Thermal evolution of compact stars

Schaab, Ch.; Weber, Fridolin; Weigel, M. K.; Glendenning, Norman K.

doi:10.1016/0375-9474(96)00164-9

Cited by 115 publications

(131 citation statements)

References 98 publications

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“…In all these cases the critical temperatures are of the same order of magnitude as T cn and T cp in ordinary npe matter. Some authors discussed the superfluidity of quark matter (e.g., Bailin and Love 1984, Iwasaki 1995, Schaab et al 1996, Schaäfer and Wilczek 1999, Rajagopal 1999. In this case the situation is more intriguing since the theoretical models predict two possibilities.…”

Section: Structure Of Neutron Starsmentioning

confidence: 99%

“…The reduction factor R (ni) depends on the only argument v = δ(T )/T , the dimensionless gap parameter defined by Eq. (186). In the absence of superfluidity, we naturally have R (ni) = 1.…”

Section: (D) Bremsstrahlung In Neutron-nucleus Collisionsmentioning

confidence: 99%

“…3.8) and hence the cooling. These effects have been investigated in a number of papers, see, e.g., Schaab et al (1996Schaab et al ( , 1997a) and references therein.…”

Section: Other Aspects Of Neutron Star Coolingmentioning

confidence: 99%

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Neutrino emission from neutron stars

Kaminker²,

et al. 2001

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We review the main neutrino emission mechanisms in neutron star crusts and cores. Among them are the well-known reactions such as the electron-positron annihilation, plasmon decay, neutrino bremsstrahlung of electrons colliding with atomic nuclei in the crust, as well as the Urca processes and neutrino bremsstrahlung in nucleon-nucleon collisions in the core. We emphasize recent theoretical achievements, for instance, band structure effects in neutrino emission due to scattering of electrons in Coulomb crystals of atomic nuclei. We consider the standard composition of matter (neutrons, protons, electrons, muons, hyperons) in the core, and also the case of exotic constituents such as the pion or kaon condensates and quark matter. We discuss the reduction of the neutrino emissivities by nucleon superfluidity, as well as the specific neutrino emission produced by Cooper pairing of the superfluid particles. We also analyze the effects of strong magnetic fields on some reactions, such as the direct Urca process and the neutrino synchrotron emission of electrons. The results are presented in the form convenient for practical use. We illustrate the effects of various neutrino reactions on the cooling of neutron stars. In particular, the neutrino emission in the crust is critical in setting the initial thermal relaxation between the core and the crust. Finally, we discuss the prospects of exploring the properties of supernuclear matter by confronting cooling simulations with observations of the thermal radiation from isolated neutron stars.

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Section: Structure Of Neutron Starsmentioning

confidence: 99%

Section: (D) Bremsstrahlung In Neutron-nucleus Collisionsmentioning

confidence: 99%

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Neutrino emission from neutron stars

Kaminker²,

et al. 2001

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“…If a neutron star allows the DU process to take place, the star will exhibit a fast cooling (sometimes also referred to as enhanced cooling). If neutron superfluidity [10,11] (superconductivity in the case of protons) occurs, pairing will suppress the emission of neutrinos from hadronic processes and smooth the so-called enhanced cooling. The situation for hybrid stars is significantly different, since the presence of deconfined quark matter plays an important role for the cooling of the object.…”

Section: Introductionmentioning

confidence: 99%

Quark core impact on hybrid star cooling

2012

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In this paper we investigate the thermal evolution of hybrid stars, objects composed of a quark matter core, enveloped by ordinary hadronic matter. Our purpose is to investigate how important are the microscopic properties of the quark core to the thermal evolution of the star. In order to do that we use a simple MIT bag model for the quark core, and a relativistic mean field model for the hadronic envelope. By choosing different values for the microscopic parameters (bag constant, strange quark mass, strong coupling constant) we obtain hybrid stars with different quark core properties. We also consider the possibility of color superconductivity in the quark core. With this simple approach, we have found a set of microscopic parameters that lead to a good agreement with observed cooling neutron stars. Our results can be used to obtain clues regarding the properties of the quark core in hybrid stars, and can be used to refine more sophisticated models for the equation of state of quark matter.

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“…Although it is shown in Ref. [7] that the cooling evolution could be essentially affected by the inclusion of internal heating, nevertheless the latter is expected to be important for late time evolution and will not affect the results of this paper. It has been omitted in the present cooling scenario.…”

Section: Introductionmentioning

confidence: 84%

Brightness constraint for cooling models of young neutron stars

Grigorian

2006

Phys. Rev. C

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We study the systematics of neutron star cooling curves with three representative masses from the most populated interval of the estimated mass distribution for compact objects. The cooling simulations are made in the framework of the nuclear medium cooling (NMC) scenario using different combinations of possible nucleon-nucleon pairing gaps. Possible heating or enhanced cooling mechanisms in the crust are not considered. We define a constraint on the highest possible temperatures for a given age of young neutron stars and show that this limits the freedom of modeling pairing gaps and crust properties.Typeset using REVT E X 1 Studies of neutron star cooling evolution become very actual due to the presently known surface temperature and age data provided by X-ray observatories such as CHANDRA, XMM Newton and from the ROSAT catalogue [1]. These new data open a wide perspective for nuclear astrophysics for which up to now the knowledge of internal structure of the compact stars and the properties of stellar matter under extreme conditions remain central problems. Theoretical models and hypotheses about the equation of state of high density matter provide different alternatives for the explanation of the same set of observational temperature -age (TA) data points, when additional constraints are not provided. In this work we point out an existing correlation between the crust model and cooling behaviour of light neutron stars, which has a selective power in combination of TA data with the mass spectrum of neutron stars.In our recent investigations of the cooling evolution of neutron stars (NS) we have adopted the so called nuclear medium cooling (NMC) scenario [2], which goes beyond the minimal cooling scenario [3], where in-medium modifications of cooling regulators by definition have been disregarded. Both approaches agree in the philosophy that such very effective cooling mechanism like the direct Urca process should not occur in typical NS. In these approaches the main cooling process is the modified Urca process, which in our NMC scenario also includes the in-medium softening of the pion propagator [4]. Earlier investigations within this cooling scenario [5,6] have chosen the crust model as a simplified Tsuruta law T Tsur s = (10 T in ) 2/3 . Although it is shown in Ref. [7] that the cooling evolution could be essentially affected by the inclusion of internal heating, nevertheless the latter is expected to be important for late time evolution and will not affect the results of this paper. It has been omitted in the present cooling scenario. For more recent reviews on the cooling scenarios see [8][9][10].The cooling simulations presented in this work are based on a code with a number of improved inputs concerning the heat conductivity, the nucleon-nucleon pairing gaps and a new model of the neutron star crust and envelope. These models are basically taken from the recent calculations of Ref. [11], where the amount of light elements in the crust and the 2 influence of the magnetic field have been taken int...

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Thermal evolution of compact stars

Cited by 115 publications

References 98 publications

Neutrino emission from neutron stars

Neutrino emission from neutron stars

Quark core impact on hybrid star cooling

Brightness constraint for cooling models of young neutron stars

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