Glitches in southern pulsars
Identifieur interne : 002968 ( Istex/Corpus ); précédent : 002967; suivant : 002969Glitches in southern pulsars
Auteurs : N. Wang ; R. N. Manchester ; R. T. Pace ; M. Bailes ; V. M. Kaspi ; B. W. Stappers ; A. G. LyneSource :
- Monthly Notices of the Royal Astronomical Society [ 0035-8711 ] ; 2000-10.
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- KwdEn :
Abstract
Timing observations of 40 mostly young pulsars using the ATNF Parkes radio telescope between 1990 January and 1998 December are reported. In total, 20 previously unreported glitches and 10 other glitches were detected in 11 pulsars. These included 12 glitches in PSR J1341−6220, corresponding to a glitch rate of 1.5 glitches per year. We also detected the largest known glitch, in PSR J1614−5047, with Δνgν≈6.5×10−6, where ν=1/P is the pulse frequency. Glitch parameters were determined both by extrapolating timing solutions to interglitch intervals and by phase‐coherent timing fits across the glitch(es). These fits also give improved positions and dispersion measures for many of the pulsars. Analysis of glitch parameters, both from this work and from previously published results, shows that most glitches have a fractional amplitude Δνgν of between 10−8 and 10−6. There is no consistent relationship between glitch amplitude and the time since the previous glitch or the time to the following glitch, either for the ensemble or for individual pulsars. As previously recognized, the largest glitch activity is seen in pulsars with ages of order 104 yr, but for about 30 per cent of such pulsars, no glitches were detected in the 8‐year data span. There is some evidence for a new type of timing irregularity in which there is a significant increase in pulse frequency over a few days, accompanied by a decrease in the magnitude of the slow‐down rate. Fits of an exponential recovery to post‐glitch data show that for most older pulsars, only a small fraction of the glitch decays. In some younger pulsars a large fraction of the glitch decays, but in others there is very little decay. Apart from the Crab pulsar, there is no clear dependence of recovery time‐scale on pulsar age.
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DOI: 10.1046/j.1365-8711.2000.03713.x
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Wang</name><affiliation><mods:affiliation>Urumqi Astronomical Observatory, CAS, 40 South Beijing Road, Urumqi 830011, China</mods:affiliation></affiliation><affiliation><mods:affiliation>Australia Telescope National Facility, CSIRO, PO Box 76, Epping, NSW 1710, Australia</mods:affiliation></affiliation><affiliation><mods:affiliation>Geophysics Department, Peking University, Beijing 100871, China</mods:affiliation></affiliation><affiliation><mods:affiliation>E-mail: wangna@ms.xjb.ac.cn (NW); rmanches@atnf.csiro.au (RNM)</mods:affiliation></affiliation></author><author><name sortKey="Manchester, R N" sort="Manchester, R N" uniqKey="Manchester R" first="R. N." last="Manchester">R. N. 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In total, 20 previously unreported glitches and 10 other glitches were detected in 11 pulsars. These included 12 glitches in PSR J1341−6220, corresponding to a glitch rate of 1.5 glitches per year. We also detected the largest known glitch, in PSR J1614−5047, with Δνgν≈6.5×10−6, where ν=1/P is the pulse frequency. Glitch parameters were determined both by extrapolating timing solutions to interglitch intervals and by phase‐coherent timing fits across the glitch(es). These fits also give improved positions and dispersion measures for many of the pulsars. Analysis of glitch parameters, both from this work and from previously published results, shows that most glitches have a fractional amplitude Δνgν of between 10−8 and 10−6. There is no consistent relationship between glitch amplitude and the time since the previous glitch or the time to the following