Large-scale Structure of the Chromospheric Doppler Velocities on the Solar Disk from 2D-spectroscopy within the He I 10830 Å Line

Details Large-scale Structure of the Chromospheric Doppler Velocities on the Solar Disk from 2D-spectroscopy within the He I 10830 Å Line Large-scale Structure of the Chromospheric Doppler Velocities on the Solar Disk from 2D-spectroscopy within the He I 10830 Å Line

Jan 2004

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2004soph..219...79k&link_type=abstract

Solar Physics, v. 219, Issue 1, p. 79-86 (2004).

Physics

1

Scientific paper

A distribution map of the large-scale chromospheric Doppler velocities on the solar disk for 5 June 2002 is presented. The map was obtained using a 2D-spectroscopy technique within the He i 10830 Å line. The spatial resolution of the map is about 30 arc sec. The map demonstrates a downflow in the chromosphere over active regions, especially significant around the spots and inside the plages. Positive Doppler velocities correspond to strong magnetic field areas, regardless of the field sign. Three major chromospheric outflow zones are observed: an equatorial and two polar ones. Each area of substantial negative Doppler velocities matches a zone of weak intensity of inner corona observed within the Fe ix-x 171 Å line by the SOHO spacecraft. A Doppler velocity histogram and the dependence of the Doppler velocities on the cosine of the heliocentric angle for the solar disk are calculated. The total mass outflow from the upper chromosphere is estimated as 2×1013 g s-1. Four percent of this amount is sufficient to produce the fast solar wind.

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