On the relaxation of magnetospheric convection when <I>B</I><sub>z</sub> turns northward
The solar wind inputs considerable energy into the upper atmosphere, particularly when the interplanetary magnetic field (IMF) is southward. According to Poynting's theorem (Kelley, 2009), this energy becomes stored as magnetic fields and then is dissipated by Joule heat and by energizing t...
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Copernicus Publications
2012-06-01
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| Series: | Annales Geophysicae |
| Online Access: | https://www.ann-geophys.net/30/927/2012/angeo-30-927-2012.pdf |
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doaj-744e53de61f24d8aa07dbc38993570d72020-11-24T21:33:42ZengCopernicus PublicationsAnnales Geophysicae0992-76891432-05762012-06-013092792810.5194/angeo-30-927-2012On the relaxation of magnetospheric convection when <I>B</I><sub>z</sub> turns northwardM. C. Kelley0School of Electrical and Computer Engineering, Cornell University, Ithaca, NY, USAThe solar wind inputs considerable energy into the upper atmosphere, particularly when the interplanetary magnetic field (IMF) is southward. According to Poynting's theorem (Kelley, 2009), this energy becomes stored as magnetic fields and then is dissipated by Joule heat and by energizing the plasmasheet plasma. If the IMF turns suddenly northward, very little energy is transferred into the system while Joule dissipation continues. In this process, the polar cap potential (PCP) decreases. Experimentally, it was shown many years ago that the energy stored in the magnetosphere begins to decay with a time constant of two hours. Here we use Poynting's theorem to calculate this time constant and find a result that is consistent with the data.https://www.ann-geophys.net/30/927/2012/angeo-30-927-2012.pdf |
| collection |
DOAJ |
| language |
English |
| format |
Article |
| sources |
DOAJ |
| author |
M. C. Kelley |
| spellingShingle |
M. C. Kelley On the relaxation of magnetospheric convection when <I>B</I><sub>z</sub> turns northward Annales Geophysicae |
| author_facet |
M. C. Kelley |
| author_sort |
M. C. Kelley |
| title |
On the relaxation of magnetospheric convection when <I>B</I><sub>z</sub> turns northward |
| title_short |
On the relaxation of magnetospheric convection when <I>B</I><sub>z</sub> turns northward |
| title_full |
On the relaxation of magnetospheric convection when <I>B</I><sub>z</sub> turns northward |
| title_fullStr |
On the relaxation of magnetospheric convection when <I>B</I><sub>z</sub> turns northward |
| title_full_unstemmed |
On the relaxation of magnetospheric convection when <I>B</I><sub>z</sub> turns northward |
| title_sort |
on the relaxation of magnetospheric convection when <i>b</i><sub>z</sub> turns northward |
| publisher |
Copernicus Publications |
| series |
Annales Geophysicae |
| issn |
0992-7689 1432-0576 |
| publishDate |
2012-06-01 |
| description |
The solar wind inputs considerable energy into the upper atmosphere,
particularly when the interplanetary magnetic field (IMF) is southward.
According to Poynting's theorem (Kelley, 2009), this energy becomes stored
as magnetic fields and then is dissipated by Joule heat and by energizing
the plasmasheet plasma. If the IMF turns suddenly northward, very little
energy is transferred into the system while Joule dissipation continues. In
this process, the polar cap potential (PCP) decreases. Experimentally, it
was shown many years ago that the energy stored in the magnetosphere begins
to decay with a time constant of two hours. Here we use Poynting's theorem
to calculate this time constant and find a result that is consistent with
the data. |
| url |
https://www.ann-geophys.net/30/927/2012/angeo-30-927-2012.pdf |
| work_keys_str_mv |
AT mckelley ontherelaxationofmagnetosphericconvectionwhenibisubzsubturnsnorthward |
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