Radialization of Satellite Orbits in Galaxy Mergers

We consider the orbital evolution of satellites in galaxy mergers, focusing on the evolution of eccentricity. Using a large suite of N -body simulations, we study the phenomenon of satellite orbital radialization—a profound increase in the eccentricity of its orbit as it decays under dynamical frict...

Full description

Saved in:
Bibliographic Details
Published in:The Astrophysical journal 2022-02, Vol.926 (2), p.203
Main Authors: Vasiliev, Eugene, Belokurov, Vasily, Evans, N. Wyn
Format: Article
Language:English
Subjects:
Angular momentum
Astrophysics
Dynamical friction
Dynamical systems
Evolution
Friction
Galactic evolution
Galaxies
Galaxy mergers
Galaxy mergers & collisions
Many body problem
Orbit decay
Physical factors
Satellite orbits
Satellites
Simulation
Stars & galaxies
Citations: Items that this one cites
Items that cite this one
Online Access:Get full text
Tags: Add Tag
No Tags, Be the first to tag this record!
cited_by cdi_FETCH-LOGICAL-c416t-663bc3fb9fb23d9d4645c2170920419b05a332f10f131a9860d3c2e5a7b154353
cites cdi_FETCH-LOGICAL-c416t-663bc3fb9fb23d9d4645c2170920419b05a332f10f131a9860d3c2e5a7b154353
container_end_page
container_issue 2
container_start_page 203
container_title The Astrophysical journal
container_volume 926
creator Vasiliev, Eugene
Belokurov, Vasily
Evans, N. Wyn
description We consider the orbital evolution of satellites in galaxy mergers, focusing on the evolution of eccentricity. Using a large suite of N -body simulations, we study the phenomenon of satellite orbital radialization—a profound increase in the eccentricity of its orbit as it decays under dynamical friction. While radialization is detected in a variety of different setups, it is most efficient in cases of high satellite mass, not very steep host density profiles, and high initial eccentricity. To understand the origin of this phenomenon, we run additional simulations with various physical factors selectively turned off: satellite mass loss, reflex motion and distortion of the host, etc. We find that all these factors are important for radialization because it does not occur for point-mass satellites or when the host potential is replaced with an unperturbed initial profile. The analysis of forces and torques acting on both galaxies confirms the major role of self-gravity of both host and satellite in the reduction of orbital angular momentum. The classical Chandrasekhar dynamical friction formula, which accounts only for the forces between the host and the satellite, but not for internal distortions of both galaxies, does not match the evolution of eccentricity observed in N -body simulations.
doi_str_mv 10.3847/1538-4357/ac4fbc
format article
fullrecord <record><control><sourceid>proquest_iop_j</sourceid><recordid>TN_cdi_iop_journals_10_3847_1538_4357_ac4fbc</recordid><sourceformat>XML</sourceformat><sourcesystem>PC</sourcesystem><sourcerecordid>2635556469</sourcerecordid><originalsourceid>FETCH-LOGICAL-c416t-663bc3fb9fb23d9d4645c2170920419b05a332f10f131a9860d3c2e5a7b154353</originalsourceid><addsrcrecordid>eNp1kM1LxDAQxYMoWFfvHgterZtkkrQ5yqKrsLLgB3gLSZpIltquSRdc_3pbKnryNMzw3pvHD6Fzgq-gYuWccKgKBryca8u8sQco-z0dogxjzAoB5esxOklpM65UygzBo66DbsKX7kPX5p3Pn3Tvmib0Ll9HE_qUhzZf6kZ_7vMHF99cTKfoyOsmubOfOUMvtzfPi7titV7eL65XhWVE9IUQYCx4I72hUMuaCcYtJSWWFDMiDeYagHqCPQGiZSVwDZY6rktD-FAbZuhiyt3G7mPnUq823S62w0tFBXDOBRNyUOFJZWOXUnRebWN413GvCFYjGjVyUCMHNaEZLJeTJXTbv8x_5d-oAWOq</addsrcrecordid><sourcetype>Aggregation Database</sourcetype><iscdi>true</iscdi><recordtype>article</recordtype><pqid>2635556469</pqid></control><display><type>article</type><title>Radialization of Satellite Orbits in Galaxy Mergers</title><source>EZB Electronic Journals Library</source><creator>Vasiliev, Eugene ; Belokurov, Vasily ; Evans, N. Wyn</creator><creatorcontrib>Vasiliev, Eugene ; Belokurov, Vasily ; Evans, N. Wyn</creatorcontrib><description>We consider the orbital evolution of satellites in galaxy mergers, focusing on the evolution of eccentricity. Using a large suite of N -body simulations, we study the phenomenon of satellite orbital radialization—a profound increase in the eccentricity of its orbit as it decays under dynamical friction. While radialization is detected in a variety of different setups, it is most efficient in cases of high satellite mass, not very steep host density profiles, and high initial eccentricity. To understand the origin of this phenomenon, we run additional simulations with various physical factors selectively turned off: satellite mass loss, reflex motion and distortion of the host, etc. We find that all these factors are important for radialization because it does not occur for point-mass satellites or when the host potential is replaced with an unperturbed initial profile. The analysis of forces and torques acting on both galaxies confirms the major role of self-gravity of both host and satellite in the reduction of orbital angular momentum. The classical Chandrasekhar dynamical friction formula, which accounts only for the forces between the host and the satellite, but not for internal distortions of both galaxies, does not match the evolution of eccentricity observed in N -body simulations.</description><identifier>ISSN: 0004-637X</identifier><identifier>EISSN: 1538-4357</identifier><identifier>DOI: 10.3847/1538-4357/ac4fbc</identifier><language>eng</language><publisher>Philadelphia: The American Astronomical Society</publisher><subject>Angular momentum ; Astrophysics ; Dynamical friction ; Dynamical systems ; Evolution ; Friction ; Galactic evolution ; Galaxies ; Galaxy mergers ; Galaxy mergers &amp; collisions ; Many body problem ; Orbit decay ; Physical factors ; Satellite orbits ; Satellites ; Simulation ; Stars &amp; galaxies</subject><ispartof>The Astrophysical journal, 2022-02, Vol.926 (2), p.203</ispartof><rights>2022. The Author(s). Published by the American Astronomical Society.</rights><rights>2022. The Author(s). Published by the American Astronomical Society. This work is published under http://creativecommons.org/licenses/by/4.0/ (the “License”). Notwithstanding the ProQuest Terms and Conditions, you may use this content in accordance with the terms of the License.</rights><lds50>peer_reviewed</lds50><oa>free_for_read</oa><woscitedreferencessubscribed>false</woscitedreferencessubscribed><citedby>FETCH-LOGICAL-c416t-663bc3fb9fb23d9d4645c2170920419b05a332f10f131a9860d3c2e5a7b154353</citedby><cites>FETCH-LOGICAL-c416t-663bc3fb9fb23d9d4645c2170920419b05a332f10f131a9860d3c2e5a7b154353</cites><orcidid>0000-0002-5038-9267 ; 0000-0002-0038-9584</orcidid></display><links><openurl>$$Topenurl_article</openurl><openurlfulltext>$$Topenurlfull_article</openurlfulltext><thumbnail>$$Tsyndetics_thumb_exl</thumbnail><link.rule.ids>314,780,784,27924,27925</link.rule.ids></links><search><creatorcontrib>Vasiliev, Eugene</creatorcontrib><creatorcontrib>Belokurov, Vasily</creatorcontrib><creatorcontrib>Evans, N. Wyn</creatorcontrib><title>Radialization of Satellite Orbits in Galaxy Mergers</title><title>The Astrophysical journal</title><addtitle>APJ</addtitle><addtitle>Astrophys. J</addtitle><description>We consider the orbital evolution of satellites in galaxy mergers, focusing on the evolution of eccentricity. Using a large suite of N -body simulations, we study the phenomenon of satellite orbital radialization—a profound increase in the eccentricity of its orbit as it decays under dynamical friction. While radialization is detected in a variety of different setups, it is most efficient in cases of high satellite mass, not very steep host density profiles, and high initial eccentricity. To understand the origin of this phenomenon, we run additional simulations