Is the Milky Way ringing? The hunt for high‐velocity streams
Identifieur interne : 001868 ( Istex/Corpus ); précédent : 001867; suivant : 001869Is the Milky Way ringing? The hunt for high‐velocity streams
Auteurs : I. Minchev ; A. C. Quillen ; M. Williams ; K. C. Freeman ; J. Nordhaus ; A. Siebert ; O. BienayméSource :
- Monthly Notices of the Royal Astronomical Society: Letters [ 1745-3925 ] ; 2009-06-11.
English descriptors
- KwdEn :
- Angular momentum, Arcturus stream, Arifyanto fuchs, Circular orbit, Cole weinberg, Cosmological context, Dehnen, Different ways, Disc, Epicyclic, Epicyclic frequency, Galactic, Galactic disc, Galactic radii, Galactocentric distance, Galaxy, Gaussian distributions, Helmi, Host disc, Host system, Initial conditions, Initial particle distribution, Journal compilation, Kinematics, Large range, Local velocity, Mass ratio, Metallicity range, Minchev, Minchev quillen, Mnras, Numerical simulations, Orbital eccentricity, Overdensities, Particular time, Phase space, Quillen, Rotation curve, Satellite mergers, Simulation, Solar neighbourhood, Solid line, Stellar, Stellar population, Tangential, Tangential velocity, Tangential velocity distribution, Thick disc, Time development, Time outputs, Velocity distribution, Velocity space, Weighting function.
- Teeft :
- Angular momentum, Arcturus stream, Arifyanto fuchs, Circular orbit, Cole weinberg, Cosmological context, Dehnen, Different ways, Disc, Epicyclic, Epicyclic frequency, Galactic, Galactic disc, Galactic radii, Galactocentric distance, Galaxy, Gaussian distributions, Helmi, Host disc, Host system, Initial conditions, Initial particle distribution, Journal compilation, Kinematics, Large range, Local velocity, Mass ratio, Metallicity range, Minchev, Minchev quillen, Mnras, Numerical simulations, Orbital eccentricity, Overdensities, Particular time, Phase space, Quillen, Rotation curve, Satellite mergers, Simulation, Solar neighbourhood, Solid line, Stellar, Stellar population, Tangential, Tangential velocity, Tangential velocity distribution, Thick disc, Time development, Time outputs, Velocity distribution, Velocity space, Weighting function.
Abstract
We perform numerical simulations of a stellar galactic disc with initial conditions chosen to represent an unrelaxed population which might have been left following a merger. Stars are unevenly distributed in radial action angle, though the disc is axisymmetric. The velocity distribution in the simulated solar neighbourhood exhibits waves travelling in the direction of positive v, where u, v are the radial and tangential velocity components. As the system relaxes and structure wraps in phase space, the features seen in the u–v plane move closer together. We show that these results can be obtained also by a semi‐analytical method. We propose that this model could provide an explanation for the high‐velocity streams seen in the solar neighbourhood at approximate v in km s−1, of −60 (HR 1614), −80, −100 (Arcturus) and −160. In addition, we predict four new features at v≈−140, −120, 40 and 60 km s−1. By matching the number and positions of the observed streams, we estimate that the Milky Way disc was strongly perturbed ∼1.9 Gyr ago. This event could have been associated with Galactic bar formation.
