Non-thermal neutrinos from supernovae leaving a magnetar
Under the fossil field hypothesis of the origin of magnetar magnetic fields, the magnetar inherits its magnetic field from its progenitor. We show that during the supernova of such a progenitor, protons may be accelerated to ∼104 GeV as the supernova shock propagates in the stellar envelope. Inelast...
Gespeichert in:
| Veröffentlicht in: | Monthly notices of the Royal Astronomical Society 2008-12, Vol.391 (4), p.1893-1899 |
|---|---|
| Hauptverfasser: | , , , , |
| Format: | Artikel |
| Sprache: | eng |
| Schlagworte: | |
| Online-Zugang: | Volltext |
| Tags: |
Tag hinzufügen
Keine Tags, Fügen Sie den ersten Tag hinzu!
|
| container_end_page | 1899 |
|---|---|
| container_issue | 4 |
| container_start_page | 1893 |
| container_title | Monthly notices of the Royal Astronomical Society |
| container_volume | 391 |
| creator | Horiuchi, Shunsaku Suwa, Yudai Takami, Hajime Ando, Shin'ichiro Sato, Katsuhiko |
| description | Under the fossil field hypothesis of the origin of magnetar magnetic fields, the magnetar inherits its magnetic field from its progenitor. We show that during the supernova of such a progenitor, protons may be accelerated to ∼104 GeV as the supernova shock propagates in the stellar envelope. Inelastic nuclear collisions of these protons produce a flash of high-energy neutrinos arriving a few hours after thermal (10 MeV) neutrinos. The neutrino flash is characterized by energies up to O(100) GeV and durations seconds to hours, depending on the progenitor: those from smaller Type Ibc progenitors are typically shorter in duration and reach higher energies compared to those from larger Type II progenitors. A Galactic Type Ib supernova leaving behind a magnetar remnant will yield up to ∼160 neutrino-induced muon events in Super-Kamiokande, and up to ∼7000 in a km3 class detector such as IceCube, providing a means of probing supernova models and the presence of strong magnetic fields in the stellar envelope. |
| doi_str_mv | 10.1111/j.1365-2966.2008.14000.x |
| format | Article |
| fullrecord | <record><control><sourceid>proquest_cross</sourceid><recordid>TN_cdi_proquest_miscellaneous_20296295</recordid><sourceformat>XML</sourceformat><sourcesystem>PC</sourcesystem><oup_id>10.1111/j.1365-2966.2008.14000.x</oup_id><sourcerecordid>1610943141</sourcerecordid><originalsourceid>FETCH-LOGICAL-c5340-bcee818f0286d68cbc530627dbd78521b94a6b076559f4b28f2efbd1499f15973</originalsourceid><addsrcrecordid>eNqNkE9L5DAchsOyC86O-x3KgntrN3-aNLkIq-iOMM6CuCBeQtpJtGObjEk7znx7UytzEAVzSUie5-WXF4AEwQzF9XuVIcJoigVjGYaQZyiHEGbbL2Cyf_gKJhASmvICoQPwPYRVRHKC2QTwhbNpd699q5rE6r7ztXUhMd61SejX2lu3UTpptNrU9i5RSavurO6UPwTfjGqC_vG6T8H_87Pr01k6__f34vTPPK0oyWFaVlpzxA3EnC0Zr8p4DRkuluWy4BSjUuSKlbBglAqTl5gbrE25RLkQBlFRkCn4NeauvXvsdehkW4dKN42y2vVBYhh_iAWN4M834Mr13sbZIlMQxgQVEeIjVHkXgtdGrn3dKr-TCMqhT7mSQ21yqE0OfcqXPuU2qkev-SpUqjFe2aoOex9DQRnLYeSOR-6pbvTu0_nycnH1cowBZAxw_foDPX1vvHS06tDp7d5T_kGyghRUzm5u5Wy-OLm5zK8lJc-cu6WP</addsrcrecordid><sourcetype>Aggregation Database</sourcetype><iscdi>true</iscdi><recordtype>article</recordtype><pqid>207366959</pqid></control><display><type>article</type><title>Non-thermal neutrinos from supernovae leaving a magnetar</title><source>Wiley Online Library Journals Frontfile Complete</source><source>Oxford Open</source><creator>Horiuchi, Shunsaku ; Suwa, Yudai ; Takami, Hajime ; Ando, Shin'ichiro ; Sato, Katsuhiko</creator><creatorcontrib>Horiuchi, Shunsaku ; Suwa, Yudai ; Takami, Hajime ; Ando, Shin'ichiro ; Sato, Katsuhiko</creatorcontrib><description>Under the fossil field hypothesis of the origin of magnetar magnetic fields, the magnetar inherits its