with various physical factors selectively turned off: satellite mass loss, reflex motion and distortion of the host, etc. We find that all these factors are important for radialization because it does not occur for point-mass satellites or when the host potential is replaced with an unperturbed initial profile. The analysis of forces and torques acting on both galaxies confirms the major role of self-gravity of both host and satellite in the reduction of orbital angular momentum. The classical Chandrasekhar dynamical friction formula, which accounts only for the forces between the host and the satellite, but not for internal distortions of both galaxies, does not match the evolution of eccentricity observed in N -body simulations.</description><subject>Angular momentum</subject><subject>Astrophysics</subject><subject>Dynamical friction</subject><subject>Dynamical systems</subject><subject>Evolution</subject><subject>Friction</subject><subject>Galactic evolution</subject><subject>Galaxies</subject><subject>Galaxy mergers</subject><subject>Galaxy mergers &amp; collisions</subject><subject>Many body problem</subject><subject>Orbit decay</subject><subject>Physical factors</subject><subject>Satellite orbits</subject><subject>Satellites</subject><subject>Simulation</subject><subject>Stars &amp; galaxies</subject><issn>0004-637X</issn><issn>1538-4357</issn><fulltext>true</fulltext><rsrctype>article</rsrctype><creationdate>2022</creationdate><recordtype>article</recordtype><recordid>eNp1kM1LxDAQxYMoWFfvHgterZtkkrQ5yqKrsLLgB3gLSZpIltquSRdc_3pbKnryNMzw3pvHD6Fzgq-gYuWccKgKBryca8u8sQco-z0dogxjzAoB5esxOklpM65UygzBo66DbsKX7kPX5p3Pn3Tvmib0Ll9HE_qUhzZf6kZ_7vMHF99cTKfoyOsmubOfOUMvtzfPi7titV7eL65XhWVE9IUQYCx4I72hUMuaCcYtJSWWFDMiDeYagHqCPQGiZSVwDZY6rktD-FAbZuhiyt3G7mPnUq823S62w0tFBXDOBRNyUOFJZWOXUnRebWN413GvCFYjGjVyUCMHNaEZLJeTJXTbv8x_5d-oAWOq</recordid><startdate>20220201</startdate><enddate>20220201</enddate><creator>Vasiliev, Eugene</creator><creator>Belokurov, Vasily</creator><creator>Evans, N. Wyn</creator><general>The American Astronomical Society</general><general>IOP Publishing</general><scope>O3W</scope><scope>TSCCA</scope><scope>AAYXX</scope><scope>CITATION</scope><scope>7TG</scope><scope>8FD</scope><scope>H8D</scope><scope>KL.</scope><scope>L7M</scope><orcidid>https://orcid.org/0000-0002-5038-9267</orcidid><orcidid>https://orcid.org/0000-0002-0038-9584</orcidid></search><sort><creationdate>20220201</creationdate><title>Radialization of Satellite Orbits in Galaxy Mergers</title><author>Vasiliev, Eugene ; Belokurov, Vasily ; Evans, N. Wyn</author></sort><facets><frbrtype>5</frbrtype><frbrgroupid>cdi_FETCH-LOGICAL-c416t-663bc3fb9fb23d9d4645c2170920419b05a332f10f131a9860d3c2e5a7b154353</frbrgroupid><rsrctype>articles</rsrctype><prefilter>articles</prefilter><language>eng</language><creationdate>2022</creationdate><topic>Angular momentum</topic><topic>Astrophysics</topic><topic>Dynamical friction</topic><topic>Dynamical systems</topic><topic>Evolution</topic><topic>Friction</topic><topic>Galactic evolution</topic><topic>Galaxies</topic><topic>Galaxy mergers</topic><topic>Galaxy mergers &amp; collisions</topic><topic>Many body problem</topic><topic>Orbit decay</topic><topic>Physical factors</topic><topic>Satellite orbits</topic><topic>Satellites</topic><topic>Simulation</topic><topic>Stars &amp; galaxies</topic><toplevel>peer_reviewed</toplevel><toplevel>online_resources</toplevel><creatorcontrib>Vasiliev, Eugene</creatorcontrib><creatorcontrib>Belokurov, Vasily</creatorcontrib><creatorcontrib>Evans, N. Wyn</creatorcontrib><collection>Open Access: IOP Publishing Free Content</collection><collection>IOPscience (Open Access)</collection><collection>CrossRef</collection><collection>Meteorological &amp; Geoastrophysical Abstracts</collection><collection>Technology Research Database</collection><collection>Aerospace