Studying Coronal Holes through Observations of an HeI Infrared Line and the Halpha Line

Details Studying Coronal Holes through Observations of an HeI Infrared Line and the Halpha Line Studying Coronal Holes through Observations of an HeI Infrared Line and the Halpha Line

Jun 2000

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2000arep...44..401k&link_type=abstract

Astronomy Reports, Volume 44, Issue 6, June 2000, pp.401-406

Astronomy and Astrophysics

Astronomy

Scientific paper

New results from electrophotometric scanning of the solar disk in the HeI λ 10830 Å and Hα lines are presented. The intensity at the center of the HeI λ 10830.30 Å line is 1 3% higher in the regions of coronal holes than in quiescent regions; this is accompanied by a decrease in the size and contrast of the chromospheric network compared to the network in quiescent regions. Our observations in the HeI line revealed chains of “dark points” surrounding coronal holes. The Hα±0.5 observations show increased velocities of ascent near the dark points compared to the velocities inside coronal holes and in quiescent regions. It is proposed that the intensification and acceleration of the flows of solar plasma from the dark points are due to reconnection of the magnetic fields of the bipolar chromospheric network and the predominantly unipolar magnetic field inside the coronal holes. Our observations suggest that the same reconnection process takes place near the temperature minimum, in the presence of certain conditions at the boundary between coronal holes and bipolar active regions. The reconnection process produces plasma flows from the chromosphere to the corona, which are sufficient to form prominences.

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