An empirical model for the beams of radio pulsars
Identifieur interne : 009209 ( Main/Exploration ); précédent : 009208; suivant : 009210An empirical model for the beams of radio pulsars
Auteurs : Aris Karastergiou [France] ; Simon Johnston [Australie]Source :
- Monthly Notices of the Royal Astronomical Society [ 0035-8711 ] ; 2007-10.
Descripteurs français
- Pascal (Inist)
- Wicri :
- topic : Simulation.
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, Energetics, Entire range, Field line, 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, Monte Carlo methods, 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 shape, Pulse width, Radio emission, Radio pulsars, Radiopulsar, Random locations, Real data, Same time, Simple beam model, Simulation, Single component, Slower pulsars, Small number, Stellar magnetospheres, Stellar surface, Sudden variation, 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:
- https://api.istex.fr/document/6BCB393470B5BD8D4BE70F3E79B06D945DFABC49/fulltext/pdf
- https://api.istex.fr/document/8331189EC2366BA8D6F37D3F249085A6F0547DFB/fulltext/pdf
DOI: 10.1111/j.1365-2966.2007.12237.x
Affiliations:
Links toward previous steps (curation, corpus...)
- to stream Istex, to step Corpus: 001416
- to stream Istex, to step Curation: 001416
- to stream Istex, to step Checkpoint: 001458
- to stream Istex, to step Corpus: 001881
- to stream Istex, to step Curation: 001881
- to stream Istex, to step Checkpoint: 001311
- to stream Main, to step Merge: 009B82
- to stream PascalFrancis, to step Corpus: 003957
- to stream PascalFrancis, to step Curation: 002731
- to stream PascalFrancis, to step Checkpoint: 003A72
- to stream Main, to step Merge: 00A184
- to stream Main, to step Curation: 009209
Le document en format XML
<record><TEI wicri:istexFullTextTei="biblStruct"><teiHeader><fileDesc><titleStmt><title xml:lang="en">An empirical model for the beams of radio pulsars</title><author><name sortKey="Karastergiou, Aris" sort="Karastergiou, Aris" uniqKey="Karastergiou A" first="Aris" last="Karastergiou">Aris Karastergiou</name></author><author><name sortKey="Johnston, Simon" sort="Johnston, Simon" uniqKey="Johnston S" first="Simon" last="Johnston">Simon Johnston</name></author></titleStmt><publicationStmt><idno type="wicri:source">ISTEX</idno><idno type="RBID">ISTEX:6BCB393470B5BD8D4BE70F3E79B06D945DFABC49</idno><date when="2007" year="2007">2007</date><idno type="doi">10.1111/j.1365-2966.2007.12237.x</idno><idno type="url">https://api.istex.fr/document/6BCB393470B5BD8D4BE70F3E79B06D945DFABC49/fulltext/pdf</idno><idno type="wicri:Area/Istex/Corpus">001416</idno><idno type="wicri:explorRef" wicri:stream="Istex" wicri:step="Corpus" wicri:corpus="ISTEX">001416</idno><idno type="wicri:Area/Istex/Curation">001416</idno><idno type="wicri:Area/Istex/Checkpoint">001458</idno><idno type="wicri:explorRef" wicri:stream="Istex" wicri:step="Checkpoint">001458</idno><idno type="wicri:doubleKey">0035-8711:2007:Karastergiou A:an:empirical:model</idno><idno type="wicri:source">ISTEX</idno><idno type="RBID">ISTEX:8331189EC2366BA8D6F37D3F249085A6F0547DFB</idno><idno type="url">https://api.istex.fr/document/8331189EC2366BA8D6F37D3F249085A6F0547DFB/fulltext/pdf</idno><idno type="wicri:Area/Istex/Corpus">001881</idno><idno type="wicri:explorRef" wicri:stream="Istex" wicri:step="Corpus" wicri:corpus="ISTEX">001881</idno><idno type="wicri:Area/Istex/Curation">001881</idno><idno type="wicri:Area/Istex/Checkpoint">001311</idno><idno type="wicri:explorRef" wicri:stream="Istex" wicri:step="Checkpoint">001311</idno><idno type="wicri:doubleKey">0035-8711:2007:Karastergiou A:an:empirical:model</idno><idno type="wicri:Area/Main/Merge">009B82</idno><idno type="wicri:source">INIST</idno><idno type="RBID">Pascal:07-0455437</idno><idno type="wicri:Area/PascalFrancis/Corpus">003957</idno><idno type="wicri:Area/PascalFrancis/Curation">002731</idno><idno type="wicri:Area/PascalFrancis/Checkpoint">003A72</idno><idno type="wicri:explorRef" wicri:stream="PascalFrancis" wicri:step="Checkpoint">003A72</idno><idno type="wicri:doubleKey">0035-8711:2007:Karastergiou