Ändra sökning
RefereraExporteraLänk till posten
Permanent länk

Direktlänk
Referera
Referensformat
  • apa
  • harvard1
  • ieee
  • modern-language-association-8th-edition
  • vancouver
  • Annat format
Fler format
Språk
  • de-DE
  • en-GB
  • en-US
  • fi-FI
  • nn-NO
  • nn-NB
  • sv-SE
  • Annat språk
Fler språk
Utmatningsformat
  • html
  • text
  • asciidoc
  • rtf
The statistical difference between bending arcs and regular polar arcs
KTH, Skolan för elektro- och systemteknik (EES), Rymd- och plasmafysik.ORCID-id: 0000-0002-0349-0645
Visa övriga samt affilieringar
2015 (Engelska)Ingår i: Journal of Geophysical Research - Space Physics, ISSN 2169-9380, E-ISSN 2169-9402, Vol. 120, nr 12, s. 10443-10465Artikel i tidskrift (Refereegranskat) Published
Resurstyp
Text
Abstract [en]

In this work, the Polar UVI data set by Kullen et al. (2002) of 74 polar arcs is reinvestigated, focusing on bending arcs. Bending arcs are typically faint and form (depending on interplanetary magnetic field (IMF) B-y direction) on the dawnside or duskside oval with the tip of the arc splitting off the dayside oval. The tip subsequently moves into the polar cap in the antisunward direction, while the arc's nightside end remains attached to the oval, eventually becoming hook-shaped. Our investigation shows that bending arcs appear on the opposite oval side from and farther sunward than most regular polar arcs. They form during B-y-dominated IMF conditions: typically, the IMF clock angle increases from 60 to 90 degrees about 20min before the arc forms. Antisunward plasma flows from the oval into the polar cap just poleward of bending arcs are seen in Super Dual Auroral Radar Network data, indicating dayside reconnection. For regular polar arcs, recently reported characteristics are confirmed in contrast to bending arcs. This includes plasma flows along the nightside oval that originate close to the initial arc location and a significant delay in the correlation between IMF B-y and initial arc location. In our data set, the highest correlations are found with IMF B-y appearing at least 1-2 h before arc formation. In summary, bending arcs are distinctly different from regular arcs and cannot be explained by existing polar arc models. Instead, these results are consistent with the formation mechanism described in Carter et al. (2015), suggesting that bending arcs are caused by dayside reconnection.

Ort, förlag, år, upplaga, sidor
American Geophysical Union (AGU), 2015. Vol. 120, nr 12, s. 10443-10465
Nationell ämneskategori
Astronomi, astrofysik och kosmologi
Identifikatorer
URN: urn:nbn:se:kth:diva-183227DOI: 10.1002/2015JA021298ISI: 000369180200022Scopus ID: 2-s2.0-84957848598OAI: oai:DiVA.org:kth-183227DiVA, id: diva2:908838
Forskningsfinansiär
Rymdstyrelsen
Anmärkning

QC 20160303

Tillgänglig från: 2016-03-03 Skapad: 2016-03-03 Senast uppdaterad: 2017-11-30Bibliografiskt granskad

Open Access i DiVA

Fulltext saknas i DiVA

Övriga länkar

Förlagets fulltextScopus

Personposter BETA

Kullen, AnitaKarlsson, Tomas

Sök vidare i DiVA

Av författaren/redaktören
Kullen, AnitaKarlsson, Tomas
Av organisationen
Rymd- och plasmafysik
I samma tidskrift
Journal of Geophysical Research - Space Physics
Astronomi, astrofysik och kosmologi

Sök vidare utanför DiVA

GoogleGoogle Scholar

doi
urn-nbn

Altmetricpoäng

doi
urn-nbn
Totalt: 40 träffar
RefereraExporteraLänk till posten
Permanent länk

Direktlänk
Referera
Referensformat
  • apa
  • harvard1
  • ieee
  • modern-language-association-8th-edition
  • vancouver
  • Annat format
Fler format
Språk
  • de-DE
  • en-GB
  • en-US
  • fi-FI
  • nn-NO
  • nn-NB
  • sv-SE
  • Annat språk
Fler språk
Utmatningsformat
  • html
  • text
  • asciidoc
  • rtf