Url:
DOI: 10.1111/j.1745-3933.2009.00661.x
Links to Exploration step
ISTEX:82AE59B01C78B85B04D93F8211A22EF8A6F6FDF2Le document en format XML
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Stars are unevenly distributed in radial action angle, though the disc is axisymmetric. The velocity distribution in the simulated solar neighbourhood exhibits waves travelling in the direction of positive v, where u, v are the radial and tangential velocity components. As the system relaxes and structure wraps in phase space, the features seen in the u–v plane move closer together. We show that these results can be obtained also by a semi‐analytical method. We propose that this model could provide an explanation for the high‐velocity streams seen in the solar neighbourhood at approximate v in km s−1, of −60 (HR 1614), −80, −100 (Arcturus) and −160. In addition, we predict four new features at v≈−140, −120, 40 and 60 km s−1. By matching the number and positions of the observed streams, we estimate that the Milky Way disc was strongly perturbed ∼1.9 Gyr ago. This event could have been associated with Galactic bar formation.</div></front></TEI><istex><corpusName>wiley</corpusName><keywords><teeft><json:string>mnras</json:string><json:string>minchev</json:string><json:string>helmi</json:string><json:string>quillen</json:string><json:string>epicyclic</json:string><json:string>dehnen</json:string><json:string>kinematics</json:string><json:string>overdensities</json:string><json:string>thick disc</json:string><json:string>rotation curve</json:string><json:string>galactic</json:string><json:string>journal compilation</json:string><json:string>simulation</json:string><json:string>galactic disc</json:string><json:string>velocity distribution</json:string><json:string>arifyanto fuchs</json:string><json:string>galactocentric distance</json:string><json:string>numerical simulations</json:string><json:string>local velocity</json:string><json:string>velocity space</json:string><json:string>epicyclic frequency</json:string><json:string>stellar</json:string><json:string>tangential</json:string><json:string>initial conditions</json:string><json:string>tangential velocity</json:string><json:string>minchev quillen</json:string><json:string>host disc</json:string><json:string>time development</json:string><json:string>different ways</json:string><json:string>weighting function</json:string><json:string>phase space</json:string><json:string>disc</json:string><json:string>galaxy</json:string><json:string>solar neighbourhood</json:string><json:string>mass ratio</json:string><json:string>cosmological context</json:string><json:string>host system</json:string><json:string>arcturus stream</json:string><json:string>satellite mergers</json:string><json:string>stellar population</json:string><json:string>solid line</json:string><json:string>time outputs</json:string><json:string>gaussian distributions</json:string><json:string>large range</json:string><json:string>galactic radii</json:string><json:string>tangential velocity distribution</json:string><json:string>circular orbit</json:string><json:string>angular momentum</json:string><json:string>cole weinberg</json:string><json:string>initial particle distribution</json:string><json:string>orbital eccentricity</json:string><json:string>particular time</json:string><json:string>metallicity range</json:string></teeft></keywords><author><json:item><name>I. Minchev</name><affiliations><json:string>Université de Strasbourg, CNRS, Observatoire Astronomique, 67000 Strasbourg, France</json:string><json:string>E-mail: minchev@astro.u‐strasbg.fr</json:string></affiliations></json:item><json:item><name>A. C. Quillen</name><affiliations><json:string>Department of Physics and Astronomy, University of Rochester, Rochester, NY 14627, USA</json:string></affiliations></json:item><json:item><name>M. Williams</name><affiliations><json:string>Mount Stromlo Observatory, Australian National University, Cotter Road, ACT 2611, Australia</json:string><json:string>Astrophysikalisches Institut Potsdam, An der Sternwarte 16, D‐14482 Potsdam, Germany</json:string></affiliations></json:item><json:item><name>K. C. Freeman</name><affiliations><json:string>Australian National