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The Influence of Pickup Protons, from Interstellar Neutral Hydrogen, on the Propagation of Interplanetary Shocks from the Halloween 2003 Solar Events to ACE and Ulysses: A 3-D MHD Modeling Study
External Online Source: doi:10.1029/2010JA015803
Author and Affiliation:
Detman, T. R.(Carmel Research Center, Santa Monica, CA, United States);
Intriligator, D. S.(Carmel Research Center, Santa Monica, CA, United States);
Dryer, M.(Carmel Research Center, Santa Monica, CA, United States);
Sun, W.(Carmel Research Center, Santa Monica, CA, United States);
Deehr, C. S.(Carmel Research Center, Santa Monica, CA, United States);
Intriligator, J.(Carmel Research Center, Santa Monica, CA, United States)
Abstract: We describe our 3-D, time ]dependent, MHD solar wind model that we recently modified to include the physics of pickup protons from interstellar neutral hydrogen. The model has a time-dependent lower boundary condition, at 0.1 AU, that is driven by source surface map files through an empirical interface module. We describe the empirical interface and its parameter tuning to maximize model agreement with background (quiet) solar wind observations at ACE. We then give results of a simulation study of the famous Halloween 2003 series of solar events. We began with shock inputs from the Fearless Forecast real ]time shock arrival prediction study, and then we iteratively adjusted input shock speeds to obtain agreement between observed and simulated shock arrival times at ACE. We then extended the model grid to 5.5 AU and compared those simulation results with Ulysses observations at 5.2 AU. Next we undertook the more difficult tuning of shock speeds and locations to get matching shock arrival times at both ACE and Ulysses. Then we ran this last case again with neutral hydrogen density set to zero, to identify the effect of pickup ions. We show that the speed of interplanetary shocks propagating from the Sun to Ulysses is reduced by the effects of pickup protons. We plan to make further improvements to the model as we continue our benchmarking process to 10 AU, comparing our results with Cassini observations, and eventually on to 100 AU, comparing our results with Voyager 1 and 2 observations.
Publication Date: Mar 23, 2012
Document ID:
20130008807
(Acquired Feb 03, 2013)
Subject Category: SOLAR PHYSICS
Document Type: Journal Article
Publication Information: Journal of Geophysical Research; Volume 116; A03105
Contract/Grant/Task Num: NNX08AE40G
Financial Sponsor: NASA; Washington, DC, United States
Organization Source: Carmel Research Center; Santa Monica, CA, United States
Description: 12p; In English; Original contains color and black and white illustrations
Distribution Limits: Unclassified; Publicly available; Unlimited
Rights: Copyright
NASA Terms: HYDROGEN; INTERSTELLAR GAS; IONS; MAGNETOHYDRODYNAMICS; NEUTRAL GASES; PROTONS; SIMULATION; THREE DIMENSIONAL MODELS; SOLAR ACTIVITY; SOLAR ACTIVITY EFFECTS; SHOCK WAVES; ADVANCED COMPOSITION EXPLORER; HELIOSPHERE
Availability Source: Other Sources
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