Numerical Modeling of Gamma-Ray Burst Spectra

The model of gamma-ray burst (GRB) from magnetorotational supernova after its explosion is proposed in order to investigate burst gamma radiation spectrum. Formation and radiative acceleration of the collimated jet inside the channel in the Compton plasma cloud formed around the metallic core is con...

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Veröffentlicht in:	Lobachevskii journal of mathematics Jg. 46; H. 1; S. 121 - 132
Hauptverfasser:	Lartsev, A. I., Lukin, V. V.
Format:	Journal Article
Sprache:	Englisch
Veröffentlicht:	Moscow Pleiades Publishing 01.01.2025 Springer Nature B.V
Schlagworte:	Acceleration Algebra Analysis Approximation Black body radiation Elastic scattering Energy Flow velocity Fluid mechanics Gamma ray astronomy Gamma ray bursts Gamma rays Gas dynamics Geometry Graphics processing units Hydrodynamics Light speed Mathematical Logic and Foundations Mathematical models Mathematics Mathematics and Statistics Numerical models Photons Plasma Plasma clouds Probability Theory and Stochastic Processes Radiation Radiation pressure Radiative transfer Relativistic effects Relativistic velocity Spectra Three dimensional models mathematical modelling 2010 Mathematics Subject Classification: 65M08 gamma-ray burst relativistic jet radiation transfer Compton scattering computational astrophysics
ISSN:	1995-0802, 1818-9962
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Abstract	The model of gamma-ray burst (GRB) from magnetorotational supernova after its explosion is proposed in order to investigate burst gamma radiation spectrum. Formation and radiative acceleration of the collimated jet inside the channel in the Compton plasma cloud formed around the metallic core is considered. The observed spectrum is proposed to be the result of rising from the star and cloud photons scattering during the relativistic stream acceleration. These phenomena are described by a three-dimensional model of relativistic radiative hydrodynamics including the full radiative transfer equation with scattering integral. Due to relativistic speed of the flow one need to use a Compton scattering model that takes into account the change in photon frequency when colliding with fast-moving electrons. To obtain numerical solution of the radiation gas dynamics equations the splitting method is used. For the radiative transfer equation with scattering the short characteristics method is used, and for the relativistic hydrodynamics the Godunov-type one. The algorithm is designed for tetrahedral meshes and adapted for computations on cluster systems with graphics processing units. The central object radiation pressure accelerated the matter up to 90 of the light speed and the observed spectrum shifted from black-body radiation to the X-ray range. The spectra for observator different points of view are calculated.
AbstractList	The model of gamma-ray burst (GRB) from magnetorotational supernova after its explosion is proposed in order to investigate burst gamma radiation spectrum. Formation and radiative acceleration of the collimated jet inside the channel in the Compton plasma cloud formed around the metallic core is considered. The observed spectrum is proposed to be the result of rising from the star and cloud photons scattering during the relativistic stream acceleration. These phenomena are described by a three-dimensional model of relativistic radiative hydrodynamics including the full radiative transfer equation with scattering integral. Due to relativistic speed of the flow one need to use a Compton scattering model that takes into account the change in photon frequency when colliding with fast-moving electrons. To obtain numerical solution of the radiation gas dynamics equations the splitting method is used. For the radiative transfer equation with scattering the short characteristics method is used, and for the relativistic hydrodynamics the Godunov-type one. The algorithm is designed for tetrahedral meshes and adapted for computations on cluster systems with graphics processing units. The central object radiation pressure accelerated the matter up to 90 of the light speed and the observed spectrum shifted from black-body radiation to the X-ray range. The spectra for observator different points of view are calculated. The model of gamma-ray burst (GRB) from magnetorotational supernova after its explosion is proposed in order to investigate burst gamma radiation spectrum. Formation and radiative acceleration of the collimated jet inside the channel in the Compton plasma cloud formed around the metallic core is considered. The observed spectrum is proposed to be the result of rising from the star and cloud photons scattering during the relativistic stream acceleration. These phenomena are described by a three-dimensional model of relativistic radiative hydrodynamics including the full radiative transfer equation with scattering integral. Due to relativistic speed of the flow one need to use a Compton scattering model that takes into account the change in photon frequency when colliding with fast-moving electrons. To obtain numerical solution of the radiation gas dynamics equations the splitting method is used. For the radiative transfer equation with scattering the short characteristics method is used, and for the relativistic hydrodynamics the Godunov-type one. The algorithm is designed for tetrahedral meshes and adapted for computations on cluster systems with graphics processing units. The central object radiation pressure accelerated the matter up to 90 of the light speed and the observed spectrum shifted from black-body radiation to the X-ray range. The spectra for observator different points of view are calculated.
Author	Lukin, V. V. Lartsev, A. I.
Author_xml	– sequence: 1 givenname: A. I. surname: Lartsev fullname: Lartsev, A. I. email: lartsev.ai@yandex.ru organization: Keldysh Institute of Applied Mathematics of the Russian Academy of Sciences – sequence: 2 givenname: V. V. surname: Lukin fullname: Lukin, V. V. email: vvlukin@gmail.com organization: Keldysh Institute of Applied Mathematics of the Russian Academy of Sciences, Bauman Moscow State Technical University
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Cites_doi	10.1016/j.cpc.2022.108630 10.1093/mnras/stx309 10.1111/j.1365-2966.2006.10517.x 10.1051/0004-6361/202039612 10.1111/j.1365-2966.2007.11849.x 10.1007/s10509-009-0178-4 10.1007/s11214-016-0328-2 10.1088/0004-637X/752/2/116 10.1093/mnras/stu762 10.1111/j.1365-2966.2011.19451.x 10.1051/0004-6361/202245414 10.3847/1538-4365/ab18ff 10.20537/2076-7633-2014-6-2-203-215 10.3847/1538-4365/ab0d8c 10.1103/PhysRevD.78.024023 10.1103/PhysRevD.102.104001 10.1086/591925 10.1146/annurev.astro.43.072103.150558 10.1088/0004-637X/772/2/127 10.1007/978-3-662-03915-1 10.1007/978-981-15-4174-2 10.3847/2041-8213/ac1d56
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SubjectTerms	Acceleration Algebra Analysis Approximation Black body radiation Elastic scattering Energy Flow velocity Fluid mechanics Gamma ray astronomy Gamma ray bursts Gamma rays Gas dynamics Geometry Graphics processing units Hydrodynamics Light speed Mathematical Logic and Foundations Mathematical models Mathematics Mathematics and Statistics Numerical models Photons Plasma Plasma clouds Probability Theory and Stochastic Processes Radiation Radiation pressure Radiative transfer Relativistic effects Relativistic velocity Spectra Three dimensional models
Title	Numerical Modeling of Gamma-Ray Burst Spectra
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