Crustal Heating and Quiescent Emission from Transiently Accreting Neutron Stars

Nuclear reactions occurring at densities ≈ 10 g cm in the crust of a transiently accreting neutron star efficiently maintain the core at a temperature ≈ (5–10)× 10K. When accretion halts, the envelope relaxes to a thermal equilibrium set by the flux from the hot core, as if the neutron star were newly born. For the time-averaged accretion rates (∼< 10 −10 M⊙ yr ) typical of low-mass X-ray transients, standard neutrino cooling is unimportant and the core thermally reradiates the deposited heat. The resulting luminosity is ∼ 5×10–5×10 ergs s and agrees with many observations of transient neutron stars in quiescence. Confirmation of this mechanism would strongly constrain rapid neutrino cooling mechanisms for neutron stars (e.g., a pion condensate). Thermal emission had previously been dismissed as a predominant source of quiescent emission since blackbody spectral fits implied an emitting area much smaller than a neutron star’s surface. However, as with thermal emission from radio pulsars, fits with realistic emergent spectra will imply a substantially larger emitting area. Other emission mechanisms, such as accretion or a pulsar shock, can also operate in quiescence and generate intensity and spectral variations over short timescales. Indeed, quiescent accretion may produce gravitationally redshifted metal photoionization edges in the quiescent spectra (detectable with AXAF and XMM ). We discuss past observations of Aql X-1 and note that the low luminosity (< 10 ergs s) X-ray sources in globular clusters and the Be star/X-ray transients are excellent candidates for future study. Subject headings: accretion, accretion disks — stars: neutron — stars: individual(Aquila X-1, SAX J1808.4–3658) To appear in The Astrophysical Journal, part II, 504 Current Address: Space Radiation Laboratory, California Institute of Technology, MS 220-47, Pasadena, CA 91125; [email protected] 2 Brown, Bildsten, & Rutledge