magnetic field from its progenitor. We show that during the supernova of such a progenitor, protons may be accelerated to ∼104 GeV as the supernova shock propagates in the stellar envelope. Inelastic nuclear collisions of these protons produce a flash of high-energy neutrinos arriving a few hours after thermal (10 MeV) neutrinos. The neutrino flash is characterized by energies up to O(100) GeV and durations seconds to hours, depending on the progenitor: those from smaller Type Ibc progenitors are typically shorter in duration and reach higher energies compared to those from larger Type II progenitors. A Galactic Type Ib supernova leaving behind a magnetar remnant will yield up to ∼160 neutrino-induced muon events in Super-Kamiokande, and up to ∼7000 in a km3 class detector such as IceCube, providing a means of probing supernova models and the presence of strong magnetic fields in the stellar envelope.</description><identifier>ISSN: 0035-8711</identifier><identifier>EISSN: 1365-2966</identifier><identifier>DOI: 10.1111/j.1365-2966.2008.14000.x</identifier><identifier>CODEN: MNRAA4</identifier><language>eng</language><publisher>Oxford, UK: Blackwell Publishing Ltd</publisher><subject>acceleration of particles ; Astronomy ; Astrophysics ; Earth, ocean, space ; Exact sciences and technology ; Magnetic fields ; Neutrinos ; Particle physics ; pulsars: general ; Stars & galaxies ; stars: magnetic fields ; Supernovae ; supernovae: general</subject><ispartof>Monthly notices of the Royal Astronomical Society, 2008-12, Vol.391 (4), p.1893-1899</ispartof><rights>2008 The Authors. Journal compilation © 2008 RAS 2008</rights><rights>2008 The Authors. Journal compilation © 2008 RAS</rights><rights>2009 INIST-CNRS</rights><rights>Journal compilation © 2008 RAS</rights><lds50>peer_reviewed</lds50><oa>free_for_read</oa><woscitedreferencessubscribed>false</woscitedreferencessubscribed><citedby>FETCH-LOGICAL-c5340-bcee818f0286d68cbc530627dbd78521b94a6b076559f4b28f2efbd1499f15973</citedby><cites>FETCH-LOGICAL-c5340-bcee818f0286d68cbc530627dbd78521b94a6b076559f4b28f2efbd1499f15973</cites></display><links><openurl>$$Topenurl_article</openurl><openurlfulltext>$$Topenurlfull_article</openurlfulltext><thumbnail>$$Tsyndetics_thumb_exl</thumbnail><linktopdf>$$Uhttps://onlinelibrary.wiley.com/doi/pdf/10.1111%2Fj.1365-2966.2008.14000.x$$EPDF$$P50$$Gwiley$$H</linktopdf><linktohtml>$$Uhttps://onlinelibrary.wiley.com/doi/full/10.1111%2Fj.1365-2966.2008.14000.x$$EHTML$$P50$$Gwiley$$H</linktohtml><link.rule.ids>314,776,780,1411,27903,27904,45553,45554</link.rule.ids><backlink>$$Uhttp://pascal-francis.inist.fr/vibad/index.php?action=getRecordDetail&idt=20956640$$DView record in Pascal Francis$$Hfree_for_read</backlink></links><search><creatorcontrib>Horiuchi, Shunsaku</creatorcontrib><creatorcontrib>Suwa, Yudai</creatorcontrib><creatorcontrib>Takami, Hajime</creatorcontrib><creatorcontrib>Ando, Shin'ichiro</creatorcontrib><creatorcontrib>Sato, Katsuhiko</creatorcontrib><title>Non-thermal neutrinos from supernovae leaving a magnetar</title><title>Monthly notices of the Royal Astronomical Society</title><addtitle>Monthly Notices of the Royal Astronomical Society</addtitle><addtitle>Monthly Notices of the Royal Astronomical Society</addtitle><description>Under the fossil field hypothesis of the origin of magnetar magnetic fields, the magnetar inherits its magnetic field from its progenitor. We show that during the supernova of such a progenitor, protons may be accelerated to ∼104 GeV as the supernova shock propagates in the stellar envelope. Inelastic nuclear collisions of these protons produce a flash of high-energy neutrinos arriving a few hours