University, Canberra, ACT 200, Australia</json:string></affiliations></json:item><json:item><name>J. Nordhaus</name><affiliations><json:string>Department of Astrophysical Sciences, Princeton University, Princeton, NJ 08544, USA</json:string></affiliations></json:item><json:item><name>A. Siebert</name><affiliations><json:string>Université de Strasbourg, CNRS, Observatoire Astronomique, 67000 Strasbourg, France</json:string></affiliations></json:item><json:item><name>O. Bienaymé</name><affiliations><json:string>Université de Strasbourg, CNRS, Observatoire Astronomique, 67000 Strasbourg, France</json:string></affiliations></json:item></author><subject><json:item><lang><json:string>eng</json:string></lang><value>stellar dynamics</value></json:item><json:item><lang><json:string>eng</json:string></lang><value>Galaxy: evolution</value></json:item><json:item><lang><json:string>eng</json:string></lang><value>Galaxy: kinematics and dynamicsn</value></json:item><json:item><lang><json:string>eng</json:string></lang><value>solar neighbourhood</value></json:item><json:item><lang><json:string>eng</json:string></lang><value>galaxies: evolution</value></json:item></subject><articleId><json:string>MNL20661</json:string></articleId><arkIstex>ark:/67375/WNG-JP2P17X9-Z</arkIstex><language><json:string>eng</json:string></language><originalGenre><json:string>article</json:string></originalGenre><abstract>We perform numerical simulations of a stellar galactic disc with initial conditions chosen to represent an unrelaxed population which might have been left following a merger. Stars are unevenly distributed in radial action angle, though the disc is axisymmetric. The velocity distribution in the simulated solar neighbourhood exhibits waves travelling in the direction of positive v, where u, v are the radial and tangential velocity components. As the system relaxes and structure wraps in phase space, the features seen in the u–v plane move closer together. We show that these results can be obtained also by a semi‐analytical method. We propose that this model could provide an explanation for the high‐velocity streams seen in the solar neighbourhood at approximate v in km s−1, of −60 (HR 1614), −80, −100 (Arcturus) and −160. In addition, we predict four new features at v≈−140, −120, 40 and 60 km s−1. By matching the number and positions of the observed streams, we estimate that the Milky Way disc was strongly perturbed ∼1.9 Gyr ago. This event could have been associated with Galactic bar formation.</abstract><qualityIndicators><score>8.363</score><pdfWordCount>4263</pdfWordCount><pdfCharCount>21982</pdfCharCount><pdfVersion>1.4</pdfVersion><pdfPageCount>5</pdfPageCount><pdfPageSize>595.274 x 782.286 pts</pdfPageSize><refBibsNative>true</refBibsNative><abstractWordCount>175</abstractWordCount><abstractCharCount>1111</abstractCharCount><keywordCount>5</keywordCount></qualityIndicators><title>Is the Milky Way ringing? 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(1993)</json:string><json:string>Navarro et al. (2004)</json:string><json:string>Kazantzidis et al. (2008)</json:string><json:string>De Lucia & Helmi 2008</json:string><json:string>Walker et al. (1996)</json:string><json:string>Bekki & Freeman 2003</json:string><json:string>Sellwood & Binney 2002</json:string><json:string>Minchev et al. 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The hunt for high‐velocity streams</title><title level="a" type="short">Is the Milky Way ringing?</title><author xml:id="author-0000" role="corresp"><persName><forename type="first">I.</forename><surname>Minchev</surname></persName><affiliation>Université de Strasbourg, CNRS, Observatoire Astronomique, 67000 Strasbourg, France<address><country key="FR"></country></address></affiliation><affiliation>E‐mail: minchev@astro.u‐strasbg.fr</affiliation></author><author xml:id="author-0001"><persName><forename type="first">A. C.</forename><surname>Quillen</surname></persName><affiliation>Department of Physics and Astronomy, University of Rochester, Rochester, NY 14627, USA<address><country key="US"></country></address></affiliation></author><author xml:id="author-0002"><persName><forename type="first">M.