Cooling of neutron stars. Hadronic model

Blaschke, D.; Grigorian, H.; Voskresensky, D. N.

doi:10.1051/0004-6361:20040404

Cited by 113 publications

(308 citation statements)

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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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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 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.…”

Section: Introductionmentioning

confidence: 99%

“…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.…”

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confidence: 99%

“…The boundary condition for the solution of (1) reads T (r = R in , t) = T in (t). The energy flux from the surface has also a contribution from photons L γ = 4πσR 2 T 4 s , which is governing the cooling, when the inner crust temperature T in falls down to 10 8 K.For different crust models we used in our recent calculations the T s −T in relations [2,21,22] shown in Fig. 1.…”

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confidence: 99%

“…For different crust models we used in our recent calculations the T s −T in relations [2,21,22] shown in Fig. 1.…”

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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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A web‐tool for population synthesis of near‐by cooling neutron stars: An on‐line test for cooling curves

Boldin

Попов²,

Tetzlaff³

2011

Astron Nachr

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We present a new web-tool -NET-PSICONS -for population synthesis of isolated near-by cooling neutron stars (NSs). The main aim is to provide an easy test of models of the NS thermal evolution which can be used by groups studying this subject. A user can upload cooling curves for a set of masses, modify the mass spectrum if necessary, change radii to fit the EoS used for cooling curve calculations, and then a population synthesis of close-by isolated cooling NSs is performed. The output includes the log N -log S distribution confronted with the ROSAT observations and several other sets of data. In this paper, we summarize the idea of the test proposed by Popov et al. (2006), and present a user's manual for the web-tool.

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Cooling of neutron stars. Hadronic model

Cited by 113 publications

References 54 publications

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

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

Brightness constraint for cooling models of young neutron stars

A web‐tool for population synthesis of near‐by cooling neutron stars: An on‐line test for cooling curves

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