THE IMPRINT of RADIAL MIGRATION on the VERTICAL STRUCTURE of GALAXY DISKS

We use numerical simulations to examine the effects of radial migration on the vertical structure of galaxy disks. The simulations follow three exponential disks of different mass but similar circular velocity, radial scalelength, and (constant) scale height. The disks develop different non-axisymme...

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Fecha de publicación:
2016
Institución:
Universidad de Medellín
Repositorio:
Repositorio UDEM
Idioma:
eng
OAI Identifier:
oai:repository.udem.edu.co:11407/3155
Acceso en línea:
http://hdl.handle.net/11407/3155
Palabra clave:
galaxies: kinematics and dynamics
Galaxy: disk
Galaxy: evolution
stars: kinematics and dynamics
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restrictedAccess
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http://purl.org/coar/access_right/c_16ec
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spelling 2017-05-12T16:05:58Z2017-05-12T16:05:58Z20160004637Xhttp://hdl.handle.net/11407/315510.3847/1538-4357/833/1/42We use numerical simulations to examine the effects of radial migration on the vertical structure of galaxy disks. The simulations follow three exponential disks of different mass but similar circular velocity, radial scalelength, and (constant) scale height. The disks develop different non-axisymmetric patterns, ranging from feeble, long-lived multiple arms to strong, rapidly evolving few-armed spirals. These fluctuations induce radial migration through secular changes in the angular momentum of disk particles, mixing the disk radially and blurring pre-existing gradients. Migration primarily affects stars with small vertical excursions, regardless of spiral pattern. This "provenance bias" largely determines the vertical structure of migrating stars: inward migrators thin down as they move in, whereas outward migrators do not thicken up but rather preserve the disk scale height at their destination. Migrators of equal birth radius thus develop a strong scale-height gradient, not by flaring out as commonly assumed, but by thinning down as they spread inward. Similar gradients have been observed for low-[α/Fe] mono-abundance populations (MAPs) in the Galaxy, but our results argue against interpreting them as a consequence of radial migration. This is because outward migration does not lead to thickening, implying that the maximum scale height of any population should reflect its value at birth. In contrast, Galactic MAPs have scale heights that increase monotonically outward, reaching values that greatly exceed those at their presumed birth radii. Given the strong vertical bias affecting migration, a proper assessment of the importance of radial migration in the Galaxy should take carefully into account the strong radial dependence of the scale heights of the various stellar populations. © 2016. The American Astronomical Society. All rights reserved.engInstitute of Physics Publishinghttp://iopscience.iop.org/article/10.3847/1538-4357/833/1/42/meta;jsessionid=21FEC6A946A7E41099C7371A38264FD2.c1.iopscience.cld.iop.orgAstrophysical JournalScopusgalaxies: kinematics and dynamicsGalaxy: diskGalaxy: evolutionstars: kinematics and dynamicsTHE IMPRINT of RADIAL MIGRATION on the VERTICAL STRUCTURE of GALAXY DISKSArticleinfo:eu-repo/semantics/articlehttp://purl.org/coar/resource_type/c_6501http://purl.org/coar/resource_type/c_2df8fbb1info:eu-repo/semantics/restrictedAccesshttp://purl.org/coar/access_right/c_16ecVera-Ciro, C., Departamento de Ciencias Básicas, Universidad de Medellín, Cra 87 N 30-65, Medellín, Colombia, Department of Astronomy, University of Wisconsin, 475 N. Charter Street, Madison, WI, United StatesD'Onghia, E., Department of Astronomy, University of Wisconsin, 475 N. Charter Street, Madison, WI, United StatesNavarro, J.F., Department of Physics and Astronomy, University of Victoria, Victoria, BC, CanadaVera-Ciro C.D'Onghia E.Navarro J.F.THUMBNAIL27. THE IMPRINT OF RADIAL MIGRATION ON THE VERTICAL STRUCTURE OF GALAXY DISKS.pdf.jpg27. THE IMPRINT OF RADIAL MIGRATION ON THE VERTICAL STRUCTURE OF GALAXY DISKS.pdf.jpgIM Thumbnailimage/jpeg10606http://repository.udem.edu.co/bitstream/11407/3155/2/27.%20THE%20IMPRINT%20OF%20RADIAL%20MIGRATION%20ON%20THE%20VERTICAL%20STRUCTURE%20OF%20GALAXY%20DISKS.pdf.jpgc37f24bc331ddfd2bab99478655eb0a9MD52ORIGINAL27. THE IMPRINT OF RADIAL MIGRATION ON THE VERTICAL STRUCTURE OF GALAXY DISKS.pdf27. THE IMPRINT OF RADIAL MIGRATION ON THE VERTICAL STRUCTURE OF GALAXY DISKS.pdfapplication/pdf1688404http://repository.udem.edu.co/bitstream/11407/3155/1/27.%20THE%20IMPRINT%20OF%20RADIAL%20MIGRATION%20ON%20THE%20VERTICAL%20STRUCTURE%20OF%20GALAXY%20DISKS.pdfd2cd7f2cc64c2ea61f914d9ec37ac864MD5111407/3155oai:repository.udem.edu.co:11407/31552020-05-27 18:33:11.796Repositorio Institucional Universidad de Medellinrepositorio@udem.edu.co
