Association Between Magnetic Pressure Difference and the Movement of Solar Pores
Solar pores are closely related to the concentration, dissipation, and transportation of solar magnetic flux. Their observable characteristics can provide constraints on models and simulations of magnetic flux emergence and formation. The specific property investigated in this study is their horizon...
Gespeichert in:
| Veröffentlicht in: | The Astrophysical journal 2023-03, Vol.946 (1), p.9 |
|---|---|
| Hauptverfasser: | , |
| Format: | Artikel |
| Sprache: | eng |
| Schlagworte: | |
| Online-Zugang: | Volltext |
| Tags: |
Tag hinzufügen
Keine Tags, Fügen Sie den ersten Tag hinzu!
|
| container_end_page | |
|---|---|
| container_issue | 1 |
| container_start_page | 9 |
| container_title | The Astrophysical journal |
| container_volume | 946 |
| creator | Mendoza, Merlin M. Lin, Chia-Hsien |
| description | Solar pores are closely related to the concentration, dissipation, and transportation of solar magnetic flux. Their observable characteristics can provide constraints on models and simulations of magnetic flux emergence and formation. The specific property investigated in this study is their horizontal movement. The aim is to investigate whether the movement is correlated with any observable quantities. Our statistical analysis of 61 compact pores identified from the Spaceweather HMI Active Region Patches (SHARP) from 2011 to 2018 indicates that the direction of movement is often either parallel or antiparallel to the direction of maximum magnetic pressure difference (
dP
mag
) at the opposite sides of the edges of the pores. The correlation coefficients for both the parallel and antiparallel cases are higher than 0.74. Despite the high correlation, our analysis using the transfer entropy indicates no significant causal relationship between the direction of motion and the direction of maximum
dP
mag
. |
| doi_str_mv | 10.3847/1538-4357/acbe43 |
| format | Article |
| fullrecord | <record><control><sourceid>proquest_cross</sourceid><recordid>TN_cdi_crossref_primary_10_3847_1538_4357_acbe43</recordid><sourceformat>XML</sourceformat><sourcesystem>PC</sourcesystem><doaj_id>oai_doaj_org_article_f2e0e4f534ab444fb135c01ee90b7a4d</doaj_id><sourcerecordid>2789773874</sourcerecordid><originalsourceid>FETCH-LOGICAL-c397t-f91c8b51a4b20f2336df4fec5acdd17bcb43f77322b720b543f9dca08ae444683</originalsourceid><addsrcrecordid>eNp9kU1PGzEQhq2KSg0pd46WcmXBXnvj9ZFSaCMFEQmQuFlj7zjdKKy39oaq_x6HrcKl4jSa0fO-80XIKWfnopbqgleiLqSo1AU4i1J8IpND6YhMGGOymAv19IUcp7TZp6XWE7K6TCm4FoY2dPQbDn8QO3oL6w6H1tFVxJR2Een31nuM2Dmk0DV0-IX0NrzgM3YDDZ7ehy1EugoZ_0o-e9gmPPkXp-Tx5vrh6mexvPuxuLpcFk5oNRRec1fbioO0JfOlEPPGS4-uAtc0XFlnpfBKibK0qmS2ypluHLAaUEo5r8WULEbfJsDG9LF9hvjXBGjNWyHEtYGYd9ii8SUylL4SEmwWe8tF5RhH1MwqkE32mo1efQy_d5gGswm72OXxTalqnceolcwUGykXQ0oR_aErZ2b_A7M_uNkf3Iw_yJKzUdKG_t3zA3z2Hxz6jdFybrjRpm-8eAXh7pTP</addsrcrecordid><sourcetype>Open Website</sourcetype><iscdi>true</iscdi><recordtype>article</recordtype><pqid>2789773874</pqid></control><display><type>article</type><title>Association Between Magnetic Pressure Difference and the Movement of Solar Pores</title><source>DOAJ Directory of Open Access Journals</source><source>Elektronische Zeitschriftenbibliothek - Frei zugängliche E-Journals</source><source>Institute of Physics Open Access Journal Titles</source><source>Alma/SFX Local Collection</source><creator>Mendoza, Merlin M. ; Lin, Chia-Hsien</creator><creatorcontrib>Mendoza, Merlin M. ; Lin, Chia-Hsien</creatorcontrib><description>Solar pores are closely related to the concentration, dissipation, and transportation of