2017A&A...606A.145S


C.D.S. - SIMBAD4 rel 1.7 - 2020.07.10CEST02:09:37

2017A&A...606A.145S - Astronomy and Astrophysics, volume 606A, 145-145 (2017/10-1)

XMM-Newton spectroscopy of the accreting magnetar candidate 4U 0114+65.

SANJURJO-FERRRIN G., TORREJON J.M., POSTNOV K., OSKINOVA L., RODES-ROCA J.J. and BERNABEU G.

Abstract (from CDS):

Aims. 4U0114+65 is one of the slowest known X-ray pulsars. We present an analysis of a pointed observation by the XMM-Newton X-ray telescope in order to study the nature of the X-ray pulsations and the accretion process, and to diagnose the physical properties of the donor's stellar wind.
Methods. We analysed the energy-resolved light curve and the time-resolved X-ray spectra provided by the EPIC cameras on board XMM-Newton. We also analysed the first high-resolution spectrum of this source provided by the Reflection Grating Spectrometer.
Results. An X-ray pulse of 9350±160s was measured. Comparison with previous measurements confirms the secular spin up of this source. We successfully fit the pulse-phase-resolved spectra with Comptonisation models. These models imply a very small (r∼3km) and hot (kT∼2-3keV) emitting region and therefore point to a hot spot over the neutron star (NS) surface as the most reliable explanation for the X-ray pulse. The long NS spin period, the spin-up rate, and persistent X-ray emission can be explained within the theory of quasi-spherical settling accretion, which may indicate that the magnetic field is in the magnetar range. Thus, 4U 0114+65 could be a wind-accreting magnetar. We also observed two episodes of low luminosity. The first was only observed in the low-energy light curve and can be explained as an absorption by a large over-dense structure in the wind of the B1 supergiant donor. The second episode, which was deeper and affected all energies, may be due to temporal cessation of accretion onto one magnetic pole caused by non-spherical matter capture from the structured stellar wind. The light curve displays two types of dips that are clearly seen during the high-flux intervals. The short dips, with durations of tens of seconds, are produced through absorption by wind clumps. The long dips, in turn, seem to be associated with the rarefied interclump medium. From the analysis of the X-ray spectra, we found evidence of emission lines in the X-ray photoionised wind of the B1Ia donor. The Fe Kα line was found to be highly variable and much weaker than in other X-ray binaries with supergiant donors. The degree of wind clumping, measured through the covering fraction, was found to be much lower than in supergiant donor stars with earlier spectral types.
Conclusions. The XMM-Newton spectroscopy provided further support for the magnetar nature of the neutron star in 4U0114+65. The light curve presents dips that can be associated with clumps and the interclump medium in the stellar wind of the mass donor.

Abstract Copyright: © ESO, 2017

Journal keyword(s): X-rays: binaries - stars: winds, outflows - pulsars: individual: 4U 0114+65 - pulsars: individual: 4U 0114+65

Simbad objects: 22

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Number of rows : 22

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* V662 Cas HXB 01 18 02.6973905772 +65 17 29.829417242 12.27 11.99 11.14 10.33 9.58 B1Iae 231 0
2 PSR J0146+6145 Psr 01 46 22.21 +61 45 03.8   28.100 25.620     ~ 505 0
3 2XMM J050106.5+451634 X 05 01 08.0 +45 16 31           ~ 105 0
4 PSR B0525-66 Psr 05 26 00.7 -66 04 35           ~ 513 1
5 X LMC X-4 HXB 05 32 49.5558669817 -66 22 13.202534152   13.9 14.0     O8III 609 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 2E 2336 HXB 10 50 08.93 -59 53 19.9           Be 378 0
8 HD 306414 s*b 11 21 46.8237210288 -59 51 47.969821291 10.12 10.69 10.23 10.00   B1Ia 133 0
9 V* BP Cru HXB 12 26 37.5607088371 -62 46 13.259605389   12.70 10.66     B1.5Iaeq 604 0
10 V* QV Nor HXB 15 42 23.3633078550 -52 23 09.576918639   16.3 14.5     B0.2Ia:e 372 1
11 PSR J1550-5418 Psr 15 50 54.18 -54 18 23.9           ~ 331 1
12 PKS 1613-50 Rad 16 17 33.000 -51 02 00.00           ~ 453 3
13 PSR J1647-4552 Psr 16 47 10.18 -45 52 16.7           ~ 177 1
14 PSR J1708-4008 Psr 17 08 49.0 -40 09 10           ~ 261 0
15 PSR J1808-2024 Psr 18 08 39.32 -20 24 40.1           ~ 1098 2
16 2MASS J18211975-1318388 HXB 18 21 19.7677353711 -13 18 39.091923453           B0V-O9I 29 0
17 PSR J1841-0456 Psr 18 41 19.29 -04 56 11.4           ~ 234 1
18 GBS 1900+14 gB 19 07 13 +09 19.6           ~ 779 0
19 4U 1908+075 HXB 19 10 48.2141670291 +07 35 51.715745251           O7.5-9.5sg 103 0
20 NAME Sgr 1935+2154 * 19 34 55.68 +21 53 48.2           ~ 85 1
21 BD+53 2790 HXB 22 07 56.2368407539 +54 31 06.405811141 9.4 10.11 9.84 9.64 9.43 O9.5Vep 173 0
22 2E 4673 HXB 23 01 08.14 +58 52 44.5           ~ 585 1

    Equat.    Gal    SGal    Ecl

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2020.07.10-02:09:37

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