Physics
Scientific paper
Dec 1998
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1998natur.396..440z&link_type=abstract
Nature, Volume 396, Issue 6710, pp. 440-441 (1998).
Physics
112
Scientific paper
Solar prominences are sheets of relatively cool and dense gas embedded in the surrounding hotter corona. An erupting prominence can inject a mass of up to 1015g into the solar wind as part of a coronal mass ejection. These eruptions must depend critically on the topology of the prominence's magnetic field. In all present models,, the prominence hangs on horizontal or helical field lines, while an overlying magnetic arcade temporarily restrains the prominence from erupting. Such models are inconsistent, however, with the slow upward vertical gas flows that are seen in prominences. Here we report counter-streaming flows along closely spaced vertical regions of a prominence, between its top and the lower solar atmosphere. As the flows must be aligned with the magnetic field, this observation implies that a field connects the prominence directly to the photosphere, contrary to all existing models. These magnetic `tethers' might help prevent a prominence from erupting.
Engvold Odbjørn
Martin Sara F.
Zirker Jack B.
No associations
LandOfFree
Counter-streaming gas flows in solar prominences as evidence for vertical magnetic fields does not yet have a rating. At this time, there are no reviews or comments for this scientific paper.
If you have personal experience with Counter-streaming gas flows in solar prominences as evidence for vertical magnetic fields, we encourage you to share that experience with our LandOfFree.com community. Your opinion is very important and Counter-streaming gas flows in solar prominences as evidence for vertical magnetic fields will most certainly appreciate the feedback.
Profile ID: LFWR-SCP-O-763426