Crust cooling curves of accretion-heated neutron stars
نویسنده
چکیده
We discuss the recent efforts to use a sub-class of neutron-star X-ray transients (the quasi-persistent transients) to probe the properties of neutron-star crusts and cores. Quasi-persistent X-ray transients experience accretion episodes lasting years to decades, instead of the usual weeks to months of ordinary, shortduration transients. These prolonged accretion episodes should significantly heat the crusts of the neutron stars in these systems, bringing the crusts out of thermal equilibrium with their neutron-star cores. When these systems are back in quiescence, i.e. when no more accretion onto the neutron-star surfaces occurs, then the crusts should thermally radiate in X-rays, cooling them down until they are again in thermal equilibrium with the cores. In this chapter we discuss the recent X-ray monitoring campaigns we performed (using the X-ray satellites Chandra and XMM-Newton) to study several quasi-persistent neutron-star X-ray transients in their quiescent states. These observations gave us, for the first time, a detailed look into the cooling curves of accretion heated neutron-star crusts. In this chapter, we discuss how these crust cooling curves can provide insight into the structure of neutron stars.
منابع مشابه
Monitoring Chandra Observations of the Quasi-persistent Neutron-star X-ray Transient Mxb 1659–29 in Quiescence: the Cooling Curve of the Heated Neutron-star Crust
We have observed the quasi-persistent neutron-star X-ray transient and eclipsing binary MXB 1659– 29 in quiescence on three occasions with Chandra. The purpose of our observations was to monitor the quiescent behavior of the source after its last prolonged (∼2.5 years) outburst which ended in September 2001. The X-ray spectra of the source are consistent with thermal radiation from the neutron-...
متن کاملCompositional Freeze-Out of Neutron Star Crusts
We have investigated the crustal properties of neutron stars without fallback accretion. We have calculated the chemical evolution of the neutron star crust in three different cases (a modified Urca process without the thermal influence of a crust, a thick crust, and a direct Urca process with a thin crust) in order to determine the detailed composition of the envelope and atmosphere as the nuc...
متن کاملConditions for Steady Gravitational Radiation from Accreting Neutron Stars
The gravitational-wave and accretion driven evolution of the angular velocity, core temperature, and (small) amplitude of an r-mode of neutron stars in low mass X-ray binaries and similar systems is investigated. The conditions required for evolution to a stable equilibrium state (with gravitational wave flux proportional to average X-ray flux) are determined. In keeping with conclusions derive...
متن کاملForecasting neutron star temperatures: predictability and variability.
It is now possible to model thermal relaxation of neutron stars after bouts of accretion during which the star is heated out of equilibrium by nuclear reactions in its crust. Major uncertainties in these models can be encapsulated in modest variations of a handful of control parameters that change the fiducial crustal thermal conductivity, specific heat, and heating rates. Observations of therm...
متن کاملThe Ocean and Crust of a Rapidly Accreting Neutron Star: Implications for Magnetic Field Evolution and Thermonuclear Flashes
We investigate the atmospheres, oceans, and crusts of neutron stars accreting at rates sufficiently high (typically in excess of the local Eddington limit) to stabilize the burning of accreted hydrogen and helium. For hydrogen-rich accretion at global rates in excess of 10M⊙ yr −1 (typical of a few neutron stars), we discuss the thermal state of the deep ocean and crust and their coupling to th...
متن کاملذخیره در منابع من
با ذخیره ی این منبع در منابع من، دسترسی به آن را برای استفاده های بعدی آسان تر کنید
عنوان ژورنال:
دوره شماره
صفحات -
تاریخ انتشار 2008