Analysis of the Parameters of Radio Pulsars with Giant Pulses Using the Principal Component Analysis
Clustering of radio pulsars with observable giant pulses (GPs) has been carried out using the principal component analysis. Five parameters were used (period, its derivative, observed luminosity, kinematic age, and the angle between the rotation axis and the magnetic moment of the central neutron st...
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| Veröffentlicht in: | Astronomy reports 2023-03, Vol.67 (3), p.263-271 |
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| creator | Malov, I. F. Malov, O. I. |
| description | Clustering of radio pulsars with observable giant pulses (GPs) has been carried out using the principal component analysis. Five parameters were used (period, its derivative, observed luminosity, kinematic age, and the angle between the rotation axis and the magnetic moment of the central neutron star). It was shown that the set of all known GP pulsars is divided into two clusters in the phase space of the principal components. One of the clusters contains four pulsars with short periods and high luminosity; the second cluster contains nine long-period and fainter sources. A separate object, not included in these two clusters, is the pulsar in the Crab Nebula. Possible models that could explain the observed difference between GP pulsars were considered. |
| doi_str_mv | 10.1134/S1063772923030058 |
| format | Article |
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F. ; Malov, O. I.</creator><creatorcontrib>Malov, I. F. ; Malov, O. I.</creatorcontrib><description>Clustering of radio pulsars with observable giant pulses (GPs) has been carried out using the principal component analysis. Five parameters were used (period, its derivative, observed luminosity, kinematic age, and the angle between the rotation axis and the magnetic moment of the central neutron star). It was shown that the set of all known GP pulsars is divided into two clusters in the phase space of the principal components. One of the clusters contains four pulsars with short periods and high luminosity; the second cluster contains nine long-period and fainter sources. A separate object, not included in these two clusters, is the pulsar in the Crab Nebula. Possible models that could explain the observed difference between GP pulsars were considered.</description><identifier>ISSN: 1063-7729</identifier><identifier>EISSN: 1562-6881</identifier><identifier>DOI: 10.1134/S1063772923030058</identifier><language>eng</language><publisher>Moscow: Pleiades Publishing</publisher><subject>Astronomy ; Clustering ; Crab nebula ; Kinematics ; Luminosity ; Magnetic moments ; Neutron stars ; Observations and Techniques ; Parameters ; Physics ; Physics and Astronomy ; Principal components analysis ; Pulsars</subject><ispartof>Astronomy reports, 2023-03, Vol.67 (3), p.263-271</ispartof><rights>Pleiades Publishing, Ltd. 2023. ISSN 1063-7729, Astronomy Reports, 2023, Vol. 67, No. 3, pp. 263–271. © Pleiades Publishing, Ltd., 2023. Russian Text © The Author(s), 2023, published in Astronomicheskii Zhurnal, 2023, Vol. 100, No. 3, pp. 272–280.</rights><lds50>peer_reviewed</lds50><woscitedreferencessubscribed>false</woscitedreferencessubscribed><cites>FETCH-LOGICAL-c268t-899533060f1120b677a7fc10502f6e0dd9cfdb45c91b68898dce346090f324a73</cites></display><links><openurl>$$Topenurl_article</openurl><openurlfulltext>$$Topenurlfull_article</openurlfulltext><thumbnail>$$Tsyndetics_thumb_exl</thumbnail><linktopdf>$$Uhttps://link.springer.com/content/pdf/10.1134/S1063772923030058$$EPDF$$P50$$Gspringer$$H</linktopdf><linktohtml>$$Uhttps://link.springer.com/10.1134/S1063772923030058$$EHTML$$P50$$Gspringer$$H</linktohtml><link.rule.ids>314,780,784,27924,27925,41488,42557,51319</link.rule.ids></links><search><creatorcontrib>Malov, I. F.</creatorcontrib><creatorcontrib>Malov, O. I.