</forename><surname>Williams</surname></persName><affiliation>Mount Stromlo Observatory, Australian National University, Cotter Road, ACT 2611, Australia<address><country key="AU"></country></address></affiliation><affiliation>Astrophysikalisches Institut Potsdam, An der Sternwarte 16, D‐14482 Potsdam, Germany<address><country key="DE"></country></address></affiliation></author><author xml:id="author-0003"><persName><forename type="first">K. C.</forename><surname>Freeman</surname></persName><affiliation>Australian National University, Canberra, ACT 200, Australia<address><country key="AU"></country></address></affiliation></author><author xml:id="author-0004"><persName><forename type="first">J.</forename><surname>Nordhaus</surname></persName><affiliation>Department of Astrophysical Sciences, Princeton University, Princeton, NJ 08544, USA<address><country key="US"></country></address></affiliation></author><author xml:id="author-0005"><persName><forename type="first">A.</forename><surname>Siebert</surname></persName><affiliation>Université de Strasbourg, CNRS, Observatoire Astronomique, 67000 Strasbourg, France<address><country key="FR"></country></address></affiliation></author><author xml:id="author-0006"><persName><forename type="first">O.</forename><surname>Bienaymé</surname></persName><affiliation>Université de Strasbourg, CNRS, Observatoire Astronomique, 67000 Strasbourg, France<address><country key="FR"></country></address></affiliation></author><idno type="istex">82AE59B01C78B85B04D93F8211A22EF8A6F6FDF2</idno><idno type="ark">ark:/67375/WNG-JP2P17X9-Z</idno><idno type="DOI">10.1111/j.1745-3933.2009.00661.x</idno><idno type="unit">MNL20661</idno><idno type="toTypesetVersion">file:MNL2.MNL20661.pdf</idno></analytic><monogr><title level="j" type="main">Monthly Notices of the Royal Astronomical Society: Letters</title><title level="j" type="alt">MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LETTERS</title><idno type="pISSN">1745-3925</idno><idno type="eISSN">1745-3933</idno><idno type="book-DOI">10.1111/(ISSN)1745-3933</idno><idno type="book-part-DOI">10.1111/mnl.2009.396.issue-1</idno><idno type="product">MNL2</idno><idno type="publisherDivision">ST</idno><imprint><biblScope unit="vol">396</biblScope><biblScope unit="issue">1</biblScope><biblScope unit="page" from="L56">L56</biblScope><biblScope unit="page" to="L60">L60</biblScope><biblScope unit="page-count">5</biblScope><publisher>Blackwell Publishing Ltd</publisher><pubPlace>Oxford, UK</pubPlace><date type="published" when="2009-06-11"></date></imprint></monogr></biblStruct></sourceDesc></fileDesc><profileDesc><abstract xml:lang="en" style="main"><head>ABSTRACT</head><p>We perform numerical simulations of a stellar galactic disc with initial conditions chosen to represent an unrelaxed population which might have been left following a merger. Stars are unevenly distributed in radial action angle, though the disc is axisymmetric. The velocity distribution in the simulated solar neighbourhood exhibits waves travelling in the direction of positive <hi rend="italic">v</hi>, where <hi rend="italic">u</hi>, <hi rend="italic">v</hi> are the radial and tangential velocity components. As the system relaxes and structure wraps in phase space, the features seen in the <hi rend="italic">u</hi>–<hi rend="italic">v</hi> plane move closer together. We show that these results can be obtained also by a semi‐analytical method. We propose that this model could provide an explanation for the high‐velocity streams seen in the solar neighbourhood at approximate <hi rend="italic">v</hi> in km s<hi rend="superscript">−1</hi>, of −60 (HR 1614), −80, −100 (Arcturus) and −160. In addition, we predict four new features at <emph><span><hi rend="italic">v</hi>≈−140, −120, 40</span></emph> and 60 km s<hi rend="superscript">−1</hi>. By matching the number and positions of the observed streams, we estimate that the Milky Way disc was strongly perturbed ∼1.9 Gyr ago. This event could have been associated with Galactic bar formation.