2D Cooling of Magnetized Neutron Stars
By D. Aguilera, José A. Pons, J. Miralles. 2007
147 citations recorded by the source corpus.
Context: Many thermally emitting isolated neutron stars have magnetic fields larger than 10^13 G. A realistic cooling model that includes the presence of high magnetic fields should be reconsidered. Aims: We investigate the effects of anisotropic temperature distribution and Joule heating on the cooling of magnetized neutron stars. Methods: The 2D heat transfer equation with anisotropic thermal conductivity tensor and including all relevant neutrino emission processes is solved for realistic models of the neutron star interior and crust. Results: The presence of the magnetic field affects significantly the thermal surface distribution and the cooling history during both, the early neutrino cooling era and the late photon cooling era. Conclusions: There is a large effect of the Joule heating on the thermal evolution of strongly magnetized neutron stars. Both magnetic fields and Joule heating play a key role in keeping magnetars warm for a long time. Moreover, this effect is important for intermediate field neutron stars and should be considered in radio-quiet isolated neutron stars or high magnetic field radio-pulsars.
Subfields: Astronomy and Astrophysics
View Paper: https://www.semanticscholar.org/paper/10f497308a7a55bc108780b60e0bc190128f92ec
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In Astronomy and Astrophysics
Citations in the corpus
- Neutron Stars—Cooling and Transport (2015, methodology): “The multidimensional heat transport and thermal evolution equations in a locally flat reference frame read (e.g., Aguilera et al. 2008; Pons et al. 2014; Viganò et al. 2013) cv e Φ ∂T ∂t + ∇ · (e2ΦF ) = e2Φ(H − Qν), F = −e−Φκ̂ · ∇ ( eΦT ) , (4) where F is the heat flux density, H is the heating…”
- Unifying the observational diversity of isolated neutron stars via magneto-thermal evolution models. (2013, methodology): “In Aguilera et al. (2008), a 2D cooling code followed the evolution of the temperature, for a given analytical prescription of a simplified, homologous decay of the magnetic field.”
- Magneto-thermal evolution of neutron stars (2008, methodology): “In some studies about cooling of NSs, the source term in the thermal diffusion equation includes an angular-averaged Joule heating rate, where the heat production is uniform in spherical shells at a given radius r (Page et al. 2000; Aguilera et al. 2008c; Urpin & Konenkov 2008).”