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Different accretion heating of the neutron star crust during multiple outbursts in MAXI J0556-332 | A. S. Parikh
; J. Homan
; R. Wijnands
; L. S. Ootes
; D. Page
; D. Altamirano. N. Degenaar
; E. F. Brown
; E. M. Cackett
; A. Cumming
; A. Deibel
; J. K. Fridriksson
; D. H. Lin
; M. Linares
; J. M. Miller
; | Date: |
25 Oct 2017 | Abstract: | The transient neutron star (NS) low-mass X-ray binary MAXI J0556$-$332
provides a rare opportunity to study NS crust heating and subsequent cooling
for multiple outbursts of the same source. We examine {it MAXI}, {it Swift},
{it Chandra}, and {it XMM-Newton} data of MAXI J0556$-$332 obtained during
and after three accretion outbursts of different durations and brightness. We
report on new data obtained after outburst III. The source has been tracked up
to $sim$1800 d after the end of outburst I. Outburst I heated the crust
strongly, but no significant reheating was observed during outburst II. Cooling
from $sim$324 eV to $sim$147 eV was observed during the first $sim$1200 d.
Outburst III reheated the crust up to $sim$169 eV, after which the crust
cooled again to $sim$132 eV in $sim$350 d. We model the thermal evolution of
the crust and find that this source required a different strength and depth of
shallow heating during each of the three outbursts. The shallow heating
released during outburst I was $sim$13.1 MeV nucleon$^{-1}$ and outburst III
required $sim$0.4 MeV nucleon$^{-1}$. These cooling observations could not be
explained without shallow heating. The shallow heating for outburst II was not
well constrained and could vary from $sim$0--3.4 MeV nucleon$^{-1}$, i.e.,
this outburst could in principle be explained without invoking shallow heating.
We discuss the nature of the shallow heating and why it may occur at different
strengths and depths during different outbursts. | Source: | arXiv, 1710.9365 | Services: | Forum | Review | PDF | Favorites |
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