</p></abstract><textClass><keywords xml:lang="en"><term xml:id="k1">stellar dynamics</term><term xml:id="k2">Galaxy: evolution</term><term xml:id="k3">Galaxy: kinematics and dynamicsn</term><term xml:id="k4">solar neighbourhood</term><term xml:id="k5">galaxies: evolution</term></keywords><keywords rend="tocHeading1"><term>Letters</term></keywords></textClass><langUsage><language ident="en"></language></langUsage></profileDesc></teiHeader></istex:fulltextTEI><json:item><extension>txt</extension><original>false</original><mimetype>text/plain</mimetype><uri>https://api.istex.fr/document/82AE59B01C78B85B04D93F8211A22EF8A6F6FDF2/fulltext/txt</uri></json:item></fulltext><metadata><istex:metadataXml wicri:clean="Wiley, elements deleted: body"><istex:xmlDeclaration>version="1.0" encoding="UTF-8" standalone="yes"</istex:xmlDeclaration><istex:document><component version="2.0" type="serialArticle" xml:lang="en"><header><publicationMeta level="product"><publisherInfo><publisherName>Blackwell Publishing Ltd</publisherName><publisherLoc>Oxford, UK</publisherLoc></publisherInfo><doi origin="wiley" registered="yes">10.1111/(ISSN)1745-3933</doi><issn type="print">1745-3925</issn><issn type="electronic">1745-3933</issn><idGroup><id type="product" value="MNL2"></id><id type="publisherDivision" value="ST"></id></idGroup><titleGroup><title type="main" sort="MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LETTERS">Monthly Notices of the Royal Astronomical Society: Letters</title></titleGroup></publicationMeta><publicationMeta level="part" position="06001"><doi origin="wiley">10.1111/mnl.2009.396.issue-1</doi><numberingGroup><numbering type="journalVolume" number="396">396</numbering><numbering type="journalIssue" number="1">1</numbering></numberingGroup><coverDate startDate="2009-06-11">June 2009</coverDate></publicationMeta><publicationMeta level="unit" type="article" position="12" status="forIssue"><doi origin="wiley">10.1111/j.1745-3933.2009.00661.x</doi><idGroup><id type="unit" value="MNL20661"></id></idGroup><countGroup><count type="pageTotal" number="5"></count></countGroup><titleGroup><title type="tocHeading1">Letters</title></titleGroup><copyright>© 2009 The Authors. 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E‐mail: <email normalForm="minchev@astro.u-strasbg.fr">minchev@astro.u‐strasbg.fr</email></correspondenceTo><linkGroup><link type="toTypesetVersion" href="file:MNL2.MNL20661.pdf"></link></linkGroup></publicationMeta><contentMeta><unparsedEditorialHistory>Accepted 2009 March 23. Received 2009 March 16; in original form 2009 February 10</unparsedEditorialHistory><countGroup><count type="figureTotal" number="4"></count><count type="tableTotal" number="0"></count><count type="formulaTotal" number="74"></count><count type="referenceTotal" number="40"></count><count type="linksCrossRef" number="89"></count></countGroup><titleGroup><title type="main">Is the Milky Way ringing? The hunt for high‐velocity streams</title><title type="shortAuthors"><i>I. Minchev et al.</i></title><title type="short"><i>Is the Milky Way ringing</i>?</title></titleGroup><creators><creator creatorRole="author" xml:id="cr1" affiliationRef="#a1" corresponding="yes"><personName><givenNames>I.</givenNames><familyName>Minchev</familyName></personName></creator><creator creatorRole="author" xml:id="cr2" affiliationRef="#a2"><personName><givenNames>A. C.</givenNames><familyName>Quillen</familyName></personName></creator><creator creatorRole="author" xml:id="cr3" affiliationRef="#a3 #a4"><personName><givenNames>M.</givenNames><familyName>Williams</familyName></personName></creator><creator creatorRole="author" xml:id="cr4" affiliationRef="#a5"><personName><givenNames>K. C.</givenNames><familyName>Freeman</familyName></personName></creator><creator creatorRole="author" xml:id="cr5" affiliationRef="#a6"><personName><givenNames>J.</givenNames><familyName>Nordhaus</familyName></personName></creator><creator creatorRole="author" xml:id="cr6" affiliationRef="#a1"><personName><givenNames>A.</givenNames><familyName>Siebert</familyName></personName></creator><creator creatorRole="author" xml:id="cr7" affiliationRef="#a1"><personName><givenNames>O.