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...
- Autores:
- Tipo de recurso:
- 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
- Rights
- restrictedAccess
- License
- http://purl.org/coar/access_right/c_16ec
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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 |
dc.type.driver.none.fl_str_mv |
info:eu-repo/semantics/article |
dc.identifier.issn.none.fl_str_mv |
0004637X |
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 |
dc.relation.isversionof.spa.fl_str_mv |
http://iopscience.iop.org/article/10.3847/1538-4357/833/1/42/meta;jsessionid=21FEC6A946A7E41099C7371A38264FD2.c1.iopscience.cld.iop.org |
dc.relation.ispartofes.spa.fl_str_mv |
Astrophysical Journal |
dc.rights.coar.fl_str_mv |
http://purl.org/coar/access_right/c_16ec |
dc.rights.accessrights.none.fl_str_mv |
info:eu-repo/semantics/restrictedAccess |
eu_rights_str_mv |
restrictedAccess |
rights_invalid_str_mv |
http://purl.org/coar/access_right/c_16ec |
dc.publisher.spa.fl_str_mv |
Institute of Physics Publishing |
dc.source.spa.fl_str_mv |
Scopus |
institution |
Universidad de Medellín |
bitstream.url.fl_str_mv |
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