritical regime. Only at the end of the outburst, when the luminosity decreased below ∼1036(d/10kpc)2erg/s, did the source enter the propeller regime. Evidence for the existence of these regimes comes from the pulse profiles, the shape of the hardness-intensity diagram, and the correlation of various spectral parameters with the flux. The 10keV feature appears to strongly depend on the X-ray flux and on the pulse phase, which opens the possibility to interpret this feature as a cyclotron line.

Abstract Copyright: © ESO, 2016

Journal keyword(s): stars: emission-line, Be - X-rays: binaries - stars: neutron

CDS comments: Fig.2 stars not identified.

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 - 2024
#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 730 0
2 V* BQ Cam HXB 03 34 59.9116110096 +53 10 23.296879776   17.16 15.42 14.26 13.04 O8.5Ve 463 1
3 M 1 SNR 05 34 30.9 +22 00 53           ~ 6120 1
4 2E 1752 HXB 06 58 17.2878153600 -07 12 35.204283324   12.38 10.9 11.40   O9.7Ve 92 0
5 4U 1901+03 HXB 19 03 39.3926409480 +03 12 15.758070228           OB 104 0
6 XTE J1946+274 HXB 19 45 39.3568693200 +27 21 55.501637040   18.76 16.92 15.62 14.38 B0-1IV-Ve 121 0
7 2MASS J19493548+3012317 HXB 19 49 35.4841147968 +30 12 31.775979852   15.16 14.22 13.53 12.88 B0Ve 166 1
8 V* V2246 Cyg HXB 20 32 15.2749858128 +37 38 14.843024844   22.16 19.41 17.32 15.18 B0Ve 429 0

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2023.11.30-14:12:32

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