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General relativistic hydrodynamics w...

Donmez, Orhan.

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General relativistic hydrodynamics with Adaptive-Mesh Refinement (AMR) and modeling of accretion disks.

Record Type:	Electronic resources : Monograph/item
Title/Author:	General relativistic hydrodynamics with Adaptive-Mesh Refinement (AMR) and modeling of accretion disks./
Author:	Donmez, Orhan.
Description:	169 p.
Notes:	Source: Dissertation Abstracts International, Volume: 63-08, Section: B, page: 3755.
Contained By:	Dissertation Abstracts International63-08B.
Subject:	Physics, Astronomy and Astrophysics. -
Online resource:	http://pqdd.sinica.edu.tw/twdaoapp/servlet/advanced?query=3061127
ISBN:	0493767878

General relativistic hydrodynamics with Adaptive-Mesh Refinement (AMR) and modeling of accretion disks.
Donmez, Orhan.

General relativistic hydrodynamics with Adaptive-Mesh Refinement (AMR) and modeling of accretion disks. - 169 p.

Source: Dissertation Abstracts International, Volume: 63-08, Section: B, page: 3755.

Thesis (Ph.D.)--Drexel University, 2002.

We present a general procedure to solve the General Relativistic Hydrodynamical (GRH) equations with Adaptive-Mesh Refinement (AMR) and model of an accretion disk around a black hole. To do this, the GRH equations are written in a conservative form to exploit their hyperbolic character. The numerical solutions of the general relativistic hydrodynamic equations is done by High Resolution Shock Capturing schemes (HRSC), specifically designed to solve non-linear hyperbolic systems of conservation laws. These schemes depend on the characteristic information of the system. We use Marquina fluxes with MUSCL left and right states to solve GRH equations. First, we carry out different test problems with uniform and AMR grids on the special relativistic hydrodynamics equations to verify the second order convergence of the code in 1D, 2 D and 3D. Second, we solve the GRH equations and use the general relativistic test problems to compare the numerical solutions with analytic ones. In order to this, we couple the flux part of general relativistic hydrodynamic equation with a source part using Strang splitting. The coupling of the GRH equations is carried out in a treatment which gives second order accurate solutions in space and time. The test problems examined include shock tubes, geodesic flows, and circular motion of particle around the black hole. Finally, we apply this code to the accretion disk problems around the black hole using the Schwarzschild metric at the background of the computational domain. We find spiral shocks on the accretion disk. They are observationally expected results. We also examine the star-disk interaction near a massive black hole. We find that when stars are grounded down or a hole is punched on the accretion disk, they create shock waves which destroy the accretion disk.

ISBN: 0493767878Subjects--Topical Terms:

1019521
Physics, Astronomy and Astrophysics.

General relativistic hydrodynamics with Adaptive-Mesh Refinement (AMR) and modeling of accretion disks.
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100 1 $a Donmez, Orhan. $3 1952310
245 1 0 $a General relativistic hydrodynamics with Adaptive-Mesh Refinement (AMR) and modeling of accretion disks.
300 $a 169 p.
500 $a Source: Dissertation Abstracts International, Volume: 63-08, Section: B, page: 3755.
500 $a Adviser: Michael S. Vogeley.
502 $a Thesis (Ph.D.)--Drexel University, 2002.
520 $a We present a general procedure to solve the General Relativistic Hydrodynamical (GRH) equations with Adaptive-Mesh Refinement (AMR) and model of an accretion disk around a black hole. To do this, the GRH equations are written in a conservative form to exploit their hyperbolic character. The numerical solutions of the general relativistic hydrodynamic equations is done by High Resolution Shock Capturing schemes (HRSC), specifically designed to solve non-linear hyperbolic systems of conservation laws. These schemes depend on the characteristic information of the system. We use Marquina fluxes with MUSCL left and right states to solve GRH equations. First, we carry out different test problems with uniform and AMR grids on the special relativistic hydrodynamics equations to verify the second order convergence of the code in 1D, 2 D and 3D. Second, we solve the GRH equations and use the general relativistic test problems to compare the numerical solutions with analytic ones. In order to this, we couple the flux part of general relativistic hydrodynamic equation with a source part using Strang splitting. The coupling of the GRH equations is carried out in a treatment which gives second order accurate solutions in space and time. The test problems examined include shock tubes, geodesic flows, and circular motion of particle around the black hole. Finally, we apply this code to the accretion disk problems around the black hole using the Schwarzschild metric at the background of the computational domain. We find spiral shocks on the accretion disk. They are observationally expected results. We also examine the star-disk interaction near a massive black hole. We find that when stars are grounded down or a hole is punched on the accretion disk, they create shock waves which destroy the accretion disk.
590 $a School code: 0065.
650 4 $a Physics, Astronomy and Astrophysics. $3 1019521
650 4 $a Physics, Fluid and Plasma. $3 1018402
690 $a 0606
690 $a 0759
710 2 0 $a Drexel University. $3 1018434
773 0 $t Dissertation Abstracts International $g 63-08B.
790 1 0 $a Vogeley, Michael S., $e advisor
790 $a 0065
791 $a Ph.D.
792 $a 2002
856 4 0 $u http://pqdd.sinica.edu.tw/twdaoapp/servlet/advanced?query=3061127