umu.sePublikasjoner
Endre søk
RefereraExporteraLink to record
Permanent link

Direct link
Referera
Referensformat
  • apa
  • ieee
  • modern-language-association-8th-edition
  • vancouver
  • Annet format
Fler format
Språk
  • de-DE
  • en-GB
  • en-US
  • fi-FI
  • nn-NO
  • nn-NB
  • sv-SE
  • Annet språk
Fler språk
Utmatningsformat
  • html
  • text
  • asciidoc
  • rtf
Oxygen ion response to proton bursty bulk flows
Umeå universitet, Teknisk-naturvetenskapliga fakulteten, Institutionen för fysik.
Umeå universitet, Teknisk-naturvetenskapliga fakulteten, Institutionen för fysik.
Vise andre og tillknytning
2016 (engelsk)Inngår i: Journal of Geophysical Research - Space Physics, ISSN 2169-9380, E-ISSN 2169-9402, Vol. 121, nr 8, s. 7535-7546Artikkel i tidsskrift (Fagfellevurdert) Published
Abstract [en]

We have used Cluster spacecraft data from the years 2001 to 2005 to study how oxygen ions respond to bursty bulk flows (BBFs) as identified from proton data. We here define bursty bulk flows as periods of proton perpendicular velocities more than 100 km/s and a peak perpendicular velocity in the structure of more than 200 km/s, observed in a region with plasma beta above 1 in the near-Earth central tail region. We find that during proton BBFs only a minor increase in the O+ velocity is seen. The different behavior of the two ion species is further shown by statistics of H+ and O+ flow also outside BBFs: For perpendicular earthward velocities of H+ above about 100 km/s, the O+ perpendicular velocity is consistently lower, most commonly being a few tens of kilometers per second earthward. In summary, O+ ions in the plasma sheet experience less acceleration than H+ ions and are not fully frozen in to the magnetic field. Therefore, H+ and O+ motion is decoupled, and O+ ions have a slower earthward motion. This is particularly clear during BBFs. This may add further to the increased relative abundance of O+ ions in the plasma sheet during magnetic storms. The data indicate that O+ is typically less accelerated in association with plasma sheet X lines as compared to H+.

sted, utgiver, år, opplag, sider
2016. Vol. 121, nr 8, s. 7535-7546
HSV kategori
Identifikatorer
URN: urn:nbn:se:umu:diva-127637DOI: 10.1002/2016JA022498ISI: 000385811500016OAI: oai:DiVA.org:umu-127637DiVA, id: diva2:1047368
Tilgjengelig fra: 2016-11-17 Laget: 2016-11-16 Sist oppdatert: 2018-06-09bibliografisk kontrollert

Open Access i DiVA

fulltext(5929 kB)99 nedlastinger
Filinformasjon
Fil FULLTEXT01.pdfFilstørrelse 5929 kBChecksum SHA-512
ed374d82955905d46229c25729a34b0342e2a2cc5fb7cd279cff9d4a7f82e10b46cfe61fa4fa1c98455568eb8967ffd79a93a24ed9527966beea7040e1dc2c25
Type fulltextMimetype application/pdf

Andre lenker

Forlagets fulltekst

Personposter BETA

Hamrin, MariaPitkänen, Timo

Søk i DiVA

Av forfatter/redaktør
Hamrin, MariaPitkänen, Timo
Av organisasjonen
I samme tidsskrift
Journal of Geophysical Research - Space Physics

Søk utenfor DiVA

GoogleGoogle Scholar
Totalt: 99 nedlastinger
Antall nedlastinger er summen av alle nedlastinger av alle fulltekster. Det kan for eksempel være tidligere versjoner som er ikke lenger tilgjengelige

doi
urn-nbn

Altmetric

doi
urn-nbn
Totalt: 191 treff
RefereraExporteraLink to record
Permanent link

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