Heliospheric energetic particle observations during the October-November 2003 superstorm events

Details Heliospheric energetic particle observations during the October-November 2003 superstorm events Heliospheric energetic particle observations during the October-November 2003 superstorm events

May 2004

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2004agusmsh33a..03l&link_type=abstract

American Geophysical Union, Spring Meeting 2004, abstract #SH33A-03

Physics

2102 Corotating Streams, 2111 Ejecta, Driver Gases, And Magnetic Clouds, 2114 Energetic Particles, Heliospheric (7514), 2139 Interplanetary Shocks

Scientific paper

We present a multi-spacecraft analysis of the energetic particle observations during the October-November 2003 ``superstorms'' period. We use energetic particle measurements from the following instruments: (1) the Low-Energy Magnetospheric Measurement System (LEMMS) on board the Cassini spacecraft, (2) the Heliosphere Instrument for Spectra, Composition and Anisotropy at Low-Energies (HI-SCALE) and the Cosmic Ray and Solar Particle Investigation (COSPIN) telescopes on board Ulysses, (3) the Electron, Proton and Alpha Monitor (EPAM) on board ACE and (4) the Energetic Particle Sensor (EPS) on board the GOES spacecraft. We combine energetic particle data with solar wind and magnetic field observations from the magnetometers and plasma instruments on board the respective spacecraft. The Cassini spacecraft was en route to Saturn, close to the ecliptic plane, at 8.7 AU from the Sun and less than 70 degrees west in longitude with respect to the Sun-Earth line. The Ulysses spacecraft was at 5.2 AU from the Sun, very close to the ecliptic plane, and 54 degrees to the west with respect to the Sun-Cassini line. Prior to the occurrence of these series of events, the structure of the inner heliosphere was well-organized by recurrent corotating high-speed streams. The intense solar events of October-November 2003 disturbed this stable structure, filling the inner heliosphere with energetic particles and sending a sequence of fast CMEs past the three spacecraft. In this paper we characterize the particle intensity enhancements seen at the three spacecraft and associate them with the solar wind disturbances traveling between the Sun and the spacecraft.

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