Ion Effective Temperatures in Polar Coronal Holes: Observations versus Ion-Cyclotron Resonance

Details Ion Effective Temperatures in Polar Coronal Holes: Observations versus Ion-Cyclotron Resonance Ion Effective Temperatures in Polar Coronal Holes: Observations versus Ion-Cyclotron Resonance

Dec 2002

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2002apj...581l.125p&link_type=abstract

The Astrophysical Journal, Volume 581, Issue 2, pp. L125-L127.

Astronomy and Astrophysics

Astronomy

6

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

Scientific paper

The resonant cyclotron interaction between ion-cyclotron waves and solar wind species is considered nowadays to be a strong candidate for heating and acceleration of protons, α-particles, and heavy ions. A crucial physical parameter for determining the amount and the location of significant heating and acceleration, which the different solar wind ions receive from the waves in the frame of the ion-cyclotron mechanism, is their charge-to-mass ratio q/m. Therefore, comparisons of ion temperatures derived from spectroscopic observations and calculated by ion-cyclotron models, for ions that span a broad range in q/m, would provide a rigorous test for such models. By using an ion-cyclotron model, we calculate the effective temperatures for 10 different ions that cover the range 0.16-0.37 in q/m. Effective temperatures correspond to unresolved thermal motions and wave motions. The good agreement between our calculations, based on the specific mechanism that we employed here (ion-cyclotron resonance) and on spectroscopic observations of effective temperatures in polar coronal holes, provides support that the above mechanism accounts for the energetics and kinematics of fast solar wind heavy ions. However, such an agreement does not prove that other potential mechanisms can be excluded.

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