Cooling Limits from the Youngest Neutron Stars

Patrick Slane

Harvard-Smithsonian Center for Astrophysics


One of the primary means of constraining the cooling properties of neutron stars, and thus the structure and composition of their deep interiors, is through measurements of their X-ray properties. The youngest neutron stars provided some of the strongest constraints, particularly in cases where the total luminosity is low. However, the X-ray emission from young neutron stars is often dominated by nonthermal emission. Thus, high-sensitivity observations and subsequent spectral modeling are necessary to confidently identify the emission, or limits to the emission, directly from the stellar surface. Here I summarize recent work on establishing the temperature properties of the youngest neutron stars.


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