glitch, either for the ensemble or for individual pulsars. As previously recognized, the largest glitch activity is seen in pulsars with ages of order 104 yr, but for about 30 per cent of such pulsars, no glitches were detected in the 8‐year data span. There is some evidence for a new type of timing irregularity in which there is a significant increase in pulse frequency over a few days, accompanied by a decrease in the magnitude of the slow‐down rate. Fits of an exponential recovery to post‐glitch data show that for most older pulsars, only a small fraction of the glitch decays. In some younger pulsars a large fraction of the glitch decays, but in others there is very little decay. Apart from the Crab pulsar, there is no clear dependence of recovery time‐scale on pulsar age.</div></front></TEI><istex><corpusName>wiley</corpusName><author><json:item><name>N. Wang</name><affiliations><json:string>Urumqi Astronomical Observatory, CAS, 40 South Beijing Road, Urumqi 830011, China</json:string><json:string>Australia Telescope National Facility, CSIRO, PO Box 76, Epping, NSW 1710, Australia</json:string><json:string>Geophysics Department, Peking University, Beijing 100871, China</json:string><json:string>E-mail: wangna@ms.xjb.ac.cn (NW); rmanches@atnf.csiro.au (RNM)</json:string></affiliations></json:item><json:item><name>R. N. Manchester</name><affiliations><json:string>Australia Telescope National Facility, CSIRO, PO Box 76, Epping, NSW 1710, Australia</json:string><json:string>E-mail: wangna@ms.xjb.ac.cn (NW); rmanches@atnf.csiro.au (RNM)</json:string></affiliations></json:item><json:item><name>R. T. 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Stappers</name><affiliations><json:string>Mt Stromlo Observatory, ANU, Private Bag, Weston Creek, ACT 2611, Australia</json:string><json:string>E-mail: wangna@ms.xjb.ac.cn (NW); rmanches@atnf.csiro.au (RNM)</json:string></affiliations></json:item><json:item><name>A. G. Lyne</name><affiliations><json:string>University of Manchester, Jodrell Bank Observatory, Macclesfield, Cheshire SK11 9DL</json:string></affiliations></json:item></author><subject><json:item><lang><json:string>eng</json:string></lang><value>stars: neutron</value></json:item><json:item><lang><json:string>eng</json:string></lang><value>pulsars: general</value></json:item></subject><articleId><json:string>MNR3713</json:string></articleId><language><json:string>eng</json:string></language><originalGenre><json:string>article</json:string></originalGenre><abstract>Timing observations of 40 mostly young pulsars using the ATNF Parkes radio telescope between 1990 January and 1998 December are reported. In total, 20 previously unreported glitches and 10 other glitches were detected in 11 pulsars. These included 12 glitches in PSR J1341−6220, corresponding to a glitch rate of 1.5 glitches per year. We also detected the largest known glitch, in PSR J1614−5047, with Δνgν≈6.5×10−6, where ν=1/P is the pulse frequency. Glitch parameters were determined both by extrapolating timing solutions to interglitch intervals and by phase‐coherent timing fits across the glitch(es). These fits also give improved positions and dispersion measures for many of the pulsars. Analysis of glitch parameters, both from this work and from previously published results, shows that most glitches have a fractional amplitude Δνgν of between 10−8 and 10−6. There is no consistent relationship between glitch amplitude and the time since the previous glitch or the time to the following glitch, either for the ensemble or for individual pulsars. As previously recognized, the largest glitch activity is seen in pulsars with ages of order 104 yr, but for about 30 per cent of such pulsars, no glitches were detected in the 8‐year data span. There is some evidence for a new type of timing irregularity in which there is a significant increase in pulse frequency over a few days, accompanied by a decrease in the magnitude of the slow‐down rate. Fits of an exponential recovery to post‐glitch data show that for most older pulsars, only a small fraction of the glitch decays. In some younger pulsars a large fraction of the glitch decays, but in others there is very little decay. 