An empirical model for the beams of radio pulsars
Identifieur interne : 001416 ( Istex/Corpus ); précédent : 001415; suivant : 001417An empirical model for the beams of radio pulsars
Auteurs : Aris Karastergiou ; Simon JohnstonSource :
- Monthly Notices of the Royal Astronomical Society [ 0035-8711 ] ; 2007-10.
English descriptors
- KwdEn :
- Abrupt change, Abrupt transition, Active heights, Active patches, Average pulse, Beam model, Discrete heights, Double component, Emission cone, Emission height, Emission heights, Emission patches, Empirical model, Energetic pulsars, Entire range, Free parameters, Height range, High altitudes, High frequencies, Johnston weisberg, Journal compilation, Karastergiou, Karastergiou johnston, Large diversity, Large fraction, Large number, Light cylinder, Light cylinder radius, Lower altitudes, Lyne manchester, Magnetic axis, Magnetic pole, Magnetosphere, Maximum altitude, Maximum emission height, Maximum height, Minimum height, Mitra, Mitra rankin, Mnras, Natural explanation, Numerical simulations, Observational data, Older pulsars, Other hand, Parameter space, Parkes radio telescope, Particular frequency, Patchy, Pulsar, Pulsar beam, Pulsar beams, Pulsar period, Pulse longitude, Pulse period, Pulse width, Radio emission, Radio pulsars, Random locations, Real data, Same time, Simple beam model, Simulation, Single component, Slower pulsars, Small number, Stellar surface, Temporal resolution, Total number, Transition point, Visual inspection, Wide range, Young pulsars.
- Teeft :
- Abrupt change, Abrupt transition, Active heights, Active patches, Average pulse, Beam model, Discrete heights, Double component, Emission cone, Emission height, Emission heights, Emission patches, Empirical model, Energetic pulsars, Entire range, Free parameters, Height range, High altitudes, High frequencies, Johnston weisberg, Journal compilation, Karastergiou, Karastergiou johnston, Large diversity, Large fraction, Large number, Light cylinder, Light cylinder radius, Lower altitudes, Lyne manchester, Magnetic axis, Magnetic pole, Magnetosphere, Maximum altitude, Maximum emission height, Maximum height, Minimum height, Mitra, Mitra rankin, Mnras, Natural explanation, Numerical simulations, Observational data, Older pulsars, Other hand, Parameter space, Parkes radio telescope, Particular frequency, Patchy, Pulsar, Pulsar beam, Pulsar beams, Pulsar period, Pulse longitude, Pulse period, Pulse width, Radio emission, Radio pulsars, Random locations, Real data, Same time, Simple beam model, Simulation, Single component, Slower pulsars, Small number, Stellar surface, Temporal resolution, Total number, Transition point, Visual inspection, Wide range, Young pulsars.
Abstract
Motivated by recent results on the location of the radio emission in pulsar magnetospheres, we have developed a model which can account for the large diversity found in the average profile shapes of pulsars. At the centre of our model lies the idea that radio emission at a particular frequency arises from a wide range of altitudes above the surface of the star, and that it is confined to a region close to the last open field lines. We assert that the radial height range over which emission occurs is responsible for the complex average pulse shapes rather than the transverse (longitudinal) range proposed in most current models. By implementing an abrupt change in the height range to discriminate between young, short‐period, highly energetic pulsars and their older counterparts, we obtain the observed transition between the simple and complex average pulse profiles observed in each group respectively. Monte Carlo simulations are used to demonstrate the match of our model to real observations.
