Radial migration does little for Galactic disc thickening
Identifieur interne : 005963 ( Main/Exploration ); précédent : 005962; suivant : 005964Radial migration does little for Galactic disc thickening
Auteurs : I. Minchev [Allemagne] ; B. Famaey [France, Allemagne] ; A. C. Quillen [États-Unis] ; W. Dehnen [Royaume-Uni] ; M. Martig [Australie] ; A. Siebert [France]Source :
- Astronomy and astrophysics : (Berlin. Print) [ 0004-6361 ] ; 2012.
Descripteurs français
- Pascal (Inist)
English descriptors
- KwdEn :
Abstract
Non-axisymmetric components, such as spirals and central bars, play a major role in shaping galactic discs. An important aspect of the disc secular evolution driven by these perturbers is the radial migration of stars. It has been suggested recently that migration can populate a thick-disc component from inner-disc stars with high vertical energies. Since this has never been demonstrated in simulations, we study in detail the effect of radial migration on the disc velocity dispersion and disc thickness, by separating simulated stars into migrators and non-migrators. We apply this method to three isolated barred Tree-SPH N-body galaxies with strong radial migration. Contrary to expectations, we find that as stellar samples migrate, on the average, their velocity dispersion change (by as much as 50%) in such a way as to approximately match the non-migrating population at the radius at which they arrive. We show that, in fact, migrators suppress heating in parts of the disc. To confirm the validity of our findings, we also apply our technique to three cosmological re-simulations, which use a completely different simulation scheme and, remarkably, find very similar results. We believe the inability of migration to thicken discs is a fundamental property of internal disc evolution, irrespective of the migration mechanism at work. We explain this with the approximate conservation of the (average) vertical and radial actions rather than the energy. This "action mixing" can be used to constrain the migration rate in the Milky Way: estimates of the average vertical action in observations for different populations of stars should reveal flattening with radius for older groups of stars.
Affiliations:
- Allemagne, Australie, France, Royaume-Uni, États-Unis
- Alsace (région administrative), Brandebourg, Grand Est
- Potsdam, Strasbourg
- Université de Strasbourg
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Minchev</name><affiliation wicri:level="3"><inist:fA14 i1="01"><s1>Leibniz-Institut fü Astrophysik Potsdam (AIP), An der Sternwarte 16</s1><s2>14482, Potsdam</s2><s3>DEU</s3><sZ>1 aut.</sZ></inist:fA14><country>Allemagne</country><placeName><region type="land" nuts="2">Brandebourg</region><settlement type="city">Potsdam</settlement></placeName></affiliation></author><author><name sortKey="Famaey, B" sort="Famaey, B" uniqKey="Famaey B" first="B." last="Famaey">B. Famaey</name><affiliation wicri:level="4"><inist:fA14 i1="02"><s1>Université de Strasbourg, CNRS, Observatoire Astronomique, 11 rue de l'Université</s1><s2>67000 Strasbourg</s2><s3>FRA</s3><sZ>2 aut.</sZ><sZ>6 aut.</sZ></inist:fA14><country>France</country><wicri:noRegion>67000 Strasbourg</wicri:noRegion><placeName><settlement type="city">Strasbourg</settlement><region type="region" nuts="2">Grand Est</region><region type="old region" nuts="2">Alsace (région administrative)</region><settlement type="city">Strasbourg</settlement></placeName><orgName type="university">Université de Strasbourg</orgName></affiliation><affiliation wicri:level="1"><inist:fA14 i1="03"><s1>AIfA, University of Bonn</s1><s3>DEU</s3><sZ>2 aut.</sZ></inist:fA14><country>Allemagne</country><wicri:noRegion>University of Bonn</wicri:noRegion><wicri:noRegion>AIfA, University of Bonn</wicri:noRegion></affiliation></author><author><name sortKey="Quillen, A C" sort="Quillen, A C" uniqKey="Quillen A" first="A. 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Martig</name><affiliation wicri:level="1"><inist:fA14 i1="06"><s1>Centre for Astrophysics & Supercomputing, Swinburne University of Technology, PO Box 218</s1><s2>Hawthorn, VIC 3122</s2><s3>AUS</s3><sZ>5 aut.</sZ></inist:fA14><country>Australie</country><wicri:noRegion>Hawthorn, VIC 3122</wicri:noRegion></affiliation></author><author><name sortKey="Siebert, A" sort="Siebert, A" uniqKey="Siebert A" first="A." last="Siebert">A. Siebert</name><affiliation wicri:level="4"><inist:fA14 i1="02"><s1>Université de Strasbourg, CNRS, Observatoire Astronomique, 11 rue de l'Université</s1><s2>67000 Strasbourg</s2><s3>FRA</s3><sZ>2 aut.</sZ><sZ>6 aut.