2012A&A...537L...1H


Query : 2012A&A...537L...1H

2012A&A...537L...1H - Astronomy and Astrophysics, volume 537, L1-1 (2012/1-1)

SXP 1062, a young Be X-ray binary pulsar with long spin period. Implications for the neutron star birth spin.

HABERL F., STURM R., FILIPOVIC M.D., PIETSCH W. and CRAWFORD E.J.

Abstract (from CDS):

The Small Magellanic Cloud (SMC) is ideally suited to investigating the recent star formation history from X-ray source population studies. It harbours a large number of Be/X-ray binaries (Be stars with an accreting neutron star as companion), and the supernova remnants can be easily resolved with imaging X-ray instruments. We search for new supernova remnants in the SMC and in particular for composite remnants with a central X-ray source. We study the morphology of newly found candidate supernova remnants using radio, optical and X-ray images and investigate their X-ray spectra. Here we report on the discovery of the new supernova remnant around the recently discovered Be/X-ray binary pulsar CXOJ012745.97-733256.5 = SXP1062 in radio and X-ray images. The Be/X-ray binary system is found near the centre of the supernova remnant, which is located at the outer edge of the eastern wing of the SMC. The remnant is oxygen-rich, indicating that it developed from a type Ib event. From XMM-Newton observations we find that the neutron star with a spin period of 1062s (the second longest known in the SMC) shows a very high average spin-down rate of 0.26s per day over the observing period of 18-days. From the currently accepted models, our estimated age of around 10000-25000-years for the supernova remnant is not long enough to spin down the neutron star from a few 10ms to its current value. Assuming an upper limit of 25000-years for the age of the neutron star and the extreme case that the neutron star was spun down by the accretion torque that we have measured during the XMM-Newton observations since its birth, a lower limit of 0.5s for the birth spin period is inferred. For more realistic, smaller long-term average accretion torques our results suggest that the neutron star was born with a correspondingly longer spin period. This implies that neutron stars in Be/X-ray binaries with long spin periods can be much younger than currently anticipated.

Abstract Copyright:

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

Simbad objects: 13

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Number of rows : 13
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 AzV 102 HXB 00 51 53.1358981896 -72 31 48.721904580 13.66 14.79 14.38   14.40 B0-5(II) 69 0
2 NAME SMC G 00 52 38.0 -72 48 01   2.79 2.2     ~ 10381 1
3 SXP 144 HXB 00 53 53.0 -72 26 42           ~ 15 1
4 [MA93] 1367 HXB 01 03 13.9173060552 -72 09 14.258500452   14.70 14.79 15.0   B0.5IV-V 90 2
5 [MA93] 1393 HXB 01 03 37.5349856136 -72 01 33.204096336   14.54 14.65     B0III-V 65 0
6 2E 273 XB* 01 06 19.49 -72 05 27.8     16.70     ~ 58 0
7 AzV 503 HXB 01 21 40.6223488848 -72 57 30.906717444   14.23 14.3     B0-5(II)e 38 0
8 [HSB2012c] XMMU J0127.7-7332 SNR 01 27.7 -73 32           ~ 4 0
9 SXP 1062 HXB 01 27 45.9424650912 -73 32 56.376382920   14.32 14.36     B0.5(III)e 72 1
10 NGC 602 Cl* 01 29 32.133 -73 33 38.13     13.018     ~ 83 1
11 NAME Magellanic Clouds GrG 03 00 -71.0           ~ 6418 1
12 V* V779 Cen HXB 11 21 15.0920532528 -60 37 25.630264596   14.4 12.27     O9III/Veq 1035 0
13 V* V2116 Oph Sy* 17 32 02.1532435416 -24 44 44.129169096   20.78 18.4     M6IIIe 673 1

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2022.10.01-13:22:39

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