Url:
DOI: 10.1111/j.1365-2966.2007.12237.x
Links to Exploration step
ISTEX:6BCB393470B5BD8D4BE70F3E79B06D945DFABC49Le document en format XML
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At the centre of our model lies the idea that radio emission at a particular frequency arises from a wide range of altitudes above the surface of the star, and that it is confined to a region close to the last open field lines. We assert that the radial height range over which emission occurs is responsible for the complex average pulse shapes rather than the transverse (longitudinal) range proposed in most current models. By implementing an abrupt change in the height range to discriminate between young, short‐period, highly energetic pulsars and their older counterparts, we obtain the observed transition between the simple and complex average pulse profiles observed in each group respectively. Monte Carlo simulations are used to demonstrate the match of our model to real observations.</abstract><qualityIndicators><score>8.944</score><pdfWordCount>5279</pdfWordCount><pdfCharCount>29293</pdfCharCount><pdfVersion>1.4</pdfVersion><pdfPageCount>7</pdfPageCount><pdfPageSize>612 x 792 pts (letter)</pdfPageSize><refBibsNative>true</refBibsNative><abstractWordCount>162</abstractWordCount><abstractCharCount>1005</abstractCharCount><keywordCount>1</keywordCount></qualityIndicators><title>An empirical model for the beams of radio pulsars</title><genre><json:string>article</json:string></genre><host><title>Monthly Notices of the Royal Astronomical Society</title><language><json:string>unknown</json:string></language><doi><json:string>10.1111/(ISSN)1365-2966</json:string></doi><issn><json:string>0035-8711</json:string></issn><eissn><json:string>1365-2966</json:string></eissn><publisherId><json:string>MNR</json:string></publisherId><volume>380</volume><issue>4</issue><pages><first>1678</first><last>1684</last><total>7</total></pages><genre><json:string>journal</json:string></genre></host><namedEntities><unitex><date><json:string>1000</json:string><json:string>2007</json:string></date><geogName></geogName><orgName><json:string>University of Sydney</json:string><json:string>Australia Accepted</json:string><json:string>National Facility</json:string><json:string>Australia Telescope</json:string></orgName><orgName_funder></orgName_funder><orgName_provider></orgName_provider><persName><json:string>Michael Kramer</json:string><json:string>A. Karastergiou</json:string><json:string>Steve Ord</json:string><json:string>Marie Curie</json:string><json:string>Rankin</json:string><json:string>Simon Johnston</json:string><json:string>Don Melrose</json:string><json:string>Aris Karastergiou</json:string><json:string>S. Johnston</json:string></persName><placeName><json:string>Australia</json:string><json:string>Manchester</json:string></placeName><ref_url></ref_url><ref_bibl><json:string>Han & Manchester 2001</json:string><json:string>Rankin (2002)</json:string><json:string>Karastergiou, Johnston & Manchester 2005</json:string><json:string>Blaskiewicz, Cordes & Wasserman 1991</json:string><json:string>Rankin 1983, 1993</json:string><json:string>Tauris & Manchester 1998</json:string><json:string>Rankin 1993</json:string><json:string>Backer 1973</json:string><json:string>Wu et al. 1998</json:string><json:string>Mitra & Li 2004</json:string><json:string>Kramer et al. 1994</json:string><json:string>Karastergiou & Johnston 2006</json:string><json:string>Weisberg (2006)</json:string><json:string>Rankin (1993)</json:string><json:string>Mitra & Rankin 2002</json:string><json:string>Gupta (2001)</json:string><json:string>Johnston, Karastergiou & Willett 2006</json:string><json:string>Kramer et al. 2006</json:string><json:string>Ruderman & Sutherland 1975</json:string></ref_bibl><bibl></bibl></unitex></namedEntities><ark><json:string>ark:/67375/WNG-383WVPNJ-L</json:string></ark><categories><wos><json:string>1 - 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At the centre of our model lies the idea that radio emission at a particular frequency arises from a wide range of altitudes above the surface of the star, and that it is confined to a region close to the last open field lines. We assert that the radial height range over which emission occurs is responsible for the complex average pulse shapes rather than the transverse (longitudinal) range proposed in most current models. By implementing an abrupt change in the height range to discriminate between young, short‐period, highly energetic pulsars and their older counterparts, we obtain the observed transition between the simple and complex average pulse profiles observed in each group respectively. 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E‐mail: <email>aris.karastergiou@gmail.com</email></correspondenceTo><linkGroup><link type="toTypesetVersion" href="file:MNR.MNR12237.pdf"></link></linkGroup></publicationMeta><contentMeta><unparsedEditorialHistory>Accepted 2007 July 16. Received 2007 July 6; in original form 2007 March 26</unparsedEditorialHistory><countGroup><count type="figureTotal" number="5"></count><count type="tableTotal" number="2"></count><count type="formulaTotal" number="15"></count><count type="referenceTotal" number="26"></count><count type="linksCrossRef" number="65"></count></countGroup><titleGroup><title type="main">An empirical model for the beams of radio pulsars</title><title type="shortAuthors"><i>A. Karastergiou and S. Johnston</i></title><title type="short"><i>An empirical model for pulsar beams</i></title></titleGroup><creators><creator creatorRole="author" xml:id="cr1" affiliationRef="#a1" corresponding="yes"><personName><givenNames>Aris</givenNames><familyName>Karastergiou</familyName></personName></creator><creator