</givenNames><familyName>Bienaymé</familyName></personName></creator></creators><affiliationGroup><affiliation xml:id="a1" countryCode="FR"><unparsedAffiliation>Université de Strasbourg, CNRS, Observatoire Astronomique, 67000 Strasbourg, France</unparsedAffiliation></affiliation><affiliation xml:id="a2" countryCode="US"><unparsedAffiliation>Department of Physics and Astronomy, University of Rochester, Rochester, NY 14627, USA</unparsedAffiliation></affiliation><affiliation xml:id="a3" countryCode="AU"><unparsedAffiliation>Mount Stromlo Observatory, Australian National University, Cotter Road, ACT 2611, Australia</unparsedAffiliation></affiliation><affiliation xml:id="a4" countryCode="DE"><unparsedAffiliation>Astrophysikalisches Institut Potsdam, An der Sternwarte 16, D‐14482 Potsdam, Germany</unparsedAffiliation></affiliation><affiliation xml:id="a5" countryCode="AU"><unparsedAffiliation>Australian National University, Canberra, ACT 200, Australia</unparsedAffiliation></affiliation><affiliation xml:id="a6" countryCode="US"><unparsedAffiliation>Department of Astrophysical Sciences, Princeton University, Princeton, NJ 08544, USA</unparsedAffiliation></affiliation></affiliationGroup><keywordGroup xml:lang="en"><keyword xml:id="k1">stellar dynamics</keyword><keyword xml:id="k2">Galaxy: evolution</keyword><keyword xml:id="k3">Galaxy: kinematics and dynamicsn</keyword><keyword xml:id="k4">solar neighbourhood</keyword><keyword xml:id="k5">galaxies: evolution</keyword></keywordGroup><abstractGroup><abstract type="main" xml:lang="en"><title type="main">ABSTRACT</title><p>We perform numerical simulations of a stellar galactic disc with initial conditions chosen to represent an unrelaxed population which might have been left following a merger. Stars are unevenly distributed in radial action angle, though the disc is axisymmetric. The velocity distribution in the simulated solar neighbourhood exhibits waves travelling in the direction of positive <i>v</i>, where <i>u</i>, <i>v</i> are the radial and tangential velocity components. As the system relaxes and structure wraps in phase space, the features seen in the <i>u</i>–<i>v</i> plane move closer together. We show that these results can be obtained also by a semi‐analytical method. We propose that this model could provide an explanation for the high‐velocity streams seen in the solar neighbourhood at approximate <i>v</i> in km s<sup>−1</sup>, of −60 (HR 1614), −80, −100 (Arcturus) and −160. In addition, we predict four new features at <span type="mathematics"><i>v</i>≈−140, −120, 40</span> and 60 km s<sup>−1</sup>. By matching the number and positions of the observed streams, we estimate that the Milky Way disc was strongly perturbed ∼1.9 Gyr ago. This event could have been associated with Galactic bar formation.</p></abstract></abstractGroup></contentMeta></header></component></istex:document></istex:metadataXml><mods version="3.6"><titleInfo lang="en"><title>Is the Milky Way ringing? The hunt for high‐velocity streams</title></titleInfo><titleInfo type="abbreviated" lang="en"><title>Is the Milky Way ringing?</title></titleInfo><titleInfo type="alternative" contentType="CDATA" lang="en"><title>Is the Milky Way ringing? The hunt for high‐velocity streams</title></titleInfo><name type="personal"><namePart type="given">I.</namePart><namePart type="family">Minchev</namePart><affiliation>Université de Strasbourg, CNRS, Observatoire Astronomique, 67000 Strasbourg, France</affiliation><affiliation>E-mail: minchev@astro.u‐strasbg.fr</affiliation><role><roleTerm type="text">author</roleTerm></role></name><name type="personal"><namePart type="given">A. C.</namePart><namePart type="family">Quillen</namePart><affiliation>Department of Physics and Astronomy, University of Rochester, Rochester, NY 14627, USA</affiliation><role><roleTerm type="text">author</roleTerm></role></name><name type="personal"><namePart type="given">M.</namePart><namePart type="family">Williams</namePart><affiliation>Mount Stromlo Observatory, Australian National University, Cotter Road, ACT 2611, Australia</affiliation><affiliation>Astrophysikalisches Institut Potsdam, An der Sternwarte 16, D‐14482 Potsdam, Germany</affiliation><role><roleTerm type="text">author</roleTerm></role></name><name type="personal"><namePart type="given">K. C.</namePart><namePart type="family">Freeman</namePart><affiliation>Australian National University, Canberra, ACT 200, Australia</affiliation><role><roleTerm type="text">author</roleTerm></role></name><name type="personal"><namePart type="given">J.