</sZ></inist:fA14><country>France</country><wicri:noRegion>67000 Strasbourg</wicri:noRegion><placeName><settlement type="city">Strasbourg</settlement><region type="region" nuts="2">Grand Est</region><region type="old region" nuts="2">Alsace (région administrative)</region><settlement type="city">Strasbourg</settlement></placeName><orgName type="university">Université de Strasbourg</orgName></affiliation></author></analytic><series><title level="j" type="main">Astronomy and astrophysics : (Berlin. Print)</title><title level="j" type="abbreviated">Astron. astrophys. : (Berl., Print)</title><idno type="ISSN">0004-6361</idno><imprint><date when="2012">2012</date></imprint></series></biblStruct></sourceDesc><seriesStmt><title level="j" type="main">Astronomy and astrophysics : (Berlin. Print)</title><title level="j" type="abbreviated">Astron. astrophys. : (Berl., Print)</title><idno type="ISSN">0004-6361</idno></seriesStmt></fileDesc><profileDesc><textClass><keywords scheme="KwdEn" xml:lang="en"><term>Disk galaxies</term><term>Dynamics</term><term>Flattening</term><term>Galactic disks</term><term>Galaxy evolution</term><term>Galaxy structure</term><term>Kinematics</term><term>Milky Way</term><term>Mixing</term><term>N galaxies</term><term>Velocity dispersion</term></keywords><keywords scheme="Pascal" xml:lang="fr"><term>Disque galactique</term><term>Dispersion vitesse</term><term>Galaxies N</term><term>Mélangeage</term><term>Voie lactée</term><term>Aplatissement</term><term>Galaxies disques</term><term>Evolution galaxies</term><term>Cinématique</term><term>Dynamique</term><term>Structure galaxies</term></keywords></textClass></profileDesc></teiHeader><front><div type="abstract" xml:lang="en">Non-axisymmetric components, such as spirals and central bars, play a major role in shaping galactic discs. An important aspect of the disc secular evolution driven by these perturbers is the radial migration of stars. It has been suggested recently that migration can populate a thick-disc component from inner-disc stars with high vertical energies. Since this has never been demonstrated in simulations, we study in detail the effect of radial migration on the disc velocity dispersion and disc thickness, by separating simulated stars into migrators and non-migrators. We apply this method to three isolated barred Tree-SPH N-body galaxies with strong radial migration. Contrary to expectations, we find that as stellar samples migrate, on the average, their velocity dispersion change (by as much as 50%) in such a way as to approximately match the non-migrating population at the radius at which they arrive. We show that, in fact, migrators suppress heating in parts of the disc. To confirm the validity of our findings, we also apply our technique to three cosmological re-simulations, which use a completely different simulation scheme and, remarkably, find very similar results. We believe the inability of migration to thicken discs is a fundamental property of internal disc evolution, irrespective of the migration mechanism at work. We explain this with the approximate conservation of the (average) vertical and radial actions rather than the energy. This "action mixing" can be used to constrain the migration rate in the Milky Way: estimates of the average vertical action in observations for different populations of stars should reveal flattening with radius for older groups of stars.</div></front></TEI><affiliations><list><country><li>Allemagne</li><li>Australie</li><li>France</li><li>Royaume-Uni</li><li>États-Unis</li></country><region><li>Alsace (région administrative)</li><li>Brandebourg</li><li>Grand Est</li></region><settlement><li>Potsdam</li><li>Strasbourg</li></settlement><orgName><li>Université de Strasbourg</li></orgName></list><tree><country name="Allemagne"><region name="Brandebourg"><name sortKey="Minchev, I" sort="Minchev, I" uniqKey="Minchev I" first="I." last="Minchev">I. Minchev</name></region><name sortKey="Famaey, B" sort="Famaey, B" uniqKey="Famaey B" first="B." last="Famaey">B. Famaey</name></country><country name="France"><region name="Grand Est"><name sortKey="Famaey, B" sort="Famaey, B" uniqKey="Famaey B" first="B." last="Famaey">B. Famaey</name></region><name sortKey="Siebert, A" sort="Siebert, A" uniqKey="Siebert A" first="A." last="Siebert">A. Siebert</name></country><country name="États-Unis"><noRegion><name sortKey="Quillen, A C" sort="Quillen, A C" uniqKey="Quillen A" first="A. C." last="Quillen">A. C. Quillen</name></noRegion></country><country name="Royaume-Uni"><noRegion><name sortKey="Dehnen, W" sort="Dehnen, W" uniqKey="Dehnen W" first="W." last="Dehnen">W. Dehnen</name></noRegion></country><country name="Australie"><noRegion><name sortKey="Martig, M" sort="Martig, M" uniqKey="Martig M" first="M." last="Martig">M. Martig</name></noRegion></country></tree></affiliations></record>Pour manipuler ce document sous Unix (Dilib)
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