after thermal (10 MeV) neutrinos. The neutrino flash is characterized by energies up to O(100) GeV and durations seconds to hours, depending on the progenitor: those from smaller Type Ibc progenitors are typically shorter in duration and reach higher energies compared to those from larger Type II progenitors. A Galactic Type Ib supernova leaving behind a magnetar remnant will yield up to ∼160 neutrino-induced muon events in Super-Kamiokande, and up to ∼7000 in a km3 class detector such as IceCube, providing a means of probing supernova models and the presence of strong magnetic fields in the stellar envelope.</description><subject>acceleration of particles</subject><subject>Astronomy</subject><subject>Astrophysics</subject><subject>Earth, ocean, space</subject><subject>Exact sciences and technology</subject><subject>Magnetic fields</subject><subject>Neutrinos</subject><subject>Particle physics</subject><subject>pulsars: general</subject><subject>Stars & galaxies</subject><subject>stars: magnetic fields</subject><subject>Supernovae</subject><subject>supernovae: general</subject><issn>0035-8711</issn><issn>1365-2966</issn><fulltext>true</fulltext><rsrctype>article</rsrctype><creationdate>2008</creationdate><recordtype>article</recordtype><recordid>eNqNkE9L5DAchsOyC86O-x3KgntrN3-aNLkIq-iOMM6CuCBeQtpJtGObjEk7znx7UytzEAVzSUie5-WXF4AEwQzF9XuVIcJoigVjGYaQZyiHEGbbL2Cyf_gKJhASmvICoQPwPYRVRHKC2QTwhbNpd699q5rE6r7ztXUhMd61SejX2lu3UTpptNrU9i5RSavurO6UPwTfjGqC_vG6T8H_87Pr01k6__f34vTPPK0oyWFaVlpzxA3EnC0Zr8p4DRkuluWy4BSjUuSKlbBglAqTl5gbrE25RLkQBlFRkCn4NeauvXvsdehkW4dKN42y2vVBYhh_iAWN4M834Mr13sbZIlMQxgQVEeIjVHkXgtdGrn3dKr-TCMqhT7mSQ21yqE0OfcqXPuU2qkev-SpUqjFe2aoOex9DQRnLYeSOR-6pbvTu0_nycnH1cowBZAxw_foDPX1vvHS06tDp7d5T_kGyghRUzm5u5Wy-OLm5zK8lJc-cu6WP</recordid><startdate>20081221</startdate><enddate>20081221</enddate><creator>Horiuchi, Shunsaku</creator><creator>Suwa, Yudai</creator><creator>Takami, Hajime</creator><creator>Ando, Shin'ichiro</creator><creator>Sato, Katsuhiko</creator><general>Blackwell Publishing Ltd</general><general>Wiley-Blackwell</general><general>Oxford University Press</general><scope>BSCLL</scope><scope>IQODW</scope><scope>AAYXX</scope><scope>CITATION</scope><scope>8FD</scope><scope>H8D</scope><scope>L7M</scope><scope>7TG</scope><scope>KL.</scope></search><sort><creationdate>20081221</creationdate><title>Non-thermal neutrinos from supernovae leaving a magnetar</title><author>Horiuchi, Shunsaku ; Suwa, Yudai ; Takami, Hajime ; Ando, Shin'ichiro ; Sato, Katsuhiko</author></sort><facets><frbrtype>5</frbrtype><frbrgroupid>cdi_FETCH-LOGICAL-c5340-bcee818f0286d68cbc530627dbd78521b94a6b076559f4b28f2efbd1499f15973</frbrgroupid><rsrctype>articles</rsrctype><prefilter>articles</prefilter><language>eng</language><creationdate>2008</creationdate><topic>acceleration of particles</topic><topic>Astronomy</topic><topic>Astrophysics</topic><topic>Earth, ocean, space</topic><topic>Exact sciences and technology</topic><topic>Magnetic fields</topic><topic>Neutrinos</topic><topic>Particle physics</topic><topic>pulsars: general</topic><topic>Stars & galaxies</topic><topic>stars: magnetic fields</topic><topic>Supernovae</topic><topic>supernovae: general</topic><toplevel>peer_reviewed</toplevel><toplevel>online_resources</toplevel><creatorcontrib>Horiuchi, Shunsaku</creatorcontrib><creatorcontrib>Suwa, Yudai</creatorcontrib><creatorcontrib>Takami, Hajime</creatorcontrib><creatorcontrib>Ando, Shin'ichiro</creatorcontrib><creatorcontrib>Sato, Katsuhiko</creatorcontrib><collection>Istex</collection><collection>Pascal-Francis</collection><collection>CrossRef</collection><collection>Technology Research Database</collection><collection>Aerospace