Database</collection><collection>Meteorological &amp; Geoastrophysical Abstracts - Academic</collection><collection>Advanced Technologies Database with Aerospace</collection><jtitle>The Astrophysical journal</jtitle></facets><delivery><delcategory>Remote Search Resource</delcategory><fulltext>fulltext</fulltext></delivery><addata><au>Vasiliev, Eugene</au><au>Belokurov, Vasily</au><au>Evans, N. Wyn</au><format>journal</format><genre>article</genre><ristype>JOUR</ristype><atitle>Radialization of Satellite Orbits in Galaxy Mergers</atitle><jtitle>The Astrophysical journal</jtitle><stitle>APJ</stitle><addtitle>Astrophys. J</addtitle><date>2022-02-01</date><risdate>2022</risdate><volume>926</volume><issue>2</issue><spage>203</spage><pages>203-</pages><issn>0004-637X</issn><eissn>1538-4357</eissn><abstract>We consider the orbital evolution of satellites in galaxy mergers, focusing on the evolution of eccentricity. Using a large suite of N -body simulations, we study the phenomenon of satellite orbital radialization—a profound increase in the eccentricity of its orbit as it decays under dynamical friction. While radialization is detected in a variety of different setups, it is most efficient in cases of high satellite mass, not very steep host density profiles, and high initial eccentricity. To understand the origin of this phenomenon, we run additional simulations with various physical factors selectively turned off: satellite mass loss, reflex motion and distortion of the host, etc. We find that all these factors are important for radialization because it does not occur for point-mass satellites or when the host potential is replaced with an unperturbed initial profile. The analysis of forces and torques acting on both galaxies confirms the major role of self-gravity of both host and satellite in the reduction of orbital angular momentum. The classical Chandrasekhar dynamical friction formula, which accounts only for the forces between the host and the satellite, but not for internal distortions of both galaxies, does not match the evolution of eccentricity observed in N -body simulations.</abstract><cop>Philadelphia</cop><pub>The American Astronomical Society</pub><doi>10.3847/1538-4357/ac4fbc</doi><tpages>14</tpages><orcidid>https://orcid.org/0000-0002-5038-9267</orcidid><orcidid>https://orcid.org/0000-0002-0038-9584</orcidid><oa>free_for_read</oa></addata></record>
fulltext fulltext
identifier ISSN: 0004-637X
ispartof The Astrophysical journal, 2022-02, Vol.926 (2), p.203
issn 0004-637X
1538-4357
language eng
recordid cdi_iop_journals_10_3847_1538_4357_ac4fbc
source EZB Electronic Journals Library
subjects Angular momentum
Astrophysics
Dynamical friction
Dynamical systems
Evolution
Friction
Galactic evolution
Galaxies
Galaxy mergers
Galaxy mergers & collisions
Many body problem
Orbit decay
Physical factors
Satellite orbits
Satellites
Simulation
Stars & galaxies
title Radialization of Satellite Orbits in Galaxy Mergers
url http://sfxeu10.hosted.exlibrisgroup.com/loughborough?ctx_ver=Z39.88-2004&ctx_enc=info:ofi/enc:UTF-8&ctx_tim=2024-12-22T21%3A51%3A36IST&url_ver=Z39.88-2004&url_ctx_fmt=infofi/fmt:kev:mtx:ctx&rfr_id=info:sid/primo.exlibrisgroup.com:primo3-Article-proquest_iop_j&rft_val_fmt=info:ofi/fmt:kev:mtx:journal&rft.genre=article&rft.atitle=Radialization%20of%20Satellite%20Orbits%20in%20Galaxy%20Mergers&rft.jtitle=The%20Astrophysical%20journal&rft.au=Vasiliev,%20Eugene&rft.date=2022-02-01&rft.volume=926&rft.issue=2&rft.spage=203&rft.pages=203-&rft.issn=0004-637X&rft.eissn=1538-4357&rft_id=info:doi/10.3847/1538-4357/ac4fbc&rft_dat=%3Cproquest_iop_j%3E2635556469%3C/proquest_iop_j%3E%3Cgrp_id%3Ecdi_FETCH-LOGICAL-c416t-663bc3fb9fb23d9d4645c2170920419b05a332f10f131a9860d3c2e5a7b154353%3C/grp_id%3E%3Coa%3E%3C/oa%3E%3Curl%3E%3C/url%3E&rft_id=info:oai/&rft_pqid=2635556469&rft_id=info:pmid/&rfr_iscdi=true