Voyager 2 Signatures of Important Processes/Dynamics in the Outer Heliosphere

Details Voyager 2 Signatures of Important Processes/Dynamics in the Outer Heliosphere Voyager 2 Signatures of Important Processes/Dynamics in the Outer Heliosphere

Dec 2011

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2011agufmsh11a1916i&link_type=abstract

American Geophysical Union, Fall Meeting 2011, abstract #SH11A-1916

Physics

[2124] Interplanetary Physics / Heliopause And Solar Wind Termination, [2126] Interplanetary Physics / Heliosphere/Interstellar Medium Interactions, [2152] Interplanetary Physics / Pickup Ions, [2164] Interplanetary Physics / Solar Wind Plasma

Scientific paper

We continue investigating the Voyager 2 (V2) Plasma Subsystem (PLS) elevated readings in L-mode on energy/unit charge (E/Q) step 12 on the B-Cup we first reported (Intriligator et al., JGR, 2010) near the termination shock at 84 AU. These elevated B12 readings, which we previously referred to as "high energy ions (HEIs)", are found in the V2 PLS data on the sunward facing B-Cup at E/Q step 12 corresponding to 1610 volts and a proton speed of ~ 600 km/s. In the present paper we update our findings and present V2 data from three years earlier when V2 was in the solar wind in the outer heliosphere (OH) at 73 AU measuring the interplanetary (IP) effects from the October-November (Halloween) 2003 solar events. We also examine other V2 OH time intervals. We show links between solar activity and the elevated B12 readings in the V2 data. We present evidence that these elevated B12 readings appear to be accompanied by significant simultaneous changes in other V2 measurements, including: low energy ions, low energy cosmic rays, anomalous cosmic rays, cosmic ray electrons, interplanetary magnetic field (IMF), and convective solar wind plasma. Our results suggest that the V2 elevated B12 readings may be signatures, tracers, by-products, or indicators of important IP processes such as those associated with intervals of particle acceleration, changes in IMF turbulence, and perhaps local reconnection. This work was funded by NASA Grant NNX08AE40G and by Carmel Research Center, Inc.

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