Neutron star cooling

Yakovlev, D. G.; Gnedin, Oleg Y.; Gusakov, M. E.; Kaminker, A. D.; Levenfish, K. P.; Potekhin, A. Y.

doi:10.1016/j.nuclphysa.2005.02.061

Cited by 102 publications

(142 citation statements)

References 22 publications

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“…A very efficient cooling scenario emerges in the first ∼10 5 years. Standard processes such as those present in the URCA or the modified URCA (MURCA) cooling (Friman & Maxwell 1979;Yakovlev et al 2005) , respectively. Typical energetic scales can be obtained from the conversion factor 1 MeV∼10 10 K.  is a reduction function of the order of unity describing the superfluid effects in the neutron and proton branches of those reactions (Yakovlev & Levenfish 1995).…”

Section: Resultsmentioning

confidence: 99%

Enhanced Neutrino Emissivities in Pseudoscalar-mediated Dark Matter Annihilation in Neutron Stars

Cermeño

Pérez-García

Lineros

2018

ApJ

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We calculate neutrino emissivities from self-annihilating dark matter (DM) (χ) in the dense and hot stellar interior of a (proto)neutron star. Using a model where DM interacts with nucleons in the stellar core through a pseudoscalar boson (a) we find that the neutrino production rates from the dominant reaction channels cc nn ¯or aa cc  , with subsequent decay of the mediator a nn ¯, could locally match and even surpass those of the standard neutrinos from the modified nuclear URCA processes at early ages. We find that the emitting region can be localized in a tiny fraction of the star (less than a few percent of the core volume) and the process can last its entire lifetime for some cases under study. We discuss the possible consequences of our results for stellar cooling in light of existing DM constraints.

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Section: Resultsmentioning

confidence: 99%

Enhanced Neutrino Emissivities in Pseudoscalar-mediated Dark Matter Annihilation in Neutron Stars

Cermeño

Pérez-García

Lineros

2018

ApJ

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“…Later the star becomes transparent to neutrinos generated in its interior. It cools down gradually, initially through neutrino emission (t ≤ 10 5 years) and then through the emission of photons (t ≥ 10 5 years) [25], and transforms into an ordinary NS. The weak interaction responsible for the emission of these neutrinos eventually drive the stars to the state of β−equilibrium along with the imposed condition of charge neutrality.…”

Section: Formalismmentioning

confidence: 99%

Study of beta equilibrated2+1flavor quark matter in the Polyakov-Nambu-Jona-Lasinio model

et al. 2012

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We report a first case study of the phase diagram of 2+1 flavor strongly interacting matter in β−equilibrium, using the Polyakov−Nambu−Jona-Lasinio model. Physical characteristics of relevant thermodynamic observables have been discussed. A comparative analysis with the corresponding observables in the Nambu-Jona-Lasinio model is presented. We find distinct differences between the models in terms of a number of thermodynamic quantities like the speed of sound, specific heat, various number densities as well as entropy. The present study is expected to give us a better insight into the role that the superdense matter created in heavy ion collision experiments play in our understanding of the properties of matter inside the core of supermassive stars in the Universe.

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“…vacuum) OPE -henceforth denoted as FOPE -underestimates the cooling of neutron stars. Based on FOPE important medium modifications at ρ ρ 0 /2 are neglected (this has been discussed in details in Senatorov & Voskresensky, 1987;Blaschke et al, 1995;Schaab et al, 1997;Yakovlev et al, 2001;Hanhart et al, 2001;Blaschke et al, 2004;Yakovlev et al, 2005;Grigorian & Voskresensky, 2005;Page & Reddy, 2006;Blaschke et al, 2012Blaschke et al, , 2013, exploring also the role of medium effects for the charged-current absorption reactions, i.e. the modified Urca processes).…”

Section: Introductionmentioning

confidence: 99%

The role of medium modifications for neutrino-pair processes from nucleon-nucleon bremsstrahlung

Fischer

2016

A&A

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In this article the neutrino-pair production from nucleon-nucleon (N N ) bremsstrahlung is explored via mediummodifications of the strong interactions at the level of the one-pion exchange approximation. It governs the bulk part of the N N interaction at low densities relevant for the neutrino physics in core-collapse supernova studies. The resulting medium modified one-pion exchange rate for the neutrino-pair processes is implemented in simulations of core collapse supernovae in order to study the impact on the neutrino signal emitted from the deleptonization of the nascent proto-neutron star. Consequences for the nucleosynthesis of heavy elements of the material ejected from the PNS surface are discussed.

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Neutron star cooling

Cited by 102 publications

References 22 publications

Enhanced Neutrino Emissivities in Pseudoscalar-mediated Dark Matter Annihilation in Neutron Stars

Enhanced Neutrino Emissivities in Pseudoscalar-mediated Dark Matter Annihilation in Neutron Stars

Study of beta equilibrated2+1flavor quark matter in the Polyakov-Nambu-Jona-Lasinio model

The role of medium modifications for neutrino-pair processes from nucleon-nucleon bremsstrahlung

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