solar magnetic flux. Their observable characteristics can provide constraints on models and simulations of magnetic flux emergence and formation. The specific property investigated in this study is their horizontal movement. The aim is to investigate whether the movement is correlated with any observable quantities. Our statistical analysis of 61 compact pores identified from the Spaceweather HMI Active Region Patches (SHARP) from 2011 to 2018 indicates that the direction of movement is often either parallel or antiparallel to the direction of maximum magnetic pressure difference (
dP
mag
) at the opposite sides of the edges of the pores. The correlation coefficients for both the parallel and antiparallel cases are higher than 0.74. Despite the high correlation, our analysis using the transfer entropy indicates no significant causal relationship between the direction of motion and the direction of maximum
dP
mag
.</description><identifier>ISSN: 0004-637X</identifier><identifier>EISSN: 1538-4357</identifier><identifier>DOI: 10.3847/1538-4357/acbe43</identifier><language>eng</language><publisher>Philadelphia: The American Astronomical Society</publisher><subject>Astrophysics ; Constraint modelling ; Correlation coefficient ; Correlation coefficients ; Entropy ; Magnetic flux ; Magnetic properties ; Pores ; Solar active region magnetic fields ; Solar active regions ; Solar activity ; Solar magnetic fields ; Solar magnetic flux ; Solar magnetic flux emergence ; Solar physics ; Statistical analysis</subject><ispartof>The Astrophysical journal, 2023-03, Vol.946 (1), p.9</ispartof><rights>2023. The Author(s). Published by the American Astronomical Society.</rights><rights>2023. The Author(s). Published by the American Astronomical Society. This work is published under http://creativecommons.org/licenses/by/4.0/ (the “License”). Notwithstanding the ProQuest Terms and Conditions, you may use this content in accordance with the terms of the License.</rights><lds50>peer_reviewed</lds50><oa>free_for_read</oa><woscitedreferencessubscribed>false</woscitedreferencessubscribed><cites>FETCH-LOGICAL-c397t-f91c8b51a4b20f2336df4fec5acdd17bcb43f77322b720b543f9dca08ae444683</cites><orcidid>0000-0002-5230-0270 ; 0000-0002-3163-1978</orcidid></display><links><openurl>$$Topenurl_article</openurl><openurlfulltext>$$Topenurlfull_article</openurlfulltext><thumbnail>$$Tsyndetics_thumb_exl</thumbnail><linktopdf>$$Uhttps://iopscience.iop.org/article/10.3847/1538-4357/acbe43/pdf$$EPDF$$P50$$Giop$$Hfree_for_read</linktopdf><link.rule.ids>314,780,784,864,2102,27924,27925,38890,53867</link.rule.ids></links><search><creatorcontrib>Mendoza, Merlin M.</creatorcontrib><creatorcontrib>Lin, Chia-Hsien</creatorcontrib><title>Association Between Magnetic Pressure Difference and the Movement of Solar Pores</title><title>The Astrophysical journal</title><addtitle>APJ</addtitle><addtitle>Astrophys. J</addtitle><description>Solar pores are closely related to the concentration, dissipation, and transportation of solar magnetic flux. Their observable characteristics can provide constraints on models and simulations of magnetic flux emergence and formation. The specific property investigated in this study is their horizontal movement. The aim is to investigate whether the movement is correlated with any observable quantities. Our statistical analysis of 61 compact pores identified from the Spaceweather HMI Active Region Patches (SHARP) from 2011 to 2018 indicates that the direction of movement is often either parallel or antiparallel to the direction of maximum magnetic pressure difference (
dP
mag
