General relativistic study of the neutrino path and calculation of the minimum photosphere for different stars

Mallick, Ritam; Majumder, Sarbani

doi:10.1103/physrevd.79.023001

Cited by 9 publications

(10 citation statements)

References 18 publications

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“…The innermost point from which the neutrinos can contribute in the EDR is the MPR, which is 4km from the center. The same two points for the slowly rotating star are 12km and 4.7km respectively [14].…”

Section: Resultsmentioning

confidence: 99%

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General Relativistic Effect on the Energy Deposition Rate for Neutrino Pair Annihilation Above the Equatorial Plane Along the Symmetry Axis Near a Rotating Neutron Star

Mallick

Bhattacharyya

Ghosh

et al. 2013

Int. J. Mod. Phys. E

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The estimate of the energy deposition rate (EDR) for neutrino pair annihilation has been carried out. The EDR for the neutrinos coming from the equatorial plane of a rotating neutron star is calculated along the rotation axis using the Cook-Shapiro-Teukolsky (CST) metric. The neutrino trajectories and hence the neutrino emitted from the disk is affected by the redshift due to disk rotation and gravitation. The EDR is very sensitive to the value of the temperature and its variation along the disk. The rotation of the star has a negative effect on the EDR; it decreases with increase in rotational velocity.

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Section: Resultsmentioning

confidence: 99%

“…In an earlier paper [14], we have shown that the path of neutrino is important for the study of EDR near a massive object. We have done a complete GR calculation of the neutrino path for the most general metric describing a rotating star, and obtained its geodesic equation along the equatorial and polar plane.…”

Section: Introductionmentioning

confidence: 96%

General Relativistic Effect on the Energy Deposition Rate for Neutrino Pair Annihilation Above the Equatorial Plane Along the Symmetry Axis Near a Rotating Neutron Star

Mallick

Bhattacharyya

Ghosh

et al. 2013

Int. J. Mod. Phys. E

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“…This orbit may exist for ultracompact stars as well. For static stars with a stellar radius less than 3 M , there is always such a ‘photon sphere’, whereas, depending on the geometry of the space–time, the rotating stars can also have a photon radius at both lower and higher radii (Mallick & Majumder 2009). On the other hand, very massive rotating quark stars in the colour‐flavour‐locked (CFL) phase can reach masses higher than the equilibrium limit for static stars (≈3 M ⊙ ), of the same order as the stellar mass black holes (Kovács, Cheng & Harko 2009), and thus they can also have a photon radius.…”

Section: General Relativistic Effects On the Electron–positron Enermentioning

confidence: 99%

Electron-positron energy deposition rate from neutrino pair annihilation in the equatorial plane of rapidly rotating neutron and quark stars

Kovács

Cheng

Harkó

2010

Monthly Notices of the Royal Astronomical Society

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The neutrino–antineutrino annihilation into electron–positron pairs near the surface of compact general relativistic stars could play an important role in supernova explosions, neutron star collapse, or for close neutron star binaries near their last stable orbit. General relativistic effects increase the energy deposition rates due to the annihilation process. We investigate the deposition of energy and momentum due to the annihilations of neutrinos and antineutrinos in the equatorial plane of the rapidly rotating neutron and quark stars, respectively. We analyse the influence of general relativistic effects, and obtain the general relativistic corrections to the energy and momentum deposition rates for arbitrary stationary and axisymmetric space–times. We obtain the energy and momentum deposition rates for several classes of rapidly rotating neutron stars, described by different equations of state of the neutron matter, and for quark stars, described by the Massachusetts Institute of Technology bag model equation of state and in the colour‐flavour‐locked phase, respectively. Compared to the Newtonian calculations, rotation and general relativistic effects increase the total annihilation rate measured by an observer at infinity. The differences in the equations of state for neutron and quark matter also have important effects on the spatial distribution of the energy deposition rate by neutrino–antineutrino annihilation.

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“…The neutron star disc with the advection‐dominated inner disc could produce the highest neutrino luminosity, while the disc with an outflow has the lowest (Zhang & Dai 2009). A detailed general relativistic calculation of the neutrino path for a general metric describing a rotating star was studied in Mallick & Majumder (2009). The minimum photosphere radius was calculated for stars with two different equations of state (EOSs), each rotating with two different velocities.…”

Section: Introductionmentioning

confidence: 99%

Electron-positron energy deposition rate from neutrino pair annihilation on the rotation axis of neutron and quark stars

Kovács¹,

Cheng²,

Harkó³

2010

Monthly Notices of the Royal Astronomical Society

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We investigate the deposition of energy due to the annihilations of neutrinos and antineutrinos on the rotation axis of rotating neutron and quark stars, respectively. The source of the neutrinos is assumed to be a neutrino-cooled accretion disc around the compact object. Under the assumption of the separability of the neutrino null geodesic equation of motion, we obtain the general relativistic expression of the energy deposition rate for arbitrary stationary and axisymmetric space-times. The neutrino trajectories are obtained by using a ray tracing algorithm, based on numerically solving the Hamilton-Jacobi equation for neutrinos by reversing the proper time evolution. We obtain the energy deposition rates for several classes of rotating neutron stars, described by different equations of state of the neutron matter, and for quark stars, described by the MIT bag model equation of state and in the colour-flavourlocked phase, respectively. The electron-positron energy deposition rate on the rotation axis of rotating neutron and quark stars is studied for two accretion disc models (isothermal disc and accretion disc in thermodynamical equilibrium). Rotation and general relativistic effects modify the total annihilation rate of the neutrino-antineutrino pairs on the rotation axis of compact stellar general relativistic objects, as measured by an observer at infinity. The differences in the equations of state for neutron and quark matter also have important effects on the spatial distribution of the energy deposition rate by neutrino-antineutrino annihilation.

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General relativistic study of the neutrino path and calculation of the minimum photosphere for different stars

Cited by 9 publications

References 18 publications

General Relativistic Effect on the Energy Deposition Rate for Neutrino Pair Annihilation Above the Equatorial Plane Along the Symmetry Axis Near a Rotating Neutron Star

General Relativistic Effect on the Energy Deposition Rate for Neutrino Pair Annihilation Above the Equatorial Plane Along the Symmetry Axis Near a Rotating Neutron Star

Electron-positron energy deposition rate from neutrino pair annihilation in the equatorial plane of rapidly rotating neutron and quark stars

Electron-positron energy deposition rate from neutrino pair annihilation on the rotation axis of neutron and quark stars

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