Identification of the Coronal Sources of the Fast Solar Wind

Details Identification of the Coronal Sources of the Fast Solar Wind Identification of the Coronal Sources of the Fast Solar Wind

2000-01-14

arxiv.org/abs/astro-ph/0001257v1

Astronomy and Astrophysics

Astrophysics

14 pages, 4 figures, 3 tables, Accepted by ApJ Letters

Scientific paper

10.1086/312525

The present spectroscopic study of the ultraviolet coronal emission in a polar hole, detected on April 6-9, 1996 with the Ultraviolet Coronagraph Spectrometer aboard the SOHO spacecraft, identifies the inter-plume lanes and background coronal hole regions as the channels where the fast solar wind is preferentially accelerated. In inter-plume lanes, at heliocentric distance 1.7 \rsun, the corona expands at a rate between 105 km/s and 150 km/s, that is, much faster than in plumes where the outflow velocity is between 0 km/s and 65 km/s. The wind velocity is inferred from the Doppler dimming of the O VI $\lambda\lambda$ 1032, 1037 \AA lines, within a range of values, whose lower and upper limit corresponds to anisotropic and isotropic velocity distribution of the oxygen coronal ions, respectively.

Affiliated with

Also associated with

No associations

Rating

Identification of the Coronal Sources of the Fast Solar Wind 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 Identification of the Coronal Sources of the Fast Solar Wind, we encourage you to share that experience with our LandOfFree.com community. Your opinion is very important and Identification of the Coronal Sources of the Fast Solar Wind will most certainly appreciate the feedback.

Rate now

Comments { 0 }

Profile ID: LFWR-SCP-O-698150