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MAGNETARS AS COOLING NEUTRON STARS WITH INTERNAL HEATING

MAGNETARS AS COOLING NEUTRON STARS WITH INTERNAL HEATING. A.D. Kaminker , D.G. Yakovlev, A.Y. Potekhin, N. Shibazaki*, P. Sternin, and O.Y. Gnedin**. Ioffe Physical Technical Institute, St.-Petersburg, Russia *Rikkyo University, Tokyo 171-8501, Japan

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MAGNETARS AS COOLING NEUTRON STARS WITH INTERNAL HEATING

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  1. MAGNETARS AS COOLING NEUTRON STARS WITH INTERNAL HEATING A.D. Kaminker, D.G. Yakovlev, A.Y. Potekhin, N. Shibazaki*, P. Sternin, and O.Y. Gnedin** Ioffe Physical Technical Institute, St.-Petersburg, Russia *Rikkyo University, Tokyo 171-8501, Japan **Ohio State University, 760 1/2 Park Street, Columbus, OH 43215, USA Introduction Physics input Games with cooling code Conclusions

  2. Cooling theory with internal heating Thermal balance: Heat transport: - effectivethermal conductivity Photon luminosity: Heat blanketing envelope: Heat content: Main cooling regulators: 1. EOS 2. Neutrino emission 3. Reheating processes 4. Superfluidity 5. Magnetic fields 6. Light elements on the surface

  3. EOS: APR III (n, p, e, µ)Gusakov et al. (2005) • Akmal-Pandharipande-Ravenhall (1998) -- neutron star models Parametrization: Heiselberg & Hiorth-Jensen (1999) Heat blanketing envelope: 2. -- relation; -- effective temperature; surface temperature, -- surface element

  4. 1- SGR 1900+14 2- SGR 0526-66 3-AXP 1E 1841-045 4-AXP 1RXS J170849-400910 5- AXP 4U 0142+61 6- AXP 1E 2259+586

  5. Model of heating: 3. at i H ii iii H0 iv

  6. 1- SGR 1900+14 2- SGR 0526-66 3-AXP 1E 1841-045 No isothermal stage 4-AXP 1RXS J170849-400910 Core — crust decoupling 5- AXP 4U 0142+61 Only outer layers of heating are appropriate for hottest NSs 6- AXP 1E 2259+586

  7. Necessary energy input vrs. photon luminosity into the layer

  8. Enchanced thermal conductivity Direct Urcaprocess included from to Appearance of isothermal layers

  9. Conclusions 1. High thermal state ofmagnetarsdemand a powerfulreheating 2. The heating should be located in a thin layer at : in theouter crust. The heat intensity should range from to . Deeperheatingwould be extremely inefficient due to neutrino radiation Only ~ 1% of the total energy released in the heat layer can be spent to heat the NSsurface 3. 4. Pumping huge energy into deeper layers can not increase-- 5. Temperature distributions within NS arestrongly nonuniform due to thermal decoupling of the outer crust from the inner parts of the star

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