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dc.contributor.author
Ferrari, Guilherme
dc.contributor.author
Dottori, Horacio Alberto
dc.contributor.author
Diaz, Ruben Joaquin
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dc.date.available
2015-07-21T00:57:51Z
dc.date.issued
2013-07
dc.identifier.citation
Ferrari, Guilherme; Dottori, Horacio Alberto; Diaz, Ruben Joaquin; Modeling the Black Hole Recoil from the Nucleus; Scientific Research Publishing; Journal of Modern Physics; 4; 7-2013; 55-63
dc.identifier.issn
2153-1196
dc.identifier.uri
http://hdl.handle.net/11336/1301
dc.description.abstract
GEMINI + GMOS and Chandra emission-line spectroscopy reveal that the Fanaroff-Riley II radio-source J133658.3- 295105 is a local object behind the barred-spiral galaxy M83 that is projected onto the galaxy?s disk at about 60" from the galaxy?s optical nucleus. J133658.3-295105 and its radiolobes are aligned with the optical nucleus of M83 and two other radio-sources neither of which are supernova remnants or HII regions. The optical nucleus of M83 is off-centered by 2.7" (~60 pc) with regard to the kinematic center. Its mass is within the range (1 - 4) × 106 Msun and the velocity dispersion at its center points to a non-resolved mass concentration of <~106 Msun. In this paper we study the circumstances in which the radio source would have been ejected from the central region of M83. We analyze different types of collisions of binary and triple systems of super-massive black holes (SMBHs) by numerical simulations using a Post-New- tonian approximation of order 7/2 (~1/c7). We developed an N-body code specially built to numerically integrate the Post-Newtonian equations of motion with a symplectic method. Numerical experiments show that the code is robust enough to handle virtually any mass ratio between particles and to follow the interaction up to a SMBH separation of three Schwarzschild radii. We show that within the current Post-Newtonian approximation, a scenario in which one of the three SMBHs suffers a slingshot-like kick is best suited to explain the ejection of J133658.3-295105, which simultaneously produces the recoil of the remaining BH pair, which drags together a subset of stars from the original cluster forming a structure that mimics the offcenter optical nucleus of M83. The simulation parameters are tuned to reproduce the velocities and positions of J133658.3-295105 as well as the optical nucleus and the putative SMBH at its center.
dc.format
application/pdf
dc.language.iso
eng
dc.publisher
Scientific Research Publishing
dc.rights
info:eu-repo/semantics/openAccess
dc.rights.uri
https://creativecommons.org/licenses/by-nc-sa/2.5/ar/
dc.subject
Galaxies: Nuclei
dc.subject
Galaxies: Dynamics
dc.subject
Black Holes Interaction
dc.subject
Black Holes: Kick-Off
dc.subject.classification
Astronomía
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dc.subject.classification
Ciencias Físicas
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dc.subject.classification
CIENCIAS NATURALES Y EXACTAS
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dc.title
Modeling the Black Hole Recoil from the Nucleus
dc.type
info:eu-repo/semantics/article
dc.type
info:ar-repo/semantics/artículo
dc.type
info:eu-repo/semantics/publishedVersion
dc.date.updated
2016-03-30 10:35:44.97925-03
dc.journal.volume
4
dc.journal.pagination
55-63
dc.journal.pais
Estados Unidos
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dc.journal.ciudad
Irvine, California
dc.description.fil
Fil: Ferrari, Guilherme. Instituto de Física. Universidade Federal do Rio Grande do Sul; Brazil;
dc.description.fil
Fil: Dottori, Horacio Alberto. Instituto de Física. Universidade Federal do Rio Grande do Sul; Brazil;
dc.description.fil
Fil: Diaz, Ruben Joaquin. Consejo Nacional de Investigaciones Científicas y Técnicas. Centro Cientifico Tecnológico - Conicet - San Juan. Instituto de Ciencias Astronómicas de la Tierra y del Espacio; Argentina;
dc.journal.title
Journal of Modern Physics
dc.relation.alternativeid
info:eu-repo/semantics/altIdentifier/doi/http://dx.doi.org/10.4236/jmp.2013.47A1007
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