MG14 - Talk detail

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Abstract

Temperature of neutron stars can be estimated from thermal evolution (cooling and heating) models of isolated neutron stars as well as from accretion models of soft X-ray transients (SXT) in low mass X-ray binaries. The results obtained from these theoretical models will be compared with the latest observational data of various pulsars and SXTs. The comparison will offer some insight into the composition of the core of neutron stars, and help to answer questions such as whether it consists of neutron dominated matter only, or whether some more exotic particles such as hyperons, pion condenstates, or quarks are needed. As to magnetars, the observed surface temperature is higher than what cooling theory alone predicts and some heating mechanism is required. I will discuss possible heating mechanisms such as the internal heating from magnetic decay and the external heating from the stellar magnetosphere.

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