</namePart><namePart type="family">Nordhaus</namePart><affiliation>Department of Astrophysical Sciences, Princeton University, Princeton, NJ 08544, USA</affiliation><role><roleTerm type="text">author</roleTerm></role></name><name type="personal"><namePart type="given">A.</namePart><namePart type="family">Siebert</namePart><affiliation>Université de Strasbourg, CNRS, Observatoire Astronomique, 67000 Strasbourg, France</affiliation><role><roleTerm type="text">author</roleTerm></role></name><name type="personal"><namePart type="given">O.</namePart><namePart type="family">Bienaymé</namePart><affiliation>Université de Strasbourg, CNRS, Observatoire Astronomique, 67000 Strasbourg, France</affiliation><role><roleTerm type="text">author</roleTerm></role></name><typeOfResource>text</typeOfResource><genre type="article" displayLabel="article" authority="ISTEX" authorityURI="https://content-type.data.istex.fr" valueURI="https://content-type.data.istex.fr/ark:/67375/XTP-6N5SZHKN-D">article</genre><originInfo><publisher>Blackwell Publishing Ltd</publisher><place><placeTerm type="text">Oxford, UK</placeTerm></place><dateIssued encoding="w3cdtf">2009-06-11</dateIssued><edition>Accepted 2009 March 23. Received 2009 March 16; in original form 2009 February 10</edition><copyrightDate encoding="w3cdtf">2009</copyrightDate></originInfo><language><languageTerm type="code" authority="rfc3066">en</languageTerm><languageTerm type="code" authority="iso639-2b">eng</languageTerm></language><physicalDescription><extent unit="figures">4</extent><extent unit="tables">0</extent><extent unit="formulas">74</extent><extent unit="references">40</extent><extent unit="linksCrossRef">89</extent></physicalDescription><abstract lang="en">We perform numerical simulations of a stellar galactic disc with initial conditions chosen to represent an unrelaxed population which might have been left following a merger. Stars are unevenly distributed in radial action angle, though the disc is axisymmetric. The velocity distribution in the simulated solar neighbourhood exhibits waves travelling in the direction of positive v, where u, v are the radial and tangential velocity components. As the system relaxes and structure wraps in phase space, the features seen in the u–v plane move closer together. We show that these results can be obtained also by a semi‐analytical method. We propose that this model could provide an explanation for the high‐velocity streams seen in the solar neighbourhood at approximate v in km s−1, of −60 (HR 1614), −80, −100 (Arcturus) and −160. In addition, we predict four new features at v≈−140, −120, 40 and 60 km s−1. By matching the number and positions of the observed streams, we estimate that the Milky Way disc was strongly perturbed ∼1.9 Gyr ago. This event could have been associated with Galactic bar formation.</abstract><subject lang="en"><genre>keywords</genre><topic>stellar dynamics</topic><topic>Galaxy: evolution</topic><topic>Galaxy: kinematics and dynamicsn</topic><topic>solar neighbourhood</topic><topic>galaxies: evolution</topic></subject><relatedItem type="host"><titleInfo><title>Monthly Notices of the Royal Astronomical Society: Letters</title></titleInfo><genre type="journal" authority="ISTEX" authorityURI="https://publication-type.data.istex.fr" valueURI="https://publication-type.data.istex.fr/ark:/67375/JMC-0GLKJH51-B">journal</genre><identifier type="ISSN">1745-3925</identifier><identifier type="eISSN">1745-3933</identifier><identifier type="DOI">10.1111/(ISSN)1745-3933</identifier><identifier type="PublisherID">MNL2</identifier><part><date>2009</date><detail type="volume"><caption>vol.</caption><number>396</number></detail><detail type="issue"><caption>no.</caption><number>1</number></detail><extent unit="pages"><start>L56</start><end>L60</end><total>5</total></extent></part></relatedItem><identifier type="istex">82AE59B01C78B85B04D93F8211A22EF8A6F6FDF2</identifier><identifier type="ark">ark:/67375/WNG-JP2P17X9-Z</identifier><identifier type="DOI">10.1111/j.1745-3933.2009.00661.x</identifier><identifier type="ArticleID">MNL20661</identifier><accessCondition type="use and reproduction" contentType="copyright">© 2009 The Authors. 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