</creatorcontrib><title>Analysis of the Parameters of Radio Pulsars with Giant Pulses Using the Principal Component Analysis</title><title>Astronomy reports</title><addtitle>Astron. Rep</addtitle><description>Clustering of radio pulsars with observable giant pulses (GPs) has been carried out using the principal component analysis. Five parameters were used (period, its derivative, observed luminosity, kinematic age, and the angle between the rotation axis and the magnetic moment of the central neutron star). It was shown that the set of all known GP pulsars is divided into two clusters in the phase space of the principal components. One of the clusters contains four pulsars with short periods and high luminosity; the second cluster contains nine long-period and fainter sources. A separate object, not included in these two clusters, is the pulsar in the Crab Nebula. Possible models that could explain the observed difference between GP pulsars were considered.</description><subject>Astronomy</subject><subject>Clustering</subject><subject>Crab nebula</subject><subject>Kinematics</subject><subject>Luminosity</subject><subject>Magnetic moments</subject><subject>Neutron stars</subject><subject>Observations and Techniques</subject><subject>Parameters</subject><subject>Physics</subject><subject>Physics and Astronomy</subject><subject>Principal components analysis</subject><subject>Pulsars</subject><issn>1063-7729</issn><issn>1562-6881</issn><fulltext>true</fulltext><rsrctype>article</rsrctype><creationdate>2023</creationdate><recordtype>article</recordtype><recordid>eNp1kEFLAzEQhYMoWKs_wNuC59WZZDebHEvRVihY1J6XdDdpU9rNmmyR_nvTruJBPM3w5nuPmSHkFuEekWUPbwicFQWVlAEDyMUZGWDOacqFwPPYx3F6nF-SqxA2AIiC8QGpR43aHoINiTNJt9bJXHm10532J-VV1dYl8_02qCh82m6dTKxqupOkQ7IItln1Pm-byrZqm4zdrnWNjtBP9jW5MCryN991SBZPj-_jaTp7mTyPR7O0olx0qZAyZww4GEQKS14UqjAVQg7UcA11LStTL7O8kriMZ0lRV5plHCQYRjNVsCG563Nb7z72OnTlxu19XCKUVGAmEaCgkcKeqrwLwWtTtt7ulD-UCOXxmeWfZ0YP7T0hss1K-9_k_01fWdN1Vg</recordid><startdate>20230301</startdate><enddate>20230301</enddate><creator>Malov, I. F.</creator><creator>Malov, O. I.</creator><general>Pleiades Publishing</general><general>Springer Nature B.V</general><scope>AAYXX</scope><scope>CITATION</scope><scope>7TG</scope><scope>8FD</scope><scope>H8D</scope><scope>KL.</scope><scope>L7M</scope></search><sort><creationdate>20230301</creationdate><title>Analysis of the Parameters of Radio Pulsars with Giant Pulses Using the Principal Component Analysis</title><author>Malov, I. F. ; Malov, O. I.</author></sort><facets><frbrtype>5</frbrtype><frbrgroupid>cdi_FETCH-LOGICAL-c268t-899533060f1120b677a7fc10502f6e0dd9cfdb45c91b68898dce346090f324a73</frbrgroupid><rsrctype>articles</rsrctype><prefilter>articles</prefilter><language>eng</language><creationdate>2023</creationdate><topic>Astronomy</topic><topic>Clustering</topic><topic>Crab nebula</topic><topic>Kinematics</topic><topic>Luminosity</topic><topic>Magnetic moments</topic><topic>Neutron stars</topic><topic>Observations and Techniques</topic><topic>Parameters</topic><topic>Physics</topic><topic>Physics and Astronomy</topic><topic>Principal components analysis</topic><topic>Pulsars</topic><toplevel>peer_reviewed</toplevel><toplevel>online_resources</toplevel><creatorcontrib>Malov, I. F.</creatorcontrib><creatorcontrib>Malov, O. I.</creatorcontrib><collection>CrossRef</collection><collection>Meteorological & Geoastrophysical Abstracts</collection><collection>Technology Research Database</collection><collection>Aerospace Database</collection><collection>Meteorological & Geoastrophysical Abstracts - Academic</collection><collection>Advanced Technologies Database with Aerospace</collection><jtitle>Astronomy reports</jtitle></facets><delivery><delcategory>Remote Search Resource</delcategory><fulltext>fulltext</fulltext></delivery><addata><au>Malov, I. F.</au><au>Malov, O. I.</au><format>journal</format><genre>article</genre><ristype>JOUR</ristype><atitle>Analysis of the Parameters of Radio Pulsars with Giant Pulses Using the Principal Component Analysis</atitle><jtitle>Astronomy reports</jtitle><stitle>Astron. 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| source | SpringerNature Journals |
| subjects | Astronomy Clustering Crab nebula Kinematics Luminosity Magnetic moments Neutron stars Observations and Techniques Parameters Physics Physics and Astronomy Principal components analysis Pulsars |
| title | Analysis of the Parameters of Radio Pulsars with Giant Pulses Using the Principal Component Analysis |
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