Database</collection><collection>Advanced Technologies Database with Aerospace</collection><collection>Meteorological & Geoastrophysical Abstracts</collection><collection>Meteorological & Geoastrophysical Abstracts - Academic</collection><jtitle>Monthly notices of the Royal Astronomical Society</jtitle></facets><delivery><delcategory>Remote Search Resource</delcategory><fulltext>fulltext</fulltext></delivery><addata><au>Horiuchi, Shunsaku</au><au>Suwa, Yudai</au><au>Takami, Hajime</au><au>Ando, Shin'ichiro</au><au>Sato, Katsuhiko</au><format>journal</format><genre>article</genre><ristype>JOUR</ristype><atitle>Non-thermal neutrinos from supernovae leaving a magnetar</atitle><jtitle>Monthly notices of the Royal Astronomical Society</jtitle><stitle>Monthly Notices of the Royal Astronomical Society</stitle><addtitle>Monthly Notices of the Royal Astronomical Society</addtitle><date>2008-12-21</date><risdate>2008</risdate><volume>391</volume><issue>4</issue><spage>1893</spage><epage>1899</epage><pages>1893-1899</pages><issn>0035-8711</issn><eissn>1365-2966</eissn><coden>MNRAA4</coden><abstract>Under the fossil field hypothesis of the origin of magnetar magnetic fields, the magnetar inherits its magnetic field from its progenitor. We show that during the supernova of such a progenitor, protons may be accelerated to ∼104 GeV as the supernova shock propagates in the stellar envelope. Inelastic nuclear collisions of these protons produce a flash of high-energy neutrinos arriving a few hours after thermal (10 MeV) neutrinos. The neutrino flash is characterized by energies up to O(100) GeV and durations seconds to hours, depending on the progenitor: those from smaller Type Ibc progenitors are typically shorter in duration and reach higher energies compared to those from larger Type II progenitors. A Galactic Type Ib supernova leaving behind a magnetar remnant will yield up to ∼160 neutrino-induced muon events in Super-Kamiokande, and up to ∼7000 in a km3 class detector such as IceCube, providing a means of probing supernova models and the presence of strong magnetic fields in the stellar envelope.</abstract><cop>Oxford, UK</cop><pub>Blackwell Publishing Ltd</pub><doi>10.1111/j.1365-2966.2008.14000.x</doi><tpages>7</tpages><oa>free_for_read</oa></addata></record> |
| fulltext | fulltext |
| identifier | ISSN: 0035-8711 |
| ispartof | Monthly notices of the Royal Astronomical Society, 2008-12, Vol.391 (4), p.1893-1899 |
| issn | 0035-8711 1365-2966 |
| language | eng |
| recordid | cdi_proquest_miscellaneous_20296295 |
| source | Wiley Online Library Journals Frontfile Complete; Oxford Open |
| subjects | acceleration of particles Astronomy Astrophysics Earth, ocean, space Exact sciences and technology Magnetic fields Neutrinos Particle physics pulsars: general Stars & galaxies stars: magnetic fields Supernovae supernovae: general |
| title | Non-thermal neutrinos from supernovae leaving a magnetar |
| url | https://sfx.bib-bvb.de/sfx_tum?ctx_ver=Z39.88-2004&ctx_enc=info:ofi/enc:UTF-8&ctx_tim=2025-01-22T17%3A42%3A34IST&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=Non-thermal%20neutrinos%20from%20supernovae%20leaving%20a%20magnetar&rft.jtitle=Monthly%20notices%20of%20the%20Royal%20Astronomical%20Society&rft.au=Horiuchi,%20Shunsaku&rft.date=2008-12-21&rft.volume=391&rft.issue=4&rft.spage=1893&rft.epage=1899&rft.pages=1893-1899&rft.issn=0035-8711&rft.eissn=1365-2966&rft.coden=MNRAA4&rft_id=info:doi/10.1111/j.1365-2966.2008.14000.x&rft_dat=%3Cproquest_cross%3E1610943141%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=207366959&rft_id=info:pmid/&rft_oup_id=10.1111/j.1365-2966.2008.14000.x&rfr_iscdi=true |