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N.</forename><surname>Manchester</surname></persName><email>wangna@ms.xjb.ac.cn (NW); rmanches@atnf.csiro.au (RNM)</email><affiliation>Australia Telescope National Facility, CSIRO, PO Box 76, Epping, NSW 1710, Australia</affiliation></author><author xml:id="author-3"><persName><forename type="first">R. T.</forename><surname>Pace</surname></persName><email>wangna@ms.xjb.ac.cn (NW); rmanches@atnf.csiro.au (RNM)</email><affiliation>Australia Telescope National Facility, CSIRO, PO Box 76, Epping, NSW 1710, Australia</affiliation></author><author xml:id="author-4"><persName><forename type="first">M.</forename><surname>Bailes</surname></persName><affiliation>Astrophysics and Supercomputing, Swinburne University of Technolgy, PO Box 218, Hawthorn, Victoria 3122, Australia</affiliation></author><author xml:id="author-5"><persName><forename type="first">V. M.</forename><surname>Kaspi</surname></persName><affiliation>MIT, Center for Space Research 37‐621, 70 Vassar Street, Cambridge, MA 02139, USA</affiliation><affiliation>McGill University, Physics Department, 3600 University Street, Montreal, Quebec, Canada H3A 2T8</affiliation></author><author xml:id="author-6"><persName><forename type="first">B. W.</forename><surname>Stappers</surname></persName><email>wangna@ms.xjb.ac.cn (NW); rmanches@atnf.csiro.au (RNM)</email><affiliation>Mt Stromlo Observatory, ANU, Private Bag, Weston Creek, ACT 2611, Australia</affiliation></author><author xml:id="author-7"><persName><forename type="first">A. G.</forename><surname>Lyne</surname></persName><affiliation>University of Manchester, Jodrell Bank Observatory, Macclesfield, Cheshire SK11 9DL</affiliation></author></analytic><monogr><title level="j">Monthly Notices of the Royal Astronomical Society</title><idno type="pISSN">0035-8711</idno><idno type="eISSN">1365-2966</idno><idno type="DOI">10.1111/(ISSN)1365-2966</idno><imprint><publisher>Blackwell Science Ltd</publisher><pubPlace>Oxford, UK</pubPlace><date type="published" when="2000-10"></date><biblScope unit="volume">317</biblScope><biblScope unit="issue">4</biblScope><biblScope unit="page" from="843">843</biblScope><biblScope unit="page" to="860">860</biblScope></imprint></monogr><idno type="istex">D8F383739567E76D2EF5E25D19F2E075DBA35CA4</idno><idno type="DOI">10.1046/j.1365-8711.2000.03713.x</idno><idno type="ArticleID">MNR3713</idno></biblStruct></sourceDesc></fileDesc><profileDesc><creation><date>2000</date></creation><langUsage><language ident="en">en</language></langUsage><abstract xml:lang="en"><p>Timing observations of 40 mostly young pulsars using the ATNF Parkes radio telescope between 1990 January and 1998 December are reported. In total, 20 previously unreported glitches and 10 other glitches were detected in 11 pulsars. These included 12 glitches in PSR J1341−6220, corresponding to a glitch rate of 1.5 glitches per year. We also detected the largest known glitch, in PSR J1614−5047, with Δνgν≈6.5×10−6, where ν=1/P is the pulse frequency. Glitch parameters were determined both by extrapolating timing solutions to interglitch intervals and by phase‐coherent timing fits across the glitch(es). These fits also give improved positions and dispersion measures for many of the pulsars. Analysis of glitch parameters, both from this work and from previously published results, shows that most glitches have a fractional amplitude Δνgν of between 10−8 and 10−6. There is no consistent relationship between glitch amplitude and the time since the previous glitch or the time to the following glitch, either for the ensemble or for individual pulsars. As previously recognized, the largest glitch activity