A:an:empirical:model</idno><idno type="wicri:Area/Main/Merge">00A184</idno><idno type="wicri:Area/Main/Curation">009209</idno><idno type="wicri:Area/Main/Exploration">009209</idno></publicationStmt><sourceDesc><biblStruct><analytic><title level="a" type="main">An empirical model for the beams of radio pulsars</title><author><name sortKey="Karastergiou, Aris" sort="Karastergiou, Aris" uniqKey="Karastergiou A" first="Aris" last="Karastergiou">Aris Karastergiou</name><affiliation wicri:level="3"><country xml:lang="fr">France</country><wicri:regionArea>IRAM, 300 rue de la Piscine, Domaine Universitaire, Saint Martin d'Heres</wicri:regionArea><placeName><region type="region" nuts="2">Auvergne-Rhône-Alpes</region><region type="old region" nuts="2">Rhône-Alpes</region><settlement type="city">Saint-Martin-d'Hères</settlement><settlement type="city" wicri:auto="agglo">Grenoble</settlement></placeName></affiliation><affiliation></affiliation></author><author><name sortKey="Johnston, Simon" sort="Johnston, Simon" uniqKey="Johnston S" first="Simon" last="Johnston">Simon Johnston</name><affiliation wicri:level="1"><country xml:lang="fr">Australie</country><wicri:regionArea>Australia Telescope National Facility, CSIRO, PO Box 76, Epping, NSW 1710</wicri:regionArea><wicri:noRegion>NSW 1710</wicri:noRegion></affiliation></author></analytic><monogr></monogr><series><title level="j" type="main">Monthly Notices of the Royal Astronomical Society</title><title level="j" type="alt">MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY</title><idno type="ISSN">0035-8711</idno><idno type="eISSN">1365-2966</idno><imprint><biblScope unit="vol">380</biblScope><biblScope unit="issue">4</biblScope><biblScope unit="page" from="1678">1678</biblScope><biblScope unit="page" to="1684">1684</biblScope><biblScope unit="page-count">7</biblScope><publisher>Blackwell Publishing Ltd</publisher><pubPlace>Oxford, UK</pubPlace><date type="published" when="2007-10">2007-10</date></imprint><idno type="ISSN">0035-8711</idno></series></biblStruct></sourceDesc><seriesStmt><idno type="ISSN">0035-8711</idno></seriesStmt></fileDesc><profileDesc><textClass><keywords scheme="KwdEn" xml:lang="en"><term>Abrupt change</term><term>Abrupt transition</term><term>Active heights</term><term>Active patches</term><term>Average pulse</term><term>Beam model</term><term>Discrete heights</term><term>Double component</term><term>Emission cone</term><term>Emission height</term><term>Emission heights</term><term>Emission patches</term><term>Empirical model</term><term>Energetic pulsars</term><term>Energetics</term><term>Entire range</term><term>Field line</term><term>Free parameters</term><term>Height range</term><term>High altitudes</term><term>High frequencies</term><term>Johnston weisberg</term><term>Journal compilation</term><term>Karastergiou</term><term>Karastergiou johnston</term><term>Large diversity</term><term>Large fraction</term><term>Large number</term><term>Light cylinder</term><term>Light cylinder radius</term><term>Lower altitudes</term><term>Lyne manchester</term><term>Magnetic axis</term><term>Magnetic pole</term><term>Magnetosphere</term><term>Maximum altitude</term><term>Maximum emission height</term><term>Maximum height</term><term>Minimum height</term><term>Mitra</term><term>Mitra rankin</term><term>Mnras</term><term>Monte Carlo methods</term><term>Natural explanation</term><term>Numerical simulations</term><term>Observational data</term><term>Older pulsars</term><term>Other hand</term><term>Parameter space</term><term>Parkes radio telescope</term><term>Particular frequency</term><term>Patchy</term><term>Pulsar</term><term>Pulsar beam</term><term>Pulsar beams</term><term>Pulsar period</term><term>Pulse longitude</term><term>Pulse period</term><term>Pulse shape</term><term>Pulse width</term><term>Radio emission</term><term>Radio pulsars</term><term>Radiopulsar</term><term>Random locations</term><term>Real data</term><term>Same time</term><term>Simple beam model</term><term>Simulation</term><term>Single component</term><term>Slower pulsars</term><term>Small number</term><term>Stellar