$^{\boldmath 1}$S$_{\boldmath 0}$ neutron pairing vs. observations of cooling neutron stars
نویسندگان
چکیده
منابع مشابه
S 0 neutron pairing vs observations of cooling neutron stars
As shown recently by Kaminker et al. (2001), current observations of thermal emission of isolated middle–aged neutron stars (NSs) can be explained by cooling of NSs of different masses with the cores composed of neutrons, protons and electrons, assuming rather strong superfluidity (SF) of protons, weak triplet-state SF of neutrons and neglecting singlet-state SF of neutrons. We show that this e...
متن کامل1S0 neutron pairing vs. observations of cooling neutron stars
As shown recently by Kaminker et al. (2001), current observations of thermal emission of isolated middle-aged neutron stars (NSs) can be explained by cooling of NSs of different masses with the cores composed of neutrons, protons and electrons, assuming rather strong superfluidity (SF) of protons, weak triplet-state SF of neutrons and neglecting singlet-state SF of neutrons. We show that this e...
متن کاملObservations of Cooling Neutron Stars
Observations of cooling neutron stars allow to measure photospheric radii and to constrain the equation of state of nuclear matter at high densities. In this paper we concentrate on neutron stars, which show thermal (photospheric) Xray emission and have measured distances. After a short summary of the radio pulsars falling into this category we review the observational data of the 7 radio quiet...
متن کاملCooling of Neutron Stars: Two Types of Triplet Neutron Pairing
We consider cooling of neutron stars (NSs) with superfluid cores composed of neutrons, protons, and electrons (assuming singlet-state pairing of protons, and triplet-state pairing of neutrons). We mainly focus on (nonstandard) triplet-state pairing of neutrons with the |mJ | = 2 projection of the total angular momentum of Cooper pairs onto quantization axis. The specific feature of this pairing...
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Cooling simulations of neutron stars (NSs) are performed assuming that stellar cores consist of neutrons, protons and electrons and using realistic density profiles of superfluid critical temperatures Tcn(ρ) and Tcp(ρ) of neutrons and protons. Taking a suitable profile of Tcp(ρ) with maximum ∼5 × 10 9 K one can obtain smooth transition from slow to rapid cooling with increasing stellar mass. Ad...
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ژورنال
عنوان ژورنال: Astronomy & Astrophysics
سال: 2001
ISSN: 0004-6361,1432-0746
DOI: 10.1051/0004-6361:20011329