The cooling of compact stars
By D. Page, U. Geppert, Fridolin Weber Inst. de Astronomia, Unam, Mexico City Mpe Garching, San Diego State University. 2005
324 citations recorded by the source corpus.
Abstract The cooling of a compact star depends very sensitively on the state of matter at supranuclear densities, which essentially controls the neutrino emission, as well as on the structure of the stellar outer layers which control the photon emission. Open issues concern the hyperon population, the presence of meson condensates, superfluidity and superconductivity, and the transition of confined hadronic matter to quark matter. This paper describes these issues and presents cooling calculations based on a broad collection of equations of state for neutron star matter and strange matter. These results are tested against the body of observed cooling data.
Subfields: Astronomy and Astrophysics, Atomic and Molecular Physics, and Optics
View Paper: https://www.semanticscholar.org/paper/7a71326284a43a9485e7bf87ac6d19b0165231fa
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In Astronomy and Astrophysics
In Atomic and Molecular Physics, and Optics
Citations in the corpus
- 2D Cooling of Magnetized Neutron Stars (2007, background): “…not only information on the physical properties such as the magnetic field, temperature, and chemical composition of the regions where this radiation is produced but also information on the properties of matter at higher densities deeper inside the star (Yakovlev & Pethick 2004; Page et al. 2006).”
- Cooling neutron star in the Cassiopeia A supernova remnant: evidence for superfluidity in the core (2010, methodology): “…all isolated NSs. Similar models of NSs withnucleon cores, where direct Urca is forbidden but CPF operates, w re used as the basis of the minimal cooling theory (Page et al. 2004, 2006, 2009) although that theory employs selectedTc(ρ) profiles, most favorable by the theory of nucleon superfluidity.”
- Analytical representations of unified equations of state of neutron-star matter (2004, background): “As well known, fractional abundances of leptons in the neutron-star core directly affect the thermal evolution of a neutron star at the neutrino cooling stage (e.g., Yakovlev & Pethick 2004; Page et al. 2006).”
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- NEUTRINO EMISSION FROM COOPER PAIRS AND MINIMAL COOLING OF NEUTRON STARS (2009, background): “…Electronic address: prakash@harsha.phy.ohiou.edu Electronic address: steinera@pa.msu.edu Historically, theoretical neutron star cooling models have fallen into two categories, “standard” cooling or enhanced cooling (see, e.g. Pethick 1992, Prakash 1994, 1998, Page et al. 2006, and Page 2009).”
- Magnetic field dissipation in neutron star crusts: From magnetars to isolated neutron stars (2007, unknown): “This approximation is valid during the neutrino cooling era if only modified URCA processes are operating (Page et al. 2006).”
- Combined Constraints on the Equation of State of Dense Neutron-rich Matter from Terrestrial Nuclear Experiments and Observations of Neutron Stars (2018, background): “…such as the mass, radius, moment of inertia, quadrupole deformation, pulsing frequency (Hessels et al. 2006), cooling curve (Yakovlev et al. 2001; Page et al. 2006), frequencies and damping times of various oscillating modes, spin parameter of pulsars, as well as the strain amplitude and phase…”