) at the opposite sides of the edges of the pores. The correlation coefficients for both the parallel and antiparallel cases are higher than 0.74. Despite the high correlation, our analysis using the transfer entropy indicates no significant causal relationship between the direction of motion and the direction of maximum
dP
mag
.</description><subject>Astrophysics</subject><subject>Constraint modelling</subject><subject>Correlation coefficient</subject><subject>Correlation coefficients</subject><subject>Entropy</subject><subject>Magnetic flux</subject><subject>Magnetic properties</subject><subject>Pores</subject><subject>Solar active region magnetic fields</subject><subject>Solar active regions</subject><subject>Solar activity</subject><subject>Solar magnetic fields</subject><subject>Solar magnetic flux</subject><subject>Solar magnetic flux emergence</subject><subject>Solar physics</subject><subject>Statistical analysis</subject><issn>0004-637X</issn><issn>1538-4357</issn><fulltext>true</fulltext><rsrctype>article</rsrctype><creationdate>2023</creationdate><recordtype>article</recordtype><sourceid>O3W</sourceid><sourceid>DOA</sourceid><recordid>eNp9kU1PGzEQhq2KSg0pd46WcmXBXnvj9ZFSaCMFEQmQuFlj7zjdKKy39oaq_x6HrcKl4jSa0fO-80XIKWfnopbqgleiLqSo1AU4i1J8IpND6YhMGGOymAv19IUcp7TZp6XWE7K6TCm4FoY2dPQbDn8QO3oL6w6H1tFVxJR2Een31nuM2Dmk0DV0-IX0NrzgM3YDDZ7ehy1EugoZ_0o-e9gmPPkXp-Tx5vrh6mexvPuxuLpcFk5oNRRec1fbioO0JfOlEPPGS4-uAtc0XFlnpfBKibK0qmS2ypluHLAaUEo5r8WULEbfJsDG9LF9hvjXBGjNWyHEtYGYd9ii8SUylL4SEmwWe8tF5RhH1MwqkE32mo1efQy_d5gGswm72OXxTalqnceolcwUGykXQ0oR_aErZ2b_A7M_uNkf3Iw_yJKzUdKG_t3zA3z2Hxz6jdFybrjRpm-8eAXh7pTP</recordid><startdate>20230301</startdate><enddate>20230301</enddate><creator>Mendoza, Merlin M.</creator><creator>Lin, Chia-Hsien</creator><general>The American Astronomical Society</general><general>IOP Publishing</general><scope>O3W</scope><scope>TSCCA</scope><scope>AAYXX</scope><scope>CITATION</scope><scope>7TG</scope><scope>8FD</scope><scope>H8D</scope><scope>KL.</scope><scope>L7M</scope><scope>DOA</scope><orcidid>https://orcid.org/0000-0002-5230-0270</orcidid><orcidid>https://orcid.org/0000-0002-3163-1978</orcidid></search><sort><creationdate>20230301</creationdate><title>Association Between Magnetic Pressure Difference and the Movement of Solar Pores</title><author>Mendoza, Merlin M. ; Lin, Chia-Hsien</author></sort><facets><frbrtype>5</frbrtype><frbrgroupid>cdi_FETCH-LOGICAL-c397t-f91c8b51a4b20f2336df4fec5acdd17bcb43f77322b720b543f9dca08ae444683</frbrgroupid><rsrctype>articles</rsrctype><prefilter>articles</prefilter><language>eng</language><creationdate>2023</creationdate><topic>Astrophysics</topic><topic>Constraint modelling</topic><topic>Correlation coefficient</topic><topic>Correlation coefficients</topic><topic>Entropy</topic><topic>Magnetic flux</topic><topic>Magnetic properties</topic><topic>Pores</topic><topic>Solar active region magnetic fields</topic><topic>Solar active regions</topic><topic>Solar activity</topic><topic>Solar magnetic fields</topic><topic>Solar magnetic flux</topic><topic>Solar magnetic flux emergence</topic><topic>Solar physics</topic><topic>Statistical analysis</topic><toplevel>peer_reviewed</toplevel><toplevel>online_resources</toplevel><creatorcontrib>Mendoza, Merlin M.</creatorcontrib><creatorcontrib>Lin, Chia-Hsien</creatorcontrib><collection>Institute of Physics Open Access Journal Titles</collection><collection>IOPscience (Open Access)</collection><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><collection>DOAJ Directory of Open Access Journals</collection><jtitle>The Astrophysical journal</jtitle></facets><delivery><delcategory>Remote Search Resource</delcategory><fulltext>fulltext</fulltext></delivery><addata><au>Mendoza, Merlin M.