Observations of Suprathermal Power Law Tails with ACE, Ulysses, MESSENGER, and Voyager

Details Observations of Suprathermal Power Law Tails with ACE, Ulysses, MESSENGER, and Voyager Observations of Suprathermal Power Law Tails with ACE, Ulysses, MESSENGER, and Voyager

Dec 2007

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2007agufmsh51b..02g&link_type=abstract

American Geophysical Union, Fall Meeting 2007, abstract #SH51B-02

Physics

7509 Corona, 7513 Coronal Mass Ejections (2101), 7514 Energetic Particles (2114), 7531 Prominence Eruptions, 7984 Space Radiation Environment

Scientific paper

Observations of ubiquitous, suprathermal power law tails with the unique spectral index of -5 on the velocity distributions of solar wind and pickup ions raise important questions and have far reaching consequences. The question of how these tails are formed during quiet times, when no shocks are present, was previously addressed and is briefly reviewed here. One consequence of the existence of these tails during quiet times is that sufficiently energetic particles are always readily available for further acceleration by shocks. To study the evolution of suprathermal tails over a large range of heliocentric distances, we will use proton spectra measured with ACE, Ulysses and Voyager during quiet times as well as upstream and downstream of quasi-stationary and traveling shocks. To look for the first time at suprathermal tails at distances closer to the Sun than 1 AU, we will present our preliminary results from the FIPS instrument on the Mercury MESSENGER Mission. Applying thermodynamic constraints on non-adiabatic heating of upstream particles by a shock, we obtain the downstream -5 power law spectra that are observed and derive an expression for the tail pressure jump across the shock.

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