Physics
Scientific paper
Dec 2010
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2010agufmsh21b1810z&link_type=abstract
American Geophysical Union, Fall Meeting 2010, abstract #SH21B-1810
Physics
[2124] Interplanetary Physics / Heliopause And Solar Wind Termination, [2126] Interplanetary Physics / Heliosphere/Interstellar Medium Interactions, [2151] Interplanetary Physics / Neutral Particles
Scientific paper
Accurate and efficient modeling of the interactions between the solar wind (SW) and local interstellar medium (LISM) based on the creation of hydrogen energetic neutral atoms (ENAs) is essential for understanding the structure of the heliosphere. I have developed a numerical code that involves most known processes that contribute to the gains and losses of hydrogen ENAs from 1 AU to the heliopause. The code takes data from advanced 3D simulations of the SW-LISM interaction, and performs a post-processing analysis to determine the rates of charge-exchange between interstellar hydrogen and energetic protons to compute the flux of ENAs generated at all points in the heliosphere. Once created in the distant regions of the heliosphere, ENAs suffer losses as they propagate to the inner heliosphere. This includes effects of photo-ionization, charge-exchange, and electron-impact ionization. Additional effects, solar gravity and radiation pressure, alter the ENA's trajectory. By directly calculating gains and losses of hydrogen ENAs along lines of sight, an accurate, global picture of hydrogen ENA fluxes at 1 AU as predicted by the 3D simulation can be computed in a short time using modest computational resources. Not only can this method be implemented to predict ENA flux for energies relevant for NASA's IBEX mission (0.01 to 6 keV), but also for higher energy ranges such as those used by the Cassini/INCA and SOHO/CELIAS/HSTOF instruments. I will present maps of ENA flux computed using my code, along with data from various ENA missions, and predicted ENA maps obtained using a fundamentally different ENA model. An overview of the code and interpretation of results will also be provided.
Heerikhuisen Jacob
Pogorelov Nikolai V.
Zirnstein E. J.
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