is seen in pulsars with ages of order 104 yr, but for about 30 per cent of such pulsars, no glitches were detected in the 8‐year data span. There is some evidence for a new type of timing irregularity in which there is a significant increase in pulse frequency over a few days, accompanied by a decrease in the magnitude of the slow‐down rate. Fits of an exponential recovery to post‐glitch data show that for most older pulsars, only a small fraction of the glitch decays. In some younger pulsars a large fraction of the glitch decays, but in others there is very little decay. Apart from the Crab pulsar, there is no clear dependence of recovery time‐scale on pulsar age.</p></abstract><textClass xml:lang="en"><keywords scheme="keyword"><list><head>keywords</head><item><term>stars: neutron</term></item><item><term>pulsars: general</term></item></list></keywords></textClass></profileDesc><revisionDesc><change when="2000-10">Published</change></revisionDesc></teiHeader></istex:fulltextTEI><json:item><extension>txt</extension><original>false</original><mimetype>text/plain</mimetype><uri>https://api-v5.istex.fr/document/D8F383739567E76D2EF5E25D19F2E075DBA35CA4/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 Science Ltd</publisherName><publisherLoc>Oxford, UK</publisherLoc></publisherInfo><doi origin="wiley" registered="yes">10.1111/(ISSN)1365-2966</doi><issn type="print">0035-8711</issn><issn type="electronic">1365-2966</issn><idGroup><id type="product" value="MNR"></id><id type="publisherDivision" value="ST"></id></idGroup><titleGroup><title type="main" sort="MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY">Monthly Notices of the Royal Astronomical Society</title></titleGroup></publicationMeta><publicationMeta level="part" position="10004"><doi origin="wiley">10.1111/mnr.2000.317.issue-4</doi><numberingGroup><numbering type="journalVolume" number="317">317</numbering><numbering type="journalIssue" number="4">4</numbering></numberingGroup><coverDate startDate="2000-10">October 2000</coverDate></publicationMeta><publicationMeta level="unit" type="article" position="0084300" status="forIssue"><doi origin="wiley">10.1046/j.1365-8711.2000.03713.x</doi><idGroup><id type="unit" value="MNR3713"></id><id type="supplier" value="mn3090"></id></idGroup><countGroup><count type="pageTotal" number="18"></count></countGroup><titleGroup><title type="tocHeading1">Papers</title></titleGroup><eventGroup><event type="firstOnline" date="2002-04-04"></event><event type="publishedOnlineFinalForm" date="2002-04-04"></event><event type="xmlConverted" agent="Converter:BPG_TO_WML3G version:2.3.2 mode:FullText source:FullText result:FullText" date="2010-02-26"></event><event type="xmlConverted" agent="Converter:WILEY_ML3G_TO_WILEY_ML3GV2 version:3.8.8" date="2014-02-02"></event><event type="xmlConverted" agent="Converter:WML3G_To_WML3G version:4.1.7 mode:FullText,remove_FC" date="2014-10-31"></event></eventGroup><numberingGroup><numbering type="pageFirst" number="843">843</numbering><numbering type="pageLast" number="860">860</numbering></numberingGroup><correspondenceTo>★ E‐mail: <email>wangna@ms.xjb.ac.cn (NW); rmanches@atnf.csiro.au (RNM)</email>† Present address: Department of Physics and Mathematical Physics, University of Adelaide, Adelaide SA 5005, Australia.‡ Present address: Astronomical Institute, University of Amsterdam, Kruislaan 403, 1098 SJ Amsterdam, The Netherlands.</correspondenceTo><linkGroup><link type="toTypesetVersion" href="file:MNR.MNR3713.pdf"></link></linkGroup></publicationMeta><contentMeta><unparsedEditorialHistory>Accepted 2000 May 8. Received 2000 May 4; in original form 1999 December 2</unparsedEditorialHistory><countGroup><count type="figureTotal" number="0"></count><count type="tableTotal" number="5"></count><count type="formulaTotal" number="0"></count><count type="referenceTotal" number="64"></count><count type="wordTotal" number="42010"></count><count type="linksPubMed" number="0"></count><count type="linksCrossRef" number="0"></count></countGroup><titleGroup><title type="main">Glitches in southern pulsars</title><title type="shortAuthors">N. Wang et al.