Relativistic Model of Detonation Transition From Neutron to Strange Matter

Tokareva, I.; Nusser, Adi; Gurovich, V. Tz.; Folomeev, Vladimir

doi:10.1142/s0218271805005803

Cited by 33 publications

(15 citation statements)

References 16 publications

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“…Finally, let us remark that to describe the flow of the new phase in a real star it would be necessary to solve the hydrodynamical equations describing the evolution of the system in which a combustion front propagates (Tokareva et al 2005). These are rather complicated partial differential equations which, moreover, should be studied together with the equations describing the dynamical readjustment of the star.…”

Section: Temperature Of the Quark Phasementioning

confidence: 99%

Burning of a Hadronic Star into a Quark or a Hybrid Star

Drago

Lavagno

Parenti

2007

ApJ

119

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We study the hydrodynamical transition from an hadronic star into a quark or a hybrid star. We discuss the possible mode of burning, using a fully relativistic formalism and realistic Equations of State in which hyperons can be present. We take into account the possibility that quarks form a diquark condensate. We also discuss the formation of a mixed phase of hadrons and quarks, and we indicate which region of the star can rapidly convert in various possible scenarios. An estimate of the final temperature of the system is provided. We find that the conversion process always corresponds to a deflagration and never to a detonation. Hydrodynamical instabilities can develop on the front. We estimate the increase in the conversion's velocity due to the formation of wrinkles and we find that, although the increase is significant, it is not sufficient to transform the deflagration into a detonation in essentially all realistic scenarios. Concerning convection, it does not always develop. In particular the system does not develop convection if hyperons are not present in the initial phase and if the newly formed quark phase is made of ungapped (or weakly gapped) quarks. At the contrary, the process of conversion from ungapped quark matter to gapped quarks always allows the formation of a convective layer. Finally, we discuss possible astrophysical implications of our results.

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Section: Temperature Of the Quark Phasementioning

confidence: 99%

Burning of a Hadronic Star into a Quark or a Hybrid Star

Drago

Lavagno

Parenti

2007

ApJ

119

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“…The energy released in such conversion can ignite hadronic matter in the neighborhood of the drop, and as a consequence, it may grow and convert to quark matter the core of the star and even the whole star if quark matter is absolutely stable. During the conversion, a combustion front (flame) separating the unburnt hadronic matter from the burnt quark matter travels outwards along the star [15][16][17][18][19][20][21][22][23][24][25].…”

Section: Introductionmentioning

confidence: 99%

Hydrodynamic Simulations of the Combustion of Dense Hadronic Matter into Quark Matter

Manrique

Lugones

2015

Braz J Phys

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We perform special-relativistic one-dimensional hydrodynamic simulations to study the combustion of hadronic matter into quark matter in neutron star conditions. For the equation of state, we use a relativistic mean-field Walecka model for hadronic matter and the MIT bag model for quark matter. We study the growth of a small core of quark matter surrounded by hadronic matter at constant density, where both regions are initially at rest. We show that a strong detonation front propagates into hadronic matter converting it into quark matter. We find that the timescale for the conversion of a compact star is around tens of microseconds.

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“…It could happen through a seed of external SQM [18], or be triggered by the rise in the central density due to a sudden spin-down in older neutron stars [19]. Several authors have studied the conversion of nuclear matter to strange matter under different assumptions [20][21][22][23][24][25][26][27][28][29][30]. They have been summarized in a recent work of mine [31] and for the constraint of space, I do not repeat them here.…”

Section: Introductionmentioning

confidence: 99%

Solving the relativistic Rankine-Hugoniot condition in the presence of a magnetic field in the astrophysical scenario of a neutron star

Mallick

2011

Phys. Rev. C

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The Rankine-Hugoniot condition has been solved to study phase transition in an astrophysical scenario mainly in the case of phase transition from a neutron star (NS) to a quark star (QS). The equations of state and temperature play a huge role in determining the nature of the front propagation, which brings about the phase transition in a NS. The shock jump conditions can be solved analytically, but the situation changes drastically by the inclusion of the magnetic field. High magnetic fields, which are always associated with a NS play a huge role in determining the structure and evolution of a NS. So, a magnetic field has been introduced in the shock jump condition in the de Hoffmann-Teller frame. The modified conservation condition for the perpendicular and oblique shocks is obtained in this frame. Numerical solution of the perpendicular shock has been obtained, which shows considerable deviation from the nonmagnetic case. The results show that the magnetic field helps in shock generation. It also indirectly hints at the instability of the matter and thereby the NS for very high magnetic field, implying that NSs can only support a magnetic field of some finite strength.

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Relativistic Model of Detonation Transition From Neutron to Strange Matter

Cited by 33 publications

References 16 publications

Burning of a Hadronic Star into a Quark or a Hybrid Star

Burning of a Hadronic Star into a Quark or a Hybrid Star

Hydrodynamic Simulations of the Combustion of Dense Hadronic Matter into Quark Matter

Solving the relativistic Rankine-Hugoniot condition in the presence of a magnetic field in the astrophysical scenario of a neutron star

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