Early neutron star evolution in high-mass X-ray binaries. (arXiv:2003.06436v1 [astro-ph.HE])
<a href="http://arxiv.org/find/astro-ph/1/au:+Ho_W/0/1/0/all/0/1">Wynn C. G. Ho</a> (Haverford), <a href="http://arxiv.org/find/astro-ph/1/au:+Wijngaarden_M/0/1/0/all/0/1">M. J. P. Wijngaarden</a> (Southampton), <a href="http://arxiv.org/find/astro-ph/1/au:+Andersson_N/0/1/0/all/0/1">Nils Andersson</a> (Southampton), <a href="http://arxiv.org/find/astro-ph/1/au:+Tauris_T/0/1/0/all/0/1">Thomas M. Tauris</a> (Aarhus), <a href="http://arxiv.org/find/astro-ph/1/au:+Haberl_F/0/1/0/all/0/1">F. Haberl</a> (MPE)
The application of standard accretion theory to observations of X-ray
binaries provides valuable insights into neutron star properties, such as their
spin period and magnetic field. However, most studies concentrate on relatively
old systems, where the neutron star is in its late propeller, accretor, or
nearly spin equilibrium phase. Here we use an analytic model from standard
accretion theory to illustrate the evolution of high-mass X-ray binaries early
in their life. We show that a young neutron star is unlikely to be an accretor
because of the long duration of ejector and propeller phases. We apply the
model to the recently discovered ~4000 yr old high-mass X-ray binary XMMU
J051342.6-672412 and find that the system’s neutron star, with a tentative spin
period of 4.4 s, cannot be in the accretor phase and has a magnetic field B >
(a few)x10^13 G, which is comparable to the magnetic field of many older
high-mass X-ray binaries and is much higher than the spin equilibrium inferred
value of (a few)x10^11 G. The observed X-ray luminosity could be the result of
thermal emission from a young cooling magnetic neutron star or a small amount
of accretion that can occur in the propeller phase.
The application of standard accretion theory to observations of X-ray
binaries provides valuable insights into neutron star properties, such as their
spin period and magnetic field. However, most studies concentrate on relatively
old systems, where the neutron star is in its late propeller, accretor, or
nearly spin equilibrium phase. Here we use an analytic model from standard
accretion theory to illustrate the evolution of high-mass X-ray binaries early
in their life. We show that a young neutron star is unlikely to be an accretor
because of the long duration of ejector and propeller phases. We apply the
model to the recently discovered ~4000 yr old high-mass X-ray binary XMMU
J051342.6-672412 and find that the system’s neutron star, with a tentative spin
period of 4.4 s, cannot be in the accretor phase and has a magnetic field B >
(a few)x10^13 G, which is comparable to the magnetic field of many older
high-mass X-ray binaries and is much higher than the spin equilibrium inferred
value of (a few)x10^11 G. The observed X-ray luminosity could be the result of
thermal emission from a young cooling magnetic neutron star or a small amount
of accretion that can occur in the propeller phase.
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