</title><title type="short">Glitches in southern pulsars</title></titleGroup><creators><creator creatorRole="author" xml:id="cr1" affiliationRef="#a1 #a2 #a3" corresponding="yes"><personName><givenNames>N.</givenNames><familyName>Wang</familyName></personName></creator><creator creatorRole="author" xml:id="cr2" affiliationRef="#a2" corresponding="yes"><personName><givenNames>R. N.</givenNames><familyName>Manchester</familyName></personName></creator><creator creatorRole="author" xml:id="cr3" affiliationRef="#a2" corresponding="yes"><personName><givenNames>R. T.</givenNames><familyName>Pace</familyName></personName></creator><creator creatorRole="author" xml:id="cr4" affiliationRef="#a4"><personName><givenNames>M.</givenNames><familyName>Bailes</familyName></personName></creator><creator creatorRole="author" xml:id="cr5" affiliationRef="#a5 #a6"><personName><givenNames>V. M.</givenNames><familyName>Kaspi</familyName></personName></creator><creator creatorRole="author" xml:id="cr6" affiliationRef="#a7" corresponding="yes"><personName><givenNames>B. W.</givenNames><familyName>Stappers</familyName></personName></creator><creator creatorRole="author" xml:id="cr7" affiliationRef="#a8"><personName><givenNames>A. G.</givenNames><familyName>Lyne</familyName></personName></creator></creators><affiliationGroup><affiliation xml:id="a1" countryCode="CN"><unparsedAffiliation>Urumqi Astronomical Observatory, CAS, 40 South Beijing Road, Urumqi 830011, China</unparsedAffiliation></affiliation><affiliation xml:id="a2" countryCode="AU"><unparsedAffiliation>Australia Telescope National Facility, CSIRO, PO Box 76, Epping, NSW 1710, Australia</unparsedAffiliation></affiliation><affiliation xml:id="a3" countryCode="CN"><unparsedAffiliation>Geophysics Department, Peking University, Beijing 100871, China</unparsedAffiliation></affiliation><affiliation xml:id="a4" countryCode="AU"><unparsedAffiliation>Astrophysics and Supercomputing, Swinburne University of Technolgy, PO Box 218, Hawthorn, Victoria 3122, Australia</unparsedAffiliation></affiliation><affiliation xml:id="a5" countryCode="US"><unparsedAffiliation>MIT, Center for Space Research 37‐621, 70 Vassar Street, Cambridge, MA 02139, USA</unparsedAffiliation></affiliation><affiliation xml:id="a6" countryCode="CA"><unparsedAffiliation>McGill University, Physics Department, 3600 University Street, Montreal, Quebec, Canada H3A 2T8</unparsedAffiliation></affiliation><affiliation xml:id="a7" countryCode="AU"><unparsedAffiliation>Mt Stromlo Observatory, ANU, Private Bag, Weston Creek, ACT 2611, Australia</unparsedAffiliation></affiliation><affiliation xml:id="a8"><unparsedAffiliation>University of Manchester, Jodrell Bank Observatory, Macclesfield, Cheshire SK11 9DL</unparsedAffiliation></affiliation></affiliationGroup><keywordGroup xml:lang="en"><keyword xml:id="k1">stars: neutron</keyword><keyword xml:id="k2">pulsars: general</keyword></keywordGroup><abstractGroup><abstract type="main" xml:lang="en"><p>Timing observations of 40 mostly young pulsars using the ATNF Parkes radio telescope between 1990 January and 1998 December are reported. In total, 20 previously unreported glitches and 10 other glitches were detected in 11 pulsars. These included 12 glitches in PSR J1341−6220, corresponding to a glitch rate of 1.5 glitches per year. We also detected the largest known glitch, in PSR J1614−5047, with Δ<i>ν</i><sub>g</sub><i>ν</i>≈6.5×10<sup>−6</sup>, where <i>ν</i>=1/<i>P</i> is the pulse frequency. Glitch parameters were determined both by extrapolating timing solutions to interglitch intervals and by phase‐coherent timing fits across the glitch(es). These fits also give improved positions and dispersion measures for many of the pulsars. Analysis of glitch