Empirically Determined Anisotropic Velocity Distributions and Outflows of O5+\ ions in a Coronal Streamer at Solar Minimum

Details Empirically Determined Anisotropic Velocity Distributions and Outflows of O5+\ ions in a Coronal Streamer at Solar Minimum Empirically Determined Anisotropic Velocity Distributions and Outflows of O5+\ ions in a Coronal Streamer at Solar Minimum

May 2002

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2002agusmsh21b..06f&link_type=abstract

American Geophysical Union, Spring Meeting 2002, abstract #SH21B-06

Astronomy and Astrophysics

Astrophysics

7509 Corona, 7549 Ultraviolet Emissions

Scientific paper

Empirical constraints on the O5+\ velocity distributions and outflow speeds in a solar minimum equatorial streamer between 2.6 and 5.1 Rsun\ are determined using a spectral synthesis code that includes O VI Doppler dimming. These constraints follow directly from UV spectra taken on 12 October 1996 with the Ultraviolet Coronagraph Spectrometer (UVCS) on the SOHO satellite and 3D electron densities derived from tomography applied to a time series of polarized white-light images taken with the Large Angle Spectrometric Coronagraph Experiment (LASCO) on SOHO. Four conclusions result from this work: 1) Our analysis shows O5+\ anisotropy in the streamer legs and stalk. The microscopic velocity distribution (which excludes wave motions that equally affect all charged particles) is also found to be anisotropic, where the most probable speed perpendicular to the magnetic field direction exceeds that in the parallel direction. 2) There is no evidence of such anisotropy in the streamer core. 3) There is preferential heating of the O5+ions over the protons in the streamer stalk and legs, but not in the core. 4) The outflow velocity of the O5+\ ions is determined at heights above 4.6 Rsun. This work is supported by NASA under grant NAG5-10093 to the Smithsonian Astrophysical Observatory.

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