Empirical Densities, Kinetic Temperatures, and Outflow Velocities in the Equatorial Streamer Belt at Solar Minimum

Details Empirical Densities, Kinetic Temperatures, and Outflow Velocities in the Equatorial Streamer Belt at Solar Minimum Empirical Densities, Kinetic Temperatures, and Outflow Velocities in the Equatorial Streamer Belt at Solar Minimum

Jun 2002

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2002apj...571.1008s&link_type=abstract

The Astrophysical Journal, Volume 571, Issue 2, pp. 1008-1014.

Astronomy and Astrophysics

Astronomy

85

Sun: Solar Wind, Sun: Corona, Sun: Uv Radiation, Techniques: Spectroscopic

Scientific paper

We use combined Ultraviolet Coronagraph Spectrometer and Large Angle Spectroscopic Coronagraph data to determine the O5+ outflow velocities as a function of height along the axis of an equatorial streamer at solar minimum and as a function of latitude (at 2.3 Rsolar from Sun center). The results show that outflow increases rather abruptly in the region between 3.6 and 4.1 Rsolar near the streamer cusp and gradually increases to ~90 km s-1 at ~5 Rsolar in the streamer stalk beyond the cusp. The latitudinal variation at 2.3 Rsolar shows that there is no outflow (within the measurement uncertainties) in the center of the streamer, called the core, and that a steep increase in outflow occurs just beyond the streamer legs, where the O VI λ1032 intensity relative to H I λ1216 (Lyα) is higher than in the core. Velocity variations in both height and latitude show that the transitions from no measurable outflow to positive outflow are relatively sharp and thus can be used to infer the location of the transition from closed to open field lines in streamer magnetic field topologies. Such information, including the densities and kinetic temperatures derived from the observations, provides hard constraints for realistic theoretical models of streamers and the source regions of the slow solar wind.

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