parameters, both from this work and from previously published results, shows that most glitches have a fractional amplitude Δ<i>ν</i><sub>g</sub><i>ν</i> of between 10<sup>−8</sup> and 10<sup>−6</sup>. There is no consistent relationship between glitch amplitude and the time since the previous glitch or the time to the following glitch, either for the ensemble or for individual pulsars. As previously recognized, the largest glitch activity is seen in pulsars with ages of order 10<sup>4</sup> yr, but for about 30 per cent of such pulsars, no glitches were detected in the 8‐year data span. There is some evidence for a new type of timing irregularity in which there is a significant increase in pulse frequency over a few days, accompanied by a decrease in the magnitude of the slow‐down rate. Fits of an exponential recovery to post‐glitch data show that for most older pulsars, only a small fraction of the glitch decays. In some younger pulsars a large fraction of the glitch decays, but in others there is very little decay. Apart from the Crab pulsar, there is no clear dependence of recovery time‐scale on pulsar age.</p></abstract></abstractGroup></contentMeta></header></component></istex:document></istex:metadataXml><mods version="3.6"><titleInfo lang="en"><title>Glitches in southern pulsars</title></titleInfo><titleInfo type="abbreviated" lang="en"><title>Glitches in southern pulsars</title></titleInfo><titleInfo type="alternative" contentType="CDATA" lang="en"><title>Glitches in southern pulsars</title></titleInfo><name type="personal"><namePart type="given">N.</namePart><namePart type="family">Wang</namePart><affiliation>Urumqi Astronomical Observatory, CAS, 40 South Beijing Road, Urumqi 830011, China</affiliation><affiliation>Australia Telescope National Facility, CSIRO, PO Box 76, Epping, NSW 1710, Australia</affiliation><affiliation>Geophysics Department, Peking University, Beijing 100871, China</affiliation><affiliation>E-mail: wangna@ms.xjb.ac.cn (NW); rmanches@atnf.csiro.au (RNM)</affiliation><role><roleTerm type="text">author</roleTerm></role></name><name type="personal"><namePart type="given">R. N.</namePart><namePart type="family">Manchester</namePart><affiliation>Australia Telescope National Facility, CSIRO, PO Box 76, Epping, NSW 1710, Australia</affiliation><affiliation>E-mail: wangna@ms.xjb.ac.cn (NW); rmanches@atnf.csiro.au (RNM)</affiliation><role><roleTerm type="text">author</roleTerm></role></name><name type="personal"><namePart type="given">R. T.</namePart><namePart type="family">Pace</namePart><affiliation>Australia Telescope National Facility, CSIRO, PO Box 76, Epping, NSW 1710, Australia</affiliation><affiliation>E-mail: wangna@ms.xjb.ac.cn (NW); rmanches@atnf.csiro.au (RNM)</affiliation><role><roleTerm type="text">author</roleTerm></role></name><name type="personal"><namePart type="given">M.</namePart><namePart type="family">Bailes</namePart><affiliation>Astrophysics and Supercomputing, Swinburne University of Technolgy, PO Box 218, Hawthorn, Victoria 3122, Australia</affiliation><role><roleTerm type="text">author</roleTerm></role></name><name type="personal"><namePart type="given">V. M.</namePart><namePart type="family">Kaspi</namePart><affiliation>MIT, Center for Space Research 37‐621, 70 Vassar Street, Cambridge, MA 02139, USA</affiliation><affiliation>McGill University, Physics Department, 3600 University Street, Montreal, Quebec, Canada H3A 2T8</affiliation><role><roleTerm type="text">author</roleTerm></role></name><name type="personal"><namePart type="given">B. W.</namePart><namePart type="family">Stappers</namePart><affiliation>Mt Stromlo Observatory, ANU, Private Bag, Weston Creek, ACT 2611, Australia</affiliation><affiliation>E-mail: wangna@ms.xjb.ac.cn (NW); rmanches@atnf.csiro.au (RNM)</affiliation><role><roleTerm type="text">author</roleTerm></role></name><name type="personal"><namePart type="given">A. G.