Search: WFRF:(Janhunen S) >
3D GUMICS Simulatio...
-
Fryer, L. J.School of Physics Astronomy, University of Southampton, Southampton, UK
(author)
3D GUMICS Simulations of Northward IMF Magnetotail Structure
- Article/chapterEnglish2023
Publisher, publication year, extent ...
-
American Geophysical Union (AGU),2023
-
printrdacarrier
Numbers
-
LIBRIS-ID:oai:DiVA.org:kth-334787
-
https://urn.kb.se/resolve?urn=urn:nbn:se:kth:diva-334787URI
-
https://doi.org/10.1029/2023JA031317DOI
Supplementary language notes
-
Language:English
-
Summary in:English
Part of subdatabase
Classification
-
Subject category:ref swepub-contenttype
-
Subject category:art swepub-publicationtype
Notes
-
QC 20230901
-
This study presents a re-evaluation of the Kullen and Janhunen (2004, https://doi.org/10.5194/angeo-22-951-2004) global northward interplanetary magnetic field (IMF) simulation, using the Grand Unified Magnetosphere–Ionosphere Coupling Simulation version 4 (GUMICS-4), a global MHD model. We investigate the dynamic coupling between northward IMF conditions and the Earth’s magnetotail and compare the results to observation-based mechanisms for the formation of transpolar arcs. The results of this study reveal that under northward IMF conditions (and northward IMF initialization), a large closed field line region forms in the magnetotail, with similarities to transpolar arc structures observed from spacecraft data. This interpretation is supported by the simultaneous increase of closed flux measured in the magnetotail. However, the reconnection configuration differs in several respects from previously theorized magnetotail structures that have been inferred from both observations and simulations results and associated with transpolar arcs. We observe that dawn–dusk lobe regions form as a result of high-latitude reconnection during the initialization stages, which later come into contact as the change in the IMF By component causes the magnetotail to twist. We conclude that in the GUMICS simulation, transpolar arc-like structures are formed as a result of reconnection in the magnetotail, rather than high-latitude reconnection or due to the mapping of the plasma sheet through a twisted magnetotail as interpreted from previous analysis of GUMICS simulations.
Subject headings and genre
Added entries (persons, corporate bodies, meetings, titles ...)
-
Fear, R. C.School of Physics Astronomy, University of Southampton, Southampton, UK
(author)
-
Gingell, I. L.School of Physics Astronomy, University of Southampton, Southampton, UK
(author)
-
Coxon, J. C.Department of Physics, Northumbria University, Northumbria, UK
(author)
-
Palmroth, M.Department of Physics, University of Helsinki, Helsinki, Finland; Finnish Meteorological Institute, Helsinki, Finland
(author)
-
Hoilijoki, S.Department of Physics, University of Helsinki, Helsinki, Finland
(author)
-
Janhunen, P.Department of Physics, University of Helsinki, Helsinki, Finland; Finnish Meteorological Institute, Helsinki, Finland
(author)
-
Kullen, AnitaKTH,Rymd- och plasmafysik(Swepub:kth)u1yjgq07
(author)
-
Cassak, P. A.Department of Physics and Astronomy, West Virginia University, Morgantown, WV, USA
(author)
-
School of Physics Astronomy, University of Southampton, Southampton, UKDepartment of Physics, Northumbria University, Northumbria, UK
(creator_code:org_t)
Related titles
-
In:Journal of Geophysical Research - Space Physics: American Geophysical Union (AGU)128:82169-93802169-9402
Internet link
Find in a library
To the university's database