magnetospheres</term><term>Stellar surface</term><term>Sudden variation</term><term>Temporal resolution</term><term>Total number</term><term>Transition point</term><term>Visual inspection</term><term>Wide range</term><term>Young pulsars</term></keywords><keywords scheme="Pascal" xml:lang="fr"><term>Emission radioélectrique</term><term>Energétique</term><term>Forme impulsion</term><term>Ligne force</term><term>Magnétosphère stellaire</term><term>Modèle empirique</term><term>Méthode Monte Carlo</term><term>Pulsar radio</term><term>Variation brusque</term></keywords><keywords scheme="Teeft" xml:lang="en"><term>Abrupt change</term><term>Abrupt transition</term><term>Active heights</term><term>Active patches</term><term>Average pulse</term><term>Beam model</term><term>Discrete heights</term><term>Double component</term><term>Emission cone</term><term>Emission height</term><term>Emission heights</term><term>Emission patches</term><term>Empirical model</term><term>Energetic pulsars</term><term>Entire range</term><term>Free parameters</term><term>Height range</term><term>High altitudes</term><term>High frequencies</term><term>Johnston weisberg</term><term>Journal compilation</term><term>Karastergiou</term><term>Karastergiou johnston</term><term>Large diversity</term><term>Large fraction</term><term>Large number</term><term>Light cylinder</term><term>Light cylinder radius</term><term>Lower altitudes</term><term>Lyne manchester</term><term>Magnetic axis</term><term>Magnetic pole</term><term>Magnetosphere</term><term>Maximum altitude</term><term>Maximum emission height</term><term>Maximum height</term><term>Minimum height</term><term>Mitra</term><term>Mitra rankin</term><term>Mnras</term><term>Natural explanation</term><term>Numerical simulations</term><term>Observational data</term><term>Older pulsars</term><term>Other hand</term><term>Parameter space</term><term>Parkes radio telescope</term><term>Particular frequency</term><term>Patchy</term><term>Pulsar</term><term>Pulsar beam</term><term>Pulsar beams</term><term>Pulsar period</term><term>Pulse longitude</term><term>Pulse period</term><term>Pulse width</term><term>Radio emission</term><term>Radio pulsars</term><term>Random locations</term><term>Real data</term><term>Same time</term><term>Simple beam model</term><term>Simulation</term><term>Single component</term><term>Slower pulsars</term><term>Small number</term><term>Stellar surface</term><term>Temporal resolution</term><term>Total number</term><term>Transition point</term><term>Visual inspection</term><term>Wide range</term><term>Young pulsars</term></keywords><keywords scheme="Wicri" type="topic" xml:lang="fr"><term>Simulation</term></keywords></textClass></profileDesc></teiHeader><front><div type="abstract" xml: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.</div></front></TEI><affiliations><list><country><li>Australie</li><li>France</li></country><region><li>Auvergne-Rhône-Alpes</li><li>Rhône-Alpes</li></region><settlement><li>Grenoble</li><li>Saint-Martin-d'Hères</li></settlement></list><tree><country name="France"><region name="Auvergne-Rhône-Alpes"><name sortKey="Karastergiou, Aris" sort="Karastergiou, Aris" uniqKey="Karastergiou A" first="Aris" last="Karastergiou">Aris Karastergiou</name></region></country><country name="Australie"><noRegion><name sortKey="Johnston, Simon" sort="Johnston, Simon" uniqKey="Johnston S" first="Simon" last="Johnston">Simon Johnston</name></noRegion></country></tree></affiliations></record>Pour manipuler ce document sous Unix (Dilib)
EXPLOR_STEP=$WICRI_ROOT/Wicri/Asie/explor/AustralieFrV1/Data/Main/Exploration
HfdSelect -h $EXPLOR_STEP/biblio.hfd -nk 009209 | SxmlIndent | more
Ou
HfdSelect -h $EXPLOR_AREA/Data/Main/Exploration/biblio.hfd -nk 009209 | SxmlIndent | more
Pour mettre un lien sur cette page dans le réseau Wicri
{{Explor lien
|wiki= Wicri/Asie
|area= AustralieFrV1
|flux= Main
|étape= Exploration
|type= RBID
|clé= ISTEX:6BCB393470B5BD8D4BE70F3E79B06D945DFABC49
|texte= An empirical model for the beams of radio pulsars
}}
| This area was generated with Dilib version V0.6.33. |  |