Signatures of the July 2000 Solar Disturbances Observed at Voyagers 1 and 2 during 2001

Details Signatures of the July 2000 Solar Disturbances Observed at Voyagers 1 and 2 during 2001 Signatures of the July 2000 Solar Disturbances Observed at Voyagers 1 and 2 during 2001

Dec 2001

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2001agufmsh41b0751d&link_type=abstract

American Geophysical Union, Fall Meeting 2001, abstract #SH41B-0751

Other

2104 Cosmic Rays, 2114 Energetic Particles, Heliospheric (7514), 2139 Interplanetary Shocks, 7514 Energetic Particles (2114), 7807 Charged Particle Motion And Acceleration

Scientific paper

Intense solar activity during July 2000 (including the well-documented July 14, Bastille Day, geomagnetic storm) produced high intensities of energetic particles and multiple large-scale solar wind disturbances at 1AU. These disturbances coalesced into a complex global merged interaction region (GMIR) that passed the Voyagers in early 2001 [1,2]. We discuss the effects this GMIR had on energetic (>0.5 MeV) proton intensities measured by the LECP (Low Energy Charged Particle) instruments on Voyagers 1 (V1) and 2 (V2). The shock at the forward edge of the GMIR passed V2 (63AU, 22° S) on 2001 DOY 12 (2001.03), with observed properties in excellent agreement with predictions [3]. The shock evidently swept up and accelerated ≈3-20 MeV ACR protons that began to increase some two weeks before the shock's passage. However, the ≈0.5-1.5 MeV protons peaked ~15 days after the shock arrival (with a time width ~30 days), due possibly to the shock's progressive weakening, which reduced its ability to accelerate ambient protons as it propagated outward. The GMIR evidently reached V1 (80.5AU, 33.7° N) ~60 days later (on 2001.2), based on Forbush decreases observed in the intensities of ACR and GCR protons >20 MeV; it is not clear if there was a leading shock at V1. At V1 the intensity increase of ≈0.5-1.5 MeV protons was a factor ~2 less than that at V2, but had a time duration ~2 times longer than that at V2. These, as well as other differences in the intensity-time profiles of >0.5 MeV protons observed at V2 and V1 are not unexpected, particularly in view of the ~60° latitudinal separation of the two spacecraft. [1] Krimigis et al., Proc. of ICRC 2001, 3637-3640 (2001). [2] McDonald et al., Proc. of ICRC 2001, 3607-3610 (2001). [3] Wang et al., J. Geophys. Res. 106, 13,007-13,013 (2001).

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