Volume 424, Number 3, September IV 2004
|Page(s)||979 - 992|
|Section||Stellar structure and evolution|
|Published online||06 September 2004|
Cooling of neutron stars. Hadronic model
Fachbereich Physik, Universität Rostock, Universitätsplatz 1, 18051 Rostock, Germany e-mail: firstname.lastname@example.org
2 Bogoliubov Laboratory for Theoretical Physics, Joint Institute for Nuclear Research, 141980 Dubna, Russia
3 Fakultät für Physik, Universität Bielefeld, Universitätsstrasse, 33615 Bielefeld, Germany
4 Department of Physics, Yerevan State University, Alex Manoogian Str. 1, 375025 Yerevan, Armenia e-mail: email@example.com
5 Gesellschaft für Schwerionenforschung mbH, Planckstr. 1, 64291 Darmstadt, Germany
6 Moscow Institute for Physics and Engineering, 115409 Moscow, Russia e-mail: firstname.lastname@example.org
Accepted: 17 June 2004
We study the cooling of isolated neutron stars. The main cooling regulators are introduced: equation of state (EoS), thermal transport, heat capacity, neutrino and photon emissivity, superfluid nucleon gaps. The neutrino emissivity includes the main processes. A strong impact of medium effects on the cooling rates is demonstrated. Taking into account medium effects on reaction rates and on nucleon superfluid gaps modern experimental data can be well explained.
Key words: dense matter / equation of state / neutrinos / stars: evolution / stars: neutron / stars: pulsars: general
© ESO, 2004
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