A hydrodynamical analysis of the burning of a neutron star

Cho, H. T.; Ng, Kin-Wang; Speliotopoulos, Achilles D.

doi:10.1016/0370-2693(94)91201-7

Cited by 19 publications

(25 citation statements)

References 13 publications

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“…The results of the current work differ from paper [14] which assume that the energy per baryon in the strange matter (ε s /n s ) must be less than the energy per baryon (ε n /n n ) in neutron matter. However, the energies ε s and ε n contain thermal contributions in addition to the rest energies of the baryons and therefore the condition, ε n /n n > ε s /n s , does not necessarily hold in general.…”

Section: Discussioncontrasting

confidence: 52%

“…General conditions under which combustion in neutron stars may occur have been discussed in paper [14]. Based on the conservation laws of hydrodynamics the authors of that paper have investigated the necessary conditions for combustion for a wide ranges of values for bag constant B of the quark matter equation of state and the density of the neutron matter (NM).…”

Section: Introductionmentioning

confidence: 99%

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On the possibility of combustion of neutrons into strange quark matter

Tokareva¹,

Nusser

2006

Physics Letters B

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Section: Discussioncontrasting

confidence: 52%

Section: Introductionmentioning

confidence: 99%

On the possibility of combustion of neutrons into strange quark matter

Tokareva¹,

Nusser

2006

Physics Letters B

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“…Such a combustion has no terrestrial counterpart [27,29] and has been discarded in the previous papers exactly because it is endothermic [14,39]. We emphasize, however, that there is no reason in fact to throw it away.…”

Section: Introductionmentioning

confidence: 95%

“…This is in sharp contrast to the direct transition from HM to 3QM, in which small fractions of strangeness are energetically disfavored. Note that the chemical potentials of up and down quarks are close to the strange quark mass in the typical situations and the time scale of β-equilibration will be ∼ 10 −8 s [39], which is much shorter than the hydrodynamical time scale (∼ 10 −3 s) in neutron stars. This implies that the deconfinement and subsequent β-equilibration are lagged by ∼ 10 −8 s at most and the width of the conversion region is not larger than ∼ 10 2 cm, which is much greater than the typical length scale of strong interactions ∼fm, but still much smaller than the typical macroscopic scale such as a neutron star radius ∼ 10km.…”

Section: Introductionmentioning

confidence: 99%

Hydrodynamical study on the conversion of hadronic matter to quark matter: I. Shock-induced conversion

2016

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We study transitions of hadronic matter (HM) to 3-flavor quark matter (3QM) locally, regarding the conversion processes as combustion and describing them hydrodynamically. Not only the jump condition on both sides of the conversion front but the structures inside the front are also considered by taking into account what happens during the conversion processes on the time scale of weak interactions as well as equations of state (EOS's) in the mixed phase. Under the assumption that HM is metastable with their free energies being larger than those of 3QM but smaller than those of 2-flavor quark matter (2QM), we consider the transition via 2QM triggered by a rapid density rise in a shock wave. Based on the results, we discuss which combustion modes (strong/weak detonation) may be realized. HM is described by an EOS based on the relativistic mean field theory and 2, 3QM's are approximated by the MIT bag model. We demonstrate for a wide range of bag constant and strong coupling constant in this combination of EOS's that the combustion may occur in the so-called endothermic regime, in which the Hugoniot curve for combustion runs below the one for the shock wave in p − V plane, and which has no terrestrial counter part. Elucidating the essential features in this scenario first by a toy model, we then analyze more realistic models. We find that strong detonation always occurs. Depending on the EOS of quark matter (QM) as well as the density of HM and the Mach number of the detonation front, deconfinement from HM to 2QM is either completed or not completed in the shock wave. In the latter case, which is more likely if the EOS of QM ensures that deconfinement occurs above the nuclear saturation density and that the maximum mass of cold quark stars is larger than 2M ⊙ , the conversion continues further via the mixing state of HM and 3QM on the time scale of weak interactions. * Electronic address: furusawa@cfca.jp 2

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“…Once SQM is nucleated inside a neutron star, how does it grow to form a strange quark star? In this paper, we numerically investigate the issue of combustion of pure neutron matter to u,d,s matter using hydrodynamics, taking into account binding energy release and neutrino emission across the burning front-going beyond previous treatments of the problem [4][5][6][7][8][9]. This problem is interesting for three main reasons: (i) In Type Ia supernovae, multidimensional studies of small scale dynamics of flame burning including turbulence provide support for a pathway to the distributed regime, which can be a platform for detonation of the white dwarf [10][11][12].…”

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confidence: 99%

Numerical simulation of the hydrodynamical combustion to strange quark matter

2010

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We present results from a numerical solution to the burning of neutron matter inside a cold neutron star into stable u,d,s quark matter. Our method solves hydrodynamical flow equations in one dimension with neutrino emission from weak equilibrating reactions, and strange quark diffusion across the burning front. We also include entropy change from heat released in forming the stable quark phase. Our numerical results suggest burning front laminar speeds of 0.002-0.04 times the speed of light, much faster than previous estimates derived using only a reactive-diffusive description. Analytic solutions to hydrodynamical jump conditions with a temperature-dependent equation of state agree very well with our numerical findings for fluid velocities. The most important effect of neutrino cooling is that the conversion front stalls at lower density (below ≈2 times saturation density). In a two-dimensional setting, such rapid speeds and neutrino cooling may allow for a flame wrinkle instability to develop, possibly leading to detonation.

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A hydrodynamical analysis of the burning of a neutron star

Cited by 19 publications

References 13 publications

On the possibility of combustion of neutrons into strange quark matter

On the possibility of combustion of neutrons into strange quark matter

Hydrodynamical study on the conversion of hadronic matter to quark matter: I. Shock-induced conversion

Numerical simulation of the hydrodynamical combustion to strange quark matter

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