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Title: Nada: A new code for studying self-gravitating tori around black holes

Abstract

We present a new two-dimensional numerical code called Nada designed to solve the full Einstein equations coupled to the general relativistic hydrodynamics equations. The code is mainly intended for studies of self-gravitating accretion disks (or tori) around black holes, although it is also suitable for regular spacetimes. Concerning technical aspects the Einstein equations are formulated and solved in the code using a formulation of the standard 3+1 Arnowitt-Deser-Misner canonical formalism system, the so-called Baumgarte-Shapiro Shibata-Nakamura approach. A key feature of the code is that derivative terms in the spacetime evolution equations are computed using a fourth-order centered finite difference approximation in conjunction with the Cartoon method to impose the axisymmetry condition under Cartesian coordinates (the choice in Nada), and the puncture/moving puncture approach to carry out black hole evolutions. Correspondingly, the general relativistic hydrodynamics equations are written in flux-conservative form and solved with high-resolution, shock-capturing schemes. We perform and discuss a number of tests to assess the accuracy and expected convergence of the code, namely, (single) black hole evolutions, shock tubes, and evolutions of both spherical and rotating relativistic stars in equilibrium, the gravitational collapse of a spherical relativistic star leading to the formation of a black hole. In addition,more » paving the way for specific applications of the code, we also present results from fully general relativistic numerical simulations of a system formed by a black hole surrounded by a self-gravitating torus in equilibrium.« less

Authors:
;  [1];  [2]
  1. Departamento de Astronomia y Astrofisica, Universidad de Valencia, Dr. Moliner 50, 46100 Burjassot (Spain)
  2. Graduate School of Arts and Sciences, University of Tokyo, Komaba, Meguro, Tokyo 153-8902 (Japan)
Publication Date:
OSTI Identifier:
21254118
Resource Type:
Journal Article
Journal Name:
Physical Review. D, Particles Fields
Additional Journal Information:
Journal Volume: 78; Journal Issue: 6; Other Information: DOI: 10.1103/PhysRevD.78.064037; (c) 2008 The American Physical Society; Country of input: International Atomic Energy Agency (IAEA); Journal ID: ISSN 0556-2821
Country of Publication:
United States
Language:
English
Subject:
72 PHYSICS OF ELEMENTARY PARTICLES AND FIELDS; ACCRETION DISKS; APPROXIMATIONS; BLACK HOLES; CARTESIAN COORDINATES; COMPUTER CODES; CONVERGENCE; EINSTEIN FIELD EQUATIONS; EQUILIBRIUM; GRAVITATIONAL COLLAPSE; HYDRODYNAMICS; RELATIVISTIC RANGE; RESOLUTION; SHOCK TUBES; SIMULATION; SPACE-TIME; SPHERICAL CONFIGURATION; STARS; TWO-DIMENSIONAL CALCULATIONS

Citation Formats

Montero, Pedro J, Font, Jose A, and Shibata, Masaru. Nada: A new code for studying self-gravitating tori around black holes. United States: N. p., 2008. Web. doi:10.1103/PHYSREVD.78.064037.
Montero, Pedro J, Font, Jose A, & Shibata, Masaru. Nada: A new code for studying self-gravitating tori around black holes. United States. https://doi.org/10.1103/PHYSREVD.78.064037
Montero, Pedro J, Font, Jose A, and Shibata, Masaru. 2008. "Nada: A new code for studying self-gravitating tori around black holes". United States. https://doi.org/10.1103/PHYSREVD.78.064037.
@article{osti_21254118,
title = {Nada: A new code for studying self-gravitating tori around black holes},
author = {Montero, Pedro J and Font, Jose A and Shibata, Masaru},
abstractNote = {We present a new two-dimensional numerical code called Nada designed to solve the full Einstein equations coupled to the general relativistic hydrodynamics equations. The code is mainly intended for studies of self-gravitating accretion disks (or tori) around black holes, although it is also suitable for regular spacetimes. Concerning technical aspects the Einstein equations are formulated and solved in the code using a formulation of the standard 3+1 Arnowitt-Deser-Misner canonical formalism system, the so-called Baumgarte-Shapiro Shibata-Nakamura approach. A key feature of the code is that derivative terms in the spacetime evolution equations are computed using a fourth-order centered finite difference approximation in conjunction with the Cartoon method to impose the axisymmetry condition under Cartesian coordinates (the choice in Nada), and the puncture/moving puncture approach to carry out black hole evolutions. Correspondingly, the general relativistic hydrodynamics equations are written in flux-conservative form and solved with high-resolution, shock-capturing schemes. We perform and discuss a number of tests to assess the accuracy and expected convergence of the code, namely, (single) black hole evolutions, shock tubes, and evolutions of both spherical and rotating relativistic stars in equilibrium, the gravitational collapse of a spherical relativistic star leading to the formation of a black hole. In addition, paving the way for specific applications of the code, we also present results from fully general relativistic numerical simulations of a system formed by a black hole surrounded by a self-gravitating torus in equilibrium.},
doi = {10.1103/PHYSREVD.78.064037},
url = {https://www.osti.gov/biblio/21254118}, journal = {Physical Review. D, Particles Fields},
issn = {0556-2821},
number = 6,
volume = 78,
place = {United States},
year = {Mon Sep 15 00:00:00 EDT 2008},
month = {Mon Sep 15 00:00:00 EDT 2008}
}