creatorRole="author" xml:id="cr2" affiliationRef="#a2"><personName><givenNames>Simon</givenNames><familyName>Johnston</familyName></personName></creator></creators><affiliationGroup><affiliation xml:id="a1" countryCode="US"><unparsedAffiliation>IRAM, 300 rue de la Piscine, Domaine Universitaire, Saint Martin d'Heres, France</unparsedAffiliation></affiliation><affiliation xml:id="a2" countryCode="AU"><unparsedAffiliation>Australia Telescope National Facility, CSIRO, PO Box 76, Epping, NSW 1710, Australia</unparsedAffiliation></affiliation></affiliationGroup><keywordGroup xml:lang="en"><keyword xml:id="k1">pulsars: general</keyword></keywordGroup><abstractGroup><abstract type="main" xml:lang="en"><title type="main">ABSTRACT</title><p>Motivated by recent results on the location of the radio emission in pulsar magnetospheres, we have developed a model which can account for the large diversity found in the average profile shapes of pulsars. At the centre of our model lies the idea that radio emission at a particular frequency arises from a wide range of altitudes above the surface of the star, and that it is confined to a region close to the last open field lines. We assert that the radial height range over which emission occurs is responsible for the complex average pulse shapes rather than the transverse (longitudinal) range proposed in most current models. By implementing an abrupt change in the height range to discriminate between young, short‐period, highly energetic pulsars and their older counterparts, we obtain the observed transition between the simple and complex average pulse profiles observed in each group respectively. Monte Carlo simulations are used to demonstrate the match of our model to real observations.</p></abstract></abstractGroup></contentMeta></header></component></istex:document></istex:metadataXml><mods version="3.6"><titleInfo lang="en"><title>An empirical model for the beams of radio pulsars</title></titleInfo><titleInfo type="abbreviated" lang="en"><title>An empirical model for pulsar beams</title></titleInfo><titleInfo type="alternative" contentType="CDATA" lang="en"><title>An empirical model for the beams of radio pulsars</title></titleInfo><name type="personal"><namePart type="given">Aris</namePart><namePart type="family">Karastergiou</namePart><affiliation>IRAM, 300 rue de la Piscine, Domaine Universitaire, Saint Martin d'Heres, France</affiliation><affiliation>E-mail: aris.karastergiou@gmail.com</affiliation><role><roleTerm type="text">author</roleTerm></role></name><name type="personal"><namePart type="given">Simon</namePart><namePart type="family">Johnston</namePart><affiliation>Australia Telescope National Facility, CSIRO, PO Box 76, Epping, NSW 1710, Australia</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">2007-10</dateIssued><edition>Accepted 2007 July 16. Received 2007 July 6; in original form 2007 March 26</edition><copyrightDate encoding="w3cdtf">2007</copyrightDate></originInfo><language><languageTerm type="code" authority="rfc3066">en</languageTerm><languageTerm type="code" authority="iso639-2b">eng</languageTerm></language><physicalDescription><extent unit="figures">5</extent><extent unit="tables">2</extent><extent unit="formulas">15</extent><extent unit="references">26</extent><extent unit="linksCrossRef">65</extent></physicalDescription><abstract lang="en">Motivated by recent results on the location of the radio emission in pulsar magnetospheres, we have developed a model which can account for the large diversity found in the average profile shapes of pulsars. At the centre of our model lies the idea that radio emission at a particular frequency arises from a wide range of altitudes above the surface of the star, and that it is confined to a region close to the last open field lines. We assert that the radial height range over which emission occurs is responsible for the complex average pulse shapes rather than the transverse (longitudinal) range proposed in most current models. By implementing an abrupt change in the height range to discriminate between young, short‐period, highly energetic pulsars and their older counterparts, we obtain the observed transition between the simple and complex average pulse profiles observed in each group respectively. Monte Carlo simulations are used to demonstrate the match of our model to real observations.</abstract><subject lang="en"><genre>keywords</genre><topic>pulsars: general</topic></subject><relatedItem type="host"><titleInfo><title>Monthly Notices of the Royal Astronomical Society</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">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>2007</date><detail type="volume"><caption>vol.</caption><number>380</number></detail><detail type="issue"><caption>no.</caption><number>4</number></detail><extent unit="pages"><start>1678</start><end>1684</end><total>7</total></extent></part></relatedItem><identifier type="istex">6BCB393470B5BD8D4BE70F3E79B06D945DFABC49</identifier><identifier type="ark">ark:/67375/WNG-383WVPNJ-L</identifier><identifier type="DOI">10.1111/j.1365-2966.2007.12237.x</identifier><identifier type="ArticleID">MNR12237</identifier><recordInfo><recordContentSource authority="ISTEX" authorityURI="https://loaded-corpus.data.istex.fr" valueURI="https://loaded-corpus.data.istex.fr/ark:/67375/XBH-L0C46X92-X">wiley</recordContentSource><recordOrigin>Blackwell Publishing Ltd</recordOrigin></recordInfo></mods><json:item><extension>json</extension><original>false</original><mimetype>application/json</mimetype><uri>https://api.istex.fr/document/6BCB393470B5BD8D4BE70F3E79B06D945DFABC49/metadata/json</uri></json:item></metadata><serie></serie></istex></record>Pour manipuler ce document sous Unix (Dilib)
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