Physics
Scientific paper
May 2001
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2001agusm..sh22f05b&link_type=abstract
American Geophysical Union, Spring Meeting 2001, abstract #SH22F-05
Physics
2104 Cosmic Rays, 2111 Ejecta, Driver Gases, And Magnetic Clouds, 2134 Interplanetary Magnetic Fields, 2164 Solar Wind Plasma
Scientific paper
Voyager 2 (V2) observed at least three Merged Interaction Regions (MIRs) between January 1, 2000 and January 24, 2001, while it moved from 60 to 63 AU. The first MIR (MIR-1) was observed from approximately DOY 110 - 180, 2000. Its maximum magnetic field strength was approximately 0.24 nT, but the magnetic field strength fluctuated considerably indicating a highly structured MIR. The radial dimension was large, of the order of 17 AU, suggesting it might be a Global Merged Interaction Region. MIR-1 was associated with a significant step-decrease in the >70 MeV/n cosmic ray intensity. The second MIR (MIR-2) was observed from approximately DOY 330 - 352, 2000. Its magnetic fields were weaker and less variable than those of MIR-1. The maximum magnetic field strength in MIR-2 was approximately 0.18 nT, and its radial extent was only approximately 5 AU. MIR-2 was associated with a only a small decrease in the cosmic ray intensity, possibly owing to its small size and relatively weak magnetic fields. MIR-3 was observed from DOY 12, 2001 to at least DOY 24, 2001, and its radial extent was greater than 13 AU. The maximum magnetic field strength was approximately 0.17 nT, and the strong magnetic fields produced a moderate decrease in the cosmic ray intensity. MIR-3 was related to the "Bastille Day" event (July 14, 2000) at 1 AU. The density was relatively high in MIR-1 and to a lesser extent in MIR-2. There was no density enhancement in the part of MIR-3 that has been observed in the magnetic field data to date; we do not yet have magnetic field data for the interval of moderately enhanced density that followed DOY 24. The magnetic field strength enhancements in these three non-corotating MIRs are smaller than those typically observed by V2 closer to the sun during the previous solar cycle, possibly owing to the relatively high thermal pressure of pickup protons in the MIRs.
Burlaga Leonard Francis
McDonald Frank B.
Ness Norman F.
Richardson John D.
No associations
LandOfFree
Merged Interaction Regions Observed by Voyager 2 Between 60 and 63 AU does not yet have a rating. At this time, there are no reviews or comments for this scientific paper.
If you have personal experience with Merged Interaction Regions Observed by Voyager 2 Between 60 and 63 AU, we encourage you to share that experience with our LandOfFree.com community. Your opinion is very important and Merged Interaction Regions Observed by Voyager 2 Between 60 and 63 AU will most certainly appreciate the feedback.
Profile ID: LFWR-SCP-O-1274265