2013MNRAS.429.3411P


C.D.S. - SIMBAD4 rel 1.7 - 2021.04.15CEST08:13:09

2013MNRAS.429.3411P - Mon. Not. R. Astron. Soc., 429, 3411-3422 (2013/March-2)

The accretion flow to the intermittent accreting millisecond pulsar, HETE J1900.1-2455, as observed by XMM-Newton and RXTE.

PAPITTO A., D'AI A., SALVO T.D., EGRON E., BOZZO E., BURDERI L., IARIA R., RIGGIO A. and MENNA M.T.

Abstract (from CDS):

We present a study of the accretion flow to the intermittent accreting millisecond pulsar, HETE J1900.1-2455, based on observations made simultaneously by XMM-Newton and RXTE. The 0.33-50 keV energy spectrum is described by the sum of a hard Comptonized component produced in an optically thin τ ≃ 1 corona, a soft thermal kTin ≃ 0.2 keV component interpreted as accretion disc emission, and of disc reflection of the hard component. Two emission features are detected at energies of 0.98(1) and 6.58(7) keV, respectively. The latter is identified as Kα transition of Fe xxiii-xxv. A simultaneous detection in the European Photon Imaging Camera (EPIC-pn), EPIC-MOS2 and Reflection Grating Spectrometer (RGS) spectra favours an astrophysical origin also for the latter, which has an energy compatible with Fe-Lα and helium-like Ne-Kα transitions. The broadness of the two features, σ/E ≃ 0.1, suggests a common origin, resulting from reflection in an accretion disc with inclination of (30+ 4- 3)°, and extending down to Rin = 25+ 16- 11 gravitational radii from the compact object. However, the strength of the feature at lower energy measured by EPIC-pn cannot be entirely reconciled with the amplitude of the Fe-Kα line, hampering the possibility of describing it in terms of a broad-band reflection model, and preventing a firm identification. Pulsations at the known 377.3 Hz spin frequency could not be detected with an upper limit of 0.4percent at 3σ confidence level on the pulsed fractional amplitude.

We interpret the value of the inner disc radius estimated from spectral modelling and the lack of significant detection of coherent X-ray pulsations as an indication of a disc accretion flow truncated by some mechanism connected to the overall evolution of the accretion disc, rather than by the neutron star magnetic field. This is compatible with the extremely close similarity of spectral and temporal properties of this source with respect to other, non-pulsing atoll sources in the hard state.


Abstract Copyright: © 2013 The Authors Published by Oxford University Press on behalf of the Royal Astronomical Society (2013)

Journal keyword(s): line: identification - line: profiles - stars: neutron - pulsars: individual: HETE J1900.1-2455 - X-rays: binaries

Simbad objects: 10

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Number of rows : 10

N Identifier Otype ICRS (J2000)
RA
ICRS (J2000)
DEC
Mag U Mag B Mag V Mag R Mag I Sp type #ref
1850 - 2021
#notes
1 [GHJ2008] 3 HXB 16 50 00.980 -49 57 43.60     11.89     K4V 358 0
2 4U 1705-44 LXB 17 08 54.470 -44 06 07.35           ~ 362 0
3 4U 1722-30 LXB 17 27 33.25 -30 48 07.4     12.50     ~ 239 1
4 NAME Slow Burster LXB 17 31 57.73 -33 50 02.5     15.50     ~ 775 1
5 [PLV2002] CX1 LXB 17 48 52.163 -20 21 32.40           ~ 171 1
6 V* V4580 Sgr LXB 18 08 27.54 -36 58 44.3   16.81 16.51     ~ 895 0
7 V* V4634 Sgr LXB 18 29 28.2 -23 47 49 18.90 19.40 19     ~ 300 0
8 2MAXI J1900-248 LXB 19 00 08.65 -24 55 13.7     18.09     ~ 188 0
9 X Aql X-1 LXB 19 11 16.0572031521 +00 35 05.876658556           ~ 1040 1
10 GSC 03588-00834 HXB 21 03 35.7101268891 +45 45 05.568943629   15.34 14.20 13.49 12.75 B0Ve 153 0

    Equat.    Gal    SGal    Ecl

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2021.04.15-08:13:09

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