</namePart><namePart type="family">Lyne</namePart><affiliation>University of Manchester, Jodrell Bank Observatory, Macclesfield, Cheshire SK11 9DL</affiliation><role><roleTerm type="text">author</roleTerm></role></name><typeOfResource>text</typeOfResource><genre type="article" displayLabel="article"></genre><originInfo><publisher>Blackwell Science Ltd</publisher><place><placeTerm type="text">Oxford, UK</placeTerm></place><dateIssued encoding="w3cdtf">2000-10</dateIssued><edition>Accepted 2000 May 8. Received 2000 May 4; in original form 1999 December 2</edition><copyrightDate encoding="w3cdtf">2000</copyrightDate></originInfo><language><languageTerm type="code" authority="rfc3066">en</languageTerm><languageTerm type="code" authority="iso639-2b">eng</languageTerm></language><physicalDescription><internetMediaType>text/html</internetMediaType><extent unit="tables">5</extent><extent unit="references">64</extent><extent unit="words">42010</extent></physicalDescription><abstract lang="en">Timing observations of 40 mostly young pulsars using the ATNF Parkes radio telescope between 1990 January and 1998 December are reported. In total, 20 previously unreported glitches and 10 other glitches were detected in 11 pulsars. These included 12 glitches in PSR J1341−6220, corresponding to a glitch rate of 1.5 glitches per year. We also detected the largest known glitch, in PSR J1614−5047, with Δνgν≈6.5×10−6, where ν=1/P is the pulse frequency. Glitch parameters were determined both by extrapolating timing solutions to interglitch intervals and by phase‐coherent timing fits across the glitch(es). These fits also give improved positions and dispersion measures for many of the pulsars. Analysis of glitch parameters, both from this work and from previously published results, shows that most glitches have a fractional amplitude Δνgν of between 10−8 and 10−6. There is no consistent relationship between glitch amplitude and the time since the previous glitch or the time to the following glitch, either for the ensemble or for individual pulsars. As previously recognized, the largest glitch activity is seen in pulsars with ages of order 104 yr, but for about 30 per cent of such pulsars, no glitches were detected in the 8‐year data span. There is some evidence for a new type of timing irregularity in which there is a significant increase in pulse frequency over a few days, accompanied by a decrease in the magnitude of the slow‐down rate. Fits of an exponential recovery to post‐glitch data show that for most older pulsars, only a small fraction of the glitch decays. In some younger pulsars a large fraction of the glitch decays, but in others there is very little decay. Apart from the Crab pulsar, there is no clear dependence of recovery time‐scale on pulsar age.</abstract><subject lang="en"><genre>keywords</genre><topic>stars: neutron</topic><topic>pulsars: general</topic></subject><relatedItem type="host"><titleInfo><title>Monthly Notices of the Royal Astronomical Society</title></titleInfo><genre type="journal">journal</genre><identifier type="ISSN">0035-8711</identifier><identifier type="eISSN">1365-2966</identifier><identifier type="DOI">10.1111/(ISSN)1365-2966</identifier><identifier type="PublisherID">MNR</identifier><part><date>2000</date><detail type="volume"><caption>vol.</caption><number>317</number></detail><detail type="issue"><caption>no.</caption><number>4</number></detail><extent unit="pages"><start>843</start><end>860</end><total>18</total></extent></part></relatedItem><identifier type="istex">D8F383739567E76D2EF5E25D19F2E075DBA35CA4</identifier><identifier type="DOI">10.1046/j.1365-8711.2000.03713.x</identifier><identifier type="ArticleID">MNR3713</identifier><recordInfo><recordContentSource>WILEY</recordContentSource><recordOrigin>Blackwell Science Ltd</recordOrigin></recordInfo></mods></metadata><serie></serie></istex></record>Pour manipuler ce document sous Unix (Dilib)
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