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ID: 9928.0, MPI für extraterrestrische Physik / High Energy Astrophysics at MPE
Crustal emission and the quiescent spectrum of the neutron star in KS 1731-260
Authors:Rutledge, Robert E.; Bildsten, Lars; Brown, Edward F.; Pavlov, George G.; Zavlin, Vyacheslav E.; Ushomirsky, Greg
Date of Publication (YYYY-MM-DD):2002-11-20
Title of Journal:The Astrophysical Journal
Journal Abbrev.:Astrophys. J.
Issue / Number:1
Start Page:413
End Page:422
Review Status:Peer-review
Audience:Experts Only
Abstract / Description:The type I X-ray-bursting low-mass X-ray binary KS 1731-260 was recently detected for the first time in quiescence by Wijnands et al. following a tau(ob) approximate to 13 yr outburst, which ended in 2001 February. We show that the emission area radius for a H atmosphere spectrum(possibly with a hard power-law component that dominates the emission above 3.5 keV) is consistent with that observed from other quiescent neutron star transients, R-infinity = 23(-15)(+30) (d/8 kpc) km and examine possible IR counterparts for KS 1731-260. Unlike all other known transient neutron stars, the duration of this recent (and the only observed) outburst is as long as the thermal diffusion time of the crust. The large amount of heat deposited by reactions in the crust will have heated the crust to temperatures much higher than the equilibrium core temperature. As a result, the thermal luminosity currently observed from the neutron star is dominated not by the core but by the crust. This scenario implies that the mean outburst recurrence timescale found by Wijnands et al. (similar to200 yr) is a lower limit. Moreover, because the thermal emission is dominated by the hot crust, the level and the time evolution of quiescent luminosity is determined mostly by the amount of heat deposited in the crust during the most recent outburst (for which reasonable constraints on the mass accretion rate exist) and is only weakly sensitive to the core temperature. Using estimates of the outburst mass accretion rate, our calculations of the quiescent flux immediately following the end of the outburst agree with the observed quiescent flux to within a factor of a few. In this paper, we present simulations of the evolution of the quiescent light curve for different scenarios of the crust microphysics and demonstrate that monitoring observations (with currently flying instruments) spanning from 1 to 30 yr can measure the crust cooling timescale and the total amount of heat stored in the crust. These quantities have not been directly measured for any neutron star. This makes KS 1731-260 a unique laboratory for studying the thermal properties of the crust by monitoring the luminosity over the next few years to decades.
Free Keywords:stars : atmospheres; stars : individual (KS 1731-260); stars : neutron; X-rays : binaries
External Publication Status:published
Document Type:Article
Communicated by:N. N.
Affiliations:MPI für extraterrestrische Physik
External Affiliations:CALTECH, MS 130-33, Pasadena, CA 91125 USA; CALTECH, Pasadena, CA 91125 USA; Univ Calif Santa Barbara, Inst Theoret Phys, Santa Barbara, CA 93106 USA; Univ Calif Santa Barbara, Dept Phys, Santa Barbara, CA 93106 USA; Univ Chicago, Enrico Fermi Inst, Chicago, IL 60637 USA; Penn State Univ, Davy Lab 525, University Pk, PA 16802 USA; Max Planck Inst Extraterr Phys, D-85740 Garching, Germany
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