dc.title.spa.fl_str_mv THE IMPRINT of RADIAL MIGRATION on the VERTICAL STRUCTURE of GALAXY DISKS
title THE IMPRINT of RADIAL MIGRATION on the VERTICAL STRUCTURE of GALAXY DISKS
spellingShingle THE IMPRINT of RADIAL MIGRATION on the VERTICAL STRUCTURE of GALAXY DISKS
galaxies: kinematics and dynamics
Galaxy: disk
Galaxy: evolution
stars: kinematics and dynamics
title_short THE IMPRINT of RADIAL MIGRATION on the VERTICAL STRUCTURE of GALAXY DISKS
title_full THE IMPRINT of RADIAL MIGRATION on the VERTICAL STRUCTURE of GALAXY DISKS
title_fullStr THE IMPRINT of RADIAL MIGRATION on the VERTICAL STRUCTURE of GALAXY DISKS
title_full_unstemmed THE IMPRINT of RADIAL MIGRATION on the VERTICAL STRUCTURE of GALAXY DISKS
title_sort THE IMPRINT of RADIAL MIGRATION on the VERTICAL STRUCTURE of GALAXY DISKS
dc.contributor.affiliation.spa.fl_str_mv Vera-Ciro, C., Departamento de Ciencias Básicas, Universidad de Medellín, Cra 87 N 30-65, Medellín, Colombia, Department of Astronomy, University of Wisconsin, 475 N. Charter Street, Madison, WI, United States
D'Onghia, E., Department of Astronomy, University of Wisconsin, 475 N. Charter Street, Madison, WI, United States
Navarro, J.F., Department of Physics and Astronomy, University of Victoria, Victoria, BC, Canada
dc.subject.spa.fl_str_mv galaxies: kinematics and dynamics
Galaxy: disk
Galaxy: evolution
stars: kinematics and dynamics
topic galaxies: kinematics and dynamics
Galaxy: disk
Galaxy: evolution
stars: kinematics and dynamics
description We use numerical simulations to examine the effects of radial migration on the vertical structure of galaxy disks. The simulations follow three exponential disks of different mass but similar circular velocity, radial scalelength, and (constant) scale height. The disks develop different non-axisymmetric patterns, ranging from feeble, long-lived multiple arms to strong, rapidly evolving few-armed spirals. These fluctuations induce radial migration through secular changes in the angular momentum of disk particles, mixing the disk radially and blurring pre-existing gradients. Migration primarily affects stars with small vertical excursions, regardless of spiral pattern. This "provenance bias" largely determines the vertical structure of migrating stars: inward migrators thin down as they move in, whereas outward migrators do not thicken up but rather preserve the disk scale height at their destination. Migrators of equal birth radius thus develop a strong scale-height gradient, not by flaring out as commonly assumed, but by thinning down as they spread inward. Similar gradients have been observed for low-[α/Fe] mono-abundance populations (MAPs) in the Galaxy, but our results argue against interpreting them as a consequence of radial migration. This is because outward migration does not lead to thickening, implying that the maximum scale height of any population should reflect its value at birth. In contrast, Galactic MAPs have scale heights that increase monotonically outward, reaching values that greatly exceed those at their presumed birth radii. Given the strong vertical bias affecting migration, a proper assessment of the importance of radial migration in the Galaxy should take carefully into account the strong radial dependence of the scale heights of the various stellar populations. © 2016. The American Astronomical Society. All rights reserved.
publishDate 2016
dc.date.created.none.fl_str_mv 2016
dc.date.accessioned.none.fl_str_mv 2017-05-12T16:05:58Z
dc.date.available.none.fl_str_mv 2017-05-12T16:05:58Z
dc.type.eng.fl_str_mv Article
dc.type.coar.fl_str_mv http://purl.org/coar/resource_type/c_6501
http://purl.org/coar/resource_type/c_2df8fbb1
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dc.identifier.uri.none.fl_str_mv http://hdl.handle.net/11407/3155
dc.identifier.doi.none.fl_str_mv 10.3847/1538-4357/833/1/42
identifier_str_mv 0004637X
10.3847/1538-4357/833/1/42
url http://hdl.handle.net/11407/3155
dc.language.iso.none.fl_str_mv eng
language eng
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dc.relation.ispartofes.spa.fl_str_mv Astrophysical Journal
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dc.publisher.spa.fl_str_mv Institute of Physics Publishing
dc.source.spa.fl_str_mv Scopus
institution Universidad de Medellín
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