Characterization of the slow wind in the outer corona

Details Characterization of the slow wind in the outer corona Characterization of the slow wind in the outer corona

2010-08-26

arxiv.org/abs/1008.4452v2

Astronomy and Astrophysics

Astrophysics

Solar and Stellar Astrophysics

5 figures, work presented with an oral presentation on 37th COSPAR Scientific Assembly, 13 - 20 July 2008, Montreal, Canada

Scientific paper

10.1016/j.asr.2010.08.008

The study concerns the streamer belt observed at high spectral resolution during the minimum of solar cycle 22 with the Ultraviolet Coronagraph Spectrometer (UVCS) onboard SOHO. On the basis of a spectroscopic analysis of the O VI doublet, the solar wind plasma parameters are inferred in the extended corona. The analysis accounts for the coronal magnetic topology, extrapolated through a 3D magneto-hydrodynamic model, in order to define the streamer boundary and to analyse the edges of coronal holes. The results of the analysis allow an accurate identification of the source regions of the slow coronal wind that are confirmed to be along the streamer boundary in the open magnetic field region.

Affiliated with

Also associated with

No associations

Rating

Characterization of the slow wind in the outer corona 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 Characterization of the slow wind in the outer corona, we encourage you to share that experience with our LandOfFree.com community. Your opinion is very important and Characterization of the slow wind in the outer corona will most certainly appreciate the feedback.

Rate now

Comments { 0 }

Profile ID: LFWR-SCP-O-704033