2017A&A...599A..87C


Query : 2017A&A...599A..87C

2017A&A...599A..87C - Astronomy and Astrophysics, volume 599A, 87-87 (2017/3-1)

The rotation-powered nature of some soft gamma-ray repeaters and anomalous X-ray pulsars.

COELHO J.G., CACERES D.L., DE LIMA R.C.R., MALHEIRO M., RUEDA J.A. and RUFFINI R.

Abstract (from CDS):

Context. Soft gamma-ray repeaters (SGRs) and anomalous X-ray pulsars (AXPs) are slow rotating isolated pulsars whose energy reservoir is still matter of debate. Adopting neutron star (NS) fiducial parameters; mass M=1.4M, radius R=10km, and moment of inertia, I=1045g.cm2, the rotational energy loss, Erot, is lower than the observed luminosity (dominated by the X-rays) LX for many of the sources.
Aims. We investigate the possibility that some members of this family could be canonical rotation-powered pulsars using realistic NS structure parameters instead of fiducial values.
Methods. We compute the NS mass, radius, moment of inertia and angular momentum from numerical integration of the axisymmetric general relativistic equations of equilibrium. We then compute the entire range of allowed values of the rotational energy loss, Erot, for the observed values of rotation period P and spin-down rate P. We also estimate the surface magnetic field using a general relativistic model of a rotating magnetic dipole.
Results. We show that realistic NS parameters lowers the estimated value of the magnetic field and radiation efficiency, LX/Erot, with respect to estimates based on fiducial NS parameters. We show that nine SGRs/AXPs can be described as canonical pulsars driven by the NS rotational energy, for LX computed in the soft (2-10keV) X-ray band. We compute the range of NS masses for which LX/Erot<1. We discuss the observed hard X-ray emission in three sources of the group of nine potentially rotation-powered NSs. This additional hard X-ray component dominates over the soft one leading to LX/Erot>1 in two of them.
Conclusions. We show that 9 SGRs/AXPs can be rotation-powered NSs if we analyze their X-ray luminosity in the soft 2-10keV band. Interestingly, four of them show radio emission and six have been associated with supernova remnants (including Swift J1834.9-0846 the first SGR observed with a surrounding wind nebula). These observations give additional support to our results of a natural explanation of these sources in terms of ordinary pulsars. Including the hard X-ray emission observed in three sources of the group of potential rotation-powered NSs, this number of sources with LX/Erot<1 becomes seven. It remains open to verification 1) the accuracy of the estimated distances and 2) the possible contribution of the associated supernova remnants to the hard X-ray emission.

Abstract Copyright: © ESO, 2017

Journal keyword(s): pulsars: general - stars: rotation - stars: neutron - stars: magnetic field - stars: magnetic field

Simbad objects: 29

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Number of rows : 29
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 PSR J0100-7211 Psr 01 00 42.86 -72 11 33.3   17.69 17.82     B3V 92 0
2 PSR J0146+6145 Psr 01 46 22.21 +61 45 03.8   28.100 25.620     ~ 541 0
3 NAME Sgr J0418+5729 gam 04 18 33.867 +57 32 22.91           ~ 211 0
4 2XMM J050106.5+451634 X 05 01 08.0 +45 16 31           ~ 118 0
5 PSR B0525-66 Psr 05 26 00.7 -66 04 35           ~ 533 1
6 2E 2336 HXB 10 50 08.93 -59 53 19.9           Be 394 0
7 PSR J1119-6127 Psr 11 19 14.30 -61 27 49.5           ~ 371 1
8 PSR J1550-5418 Psr 15 50 54.18 -54 18 23.9           ~ 376 1
9 SNR G327.2-00.1 SNR 15 50 55 -54 18.0           ~ 63 1
10 PSR J1622-4950 Psr 16 22 44.80 -49 50 54.4           ~ 131 0
11 SNR G333.9+00.0 SR? 16 23 -49.7           ~ 10 0
12 SNR G337.0-00.1 SNR 16 35 06.9 -47 47 25           ~ 126 1
13 GRB 980618A gB 16 35 52 -47 35.2           ~ 253 0
14 PSR J1647-4552 Psr 16 47 10.18 -45 52 16.7           ~ 190 1
15 PSR J1708-4008 Psr 17 08 49.0 -40 09 10           ~ 279 0
16 SNR G348.7+00.3 SNR 17 13 43.0 -38 10 12           ~ 117 2
17 [AAB2008] 1 X 17 14 05.758 -38 10 31.32           ~ 56 1
18 PSR J1745-2900 Psr 17 45 40.1640 -29 00 29.818           ~ 286 0
19 PSR J1808-2024 Psr 18 08 39.32 -20 24 40.1           ~ 1183 2
20 AX J1809.8-1943 Psr 18 09 51.07 -19 43 51.8           ~ 429 0
21 1WGA J1822.2-1604 X 18 22 18.32 -16 04 27.2           ~ 123 0
22 SNR G023.3-00.3 SNR 18 34 51.80 -08 44 38.2           ~ 204 0
23 SWIFT J1834.9-0846 N*? 18 34 52.768 -08 45 40.83           ~ 77 0
24 PSR J1841-0456 Psr 18 41 19.29 -04 56 11.4           ~ 252 1
25 PSR J1846-0258 Psr 18 46 24.94 -02 58 30.1           ~ 328 2
26 SNR G029.7-00.2 SNR 18 46 25.5 -02 59 14           ~ 321 2
27 3XMM J185246.6+003317 Psr 18 52 46.60 +00 33 20.9           ~ 34 0
28 GBS 1900+14 gB 19 07 13 +09 19.6           ~ 827 0
29 2E 4673 HXB 23 01 08.14 +58 52 44.5           ~ 610 1

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2022.09.30-22:17:01

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