Origin of Quiet-Time Suprathermal Tails Near 1 AU

Details Origin of Quiet-Time Suprathermal Tails Near 1 AU Origin of Quiet-Time Suprathermal Tails Near 1 AU

Mar 2010

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2010aipc.1216..635d&link_type=abstract

TWELFTH INTERNATIONAL SOLAR WIND CONFERENCE. AIP Conference Proceedings, Volume 1216, pp. 635-638 (2010).

Astronomy and Astrophysics

Astronomy

1

Interplanetary Matter, Solar Wind, Solar Corona, Shock Waves, Astronomical Telescopes, Ejecta, Driver Gases, And Magnetic Clouds, Particle Emission, Solar Wind, Coronal Mass Ejection, Planetary Bow Shocks, Interplanetary Shocks, Ground-Based Ultraviolet, Optical And Infrared Telescopes

Scientific paper

We have surveyed the spectral and compositional properties of suprathermal (~40-320 keV nucleon-1) heavy ions during quiet times from 1995 January 1 to 2008 December 31 using instruments on board ACE and Wind spacecraft in the interplanetary (IP) medium near 1 AU. We find that the composition of the quiet-time suprathermal heavy ion population (3He and C-Fe) depends on the level of solar activity: the ions exhibit SEP-like composition signatures during solar maximum and CIR or solar-wind like composition during solar minimum. In addition, we find that during quietest times in the IP medium, all ion species exhibit suprathermal tails with power-law spectral indices ranging from 1.27 to 2.29, i.e., significantly different from recent observations and theoretical predictions of a unique 1.5 index. We discuss the implications of these new observations for the origin of the suprathermal ion population near 1 AU.

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