The spin distribution of fast spinning neutron stars in low mass x-ray binaries: evidence for two sub-populations
The spin distribution of fast spinning neutron stars in low mass x-ray binaries: evidence for two sub-populations
We study the current sample of rapidly rotating neutron stars in both accreting and non-accreting binaries in order to determine whether the spin distribution of accreting neutron stars in low-mass X-ray binaries can be reconciled with current accretion torque models. We perform a statistical analysis of the spin distributions and show that there is evidence for two sub-populations among low-mass X-ray binaries, one at relatively low spin frequency, with an average of ~300 Hz and a broad spread, and a peaked population at higher frequency with average spin frequency of ~575 Hz. We show that the two sub-populations are separated by a cut-point at a frequency of ~540 Hz. We also show that the spin frequency of radio millisecond pulsars does not follow a log-normal distribution and shows no evidence for the existence of distinct sub-populations. We discuss the uncertainties of different accretion models and speculate that either the accreting neutron star cut-point marks the onset of gravitational waves as an efficient mechanism to remove angular momentum or some of the neutron stars in the fast sub-population do not evolve into radio millisecond pulsars.
1-12
Patruno, A.
7d408255-e680-4b6d-87ed-11f51ec9a35b
Haskell, B.
a3c09067-6932-45cc-902d-3b7117ec848d
Andersson, N.
2dd6d1ee-cefd-478a-b1ac-e6feedafe304
November 2017
Patruno, A.
7d408255-e680-4b6d-87ed-11f51ec9a35b
Haskell, B.
a3c09067-6932-45cc-902d-3b7117ec848d
Andersson, N.
2dd6d1ee-cefd-478a-b1ac-e6feedafe304
Patruno, A., Haskell, B. and Andersson, N.
(2017)
The spin distribution of fast spinning neutron stars in low mass x-ray binaries: evidence for two sub-populations.
The Astrophysical Journal, 850 (1), , [106].
(doi:10.3847/1538-4357/aa927a).
Abstract
We study the current sample of rapidly rotating neutron stars in both accreting and non-accreting binaries in order to determine whether the spin distribution of accreting neutron stars in low-mass X-ray binaries can be reconciled with current accretion torque models. We perform a statistical analysis of the spin distributions and show that there is evidence for two sub-populations among low-mass X-ray binaries, one at relatively low spin frequency, with an average of ~300 Hz and a broad spread, and a peaked population at higher frequency with average spin frequency of ~575 Hz. We show that the two sub-populations are separated by a cut-point at a frequency of ~540 Hz. We also show that the spin frequency of radio millisecond pulsars does not follow a log-normal distribution and shows no evidence for the existence of distinct sub-populations. We discuss the uncertainties of different accretion models and speculate that either the accreting neutron star cut-point marks the onset of gravitational waves as an efficient mechanism to remove angular momentum or some of the neutron stars in the fast sub-population do not evolve into radio millisecond pulsars.
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1705.07669
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Patruno_2017_ApJ_850_106
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Accepted/In Press date: 7 October 2017
e-pub ahead of print date: 21 November 2017
Published date: November 2017
Identifiers
Local EPrints ID: 414859
URI: http://eprints.soton.ac.uk/id/eprint/414859
ISSN: 0004-637X
PURE UUID: f9653e1a-1d63-4390-a73b-f7213331ff73
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Date deposited: 12 Oct 2017 16:31
Last modified: 16 Mar 2024 03:02
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Author:
A. Patruno
Author:
B. Haskell
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