</au><au>Lin, Chia-Hsien</au><format>journal</format><genre>article</genre><ristype>JOUR</ristype><atitle>Association Between Magnetic Pressure Difference and the Movement of Solar Pores</atitle><jtitle>The Astrophysical journal</jtitle><stitle>APJ</stitle><addtitle>Astrophys. J</addtitle><date>2023-03-01</date><risdate>2023</risdate><volume>946</volume><issue>1</issue><spage>9</spage><pages>9-</pages><issn>0004-637X</issn><eissn>1538-4357</eissn><abstract>Solar pores are closely related to the concentration, dissipation, and transportation of solar magnetic flux. Their observable characteristics can provide constraints on models and simulations of magnetic flux emergence and formation. The specific property investigated in this study is their horizontal movement. The aim is to investigate whether the movement is correlated with any observable quantities. Our statistical analysis of 61 compact pores identified from the Spaceweather HMI Active Region Patches (SHARP) from 2011 to 2018 indicates that the direction of movement is often either parallel or antiparallel to the direction of maximum magnetic pressure difference (
dP
mag
) at the opposite sides of the edges of the pores. The correlation coefficients for both the parallel and antiparallel cases are higher than 0.74. Despite the high correlation, our analysis using the transfer entropy indicates no significant causal relationship between the direction of motion and the direction of maximum
dP
mag
.</abstract><cop>Philadelphia</cop><pub>The American Astronomical Society</pub><doi>10.3847/1538-4357/acbe43</doi><tpages>11</tpages><orcidid>https://orcid.org/0000-0002-5230-0270</orcidid><orcidid>https://orcid.org/0000-0002-3163-1978</orcidid><oa>free_for_read</oa></addata></record> |
| fulltext | fulltext |
| identifier | ISSN: 0004-637X |
| ispartof | The Astrophysical journal, 2023-03, Vol.946 (1), p.9 |
| issn | 0004-637X 1538-4357 |
| language | eng |
| recordid | cdi_crossref_primary_10_3847_1538_4357_acbe43 |
| source | DOAJ Directory of Open Access Journals; Elektronische Zeitschriftenbibliothek - Frei zugängliche E-Journals; Institute of Physics Open Access Journal Titles; Alma/SFX Local Collection |
| subjects | Astrophysics Constraint modelling Correlation coefficient Correlation coefficients Entropy Magnetic flux Magnetic properties Pores Solar active region magnetic fields Solar active regions Solar activity Solar magnetic fields Solar magnetic flux Solar magnetic flux emergence Solar physics Statistical analysis |
| title | Association Between Magnetic Pressure Difference and the Movement of Solar Pores |
| url | https://sfx.bib-bvb.de/sfx_tum?ctx_ver=Z39.88-2004&ctx_enc=info:ofi/enc:UTF-8&ctx_tim=2024-12-19T06%3A22%3A36IST&url_ver=Z39.88-2004&url_ctx_fmt=infofi/fmt:kev:mtx:ctx&rfr_id=info:sid/primo.exlibrisgroup.com:primo3-Article-proquest_cross&rft_val_fmt=info:ofi/fmt:kev:mtx:journal&rft.genre=article&rft.atitle=Association%20Between%20Magnetic%20Pressure%20Difference%20and%20the%20Movement%20of%20Solar%20Pores&rft.jtitle=The%20Astrophysical%20journal&rft.au=Mendoza,%20Merlin%20M.&rft.date=2023-03-01&rft.volume=946&rft.issue=1&rft.spage=9&rft.pages=9-&rft.issn=0004-637X&rft.eissn=1538-4357&rft_id=info:doi/10.3847/1538-4357/acbe43&rft_dat=%3Cproquest_cross%3E2789773874%3C/proquest_cross%3E%3Curl%3E%3C/url%3E&disable_directlink=true&sfx.directlink=off&sfx.report_link=0&rft_id=info:oai/&rft_pqid=2789773874&rft_id=info:pmid/&rft_doaj_id=oai_doaj_org_article_f2e0e4f534ab444fb135c01ee90b7a4d&rfr_iscdi=true |