SH41E-2412
Modeling of the solar cycle modulated interstellar He, Ne, and O pick-up ion flux along the Earth orbit

Thursday, 17 December 2015
Poster Hall (Moscone South)
Maciej Bzowski1, Justyna M Sokol1, Marzena A. Kubiak2 and Eberhard Moebius3, (1)Space Research Center Polish Academy of Sciences, Warszawa, Poland, (2)Space Research Center Polish Academy of Sciences, Warsaw, Poland, (3)University of New Hampshire, Institute for the Study of Earth, Oceans and Space, and Department of Physics, Durham, NH, United States
Abstract:
Interstellar pick-up ions (PUIs) are used to study in-situ the interstellar flow through the heliosphere. The locations of the peaks of the downwind focusing cone and the upwind crescent as observed in the PUI flux have been used as signatures for the flow direction of neutral interstellar (ISN) gas into the heliosphere. We study the modulation of interstellar He, Ne, and O PUI along the Earth orbit over almost the entire solar activity cycle from 2002 to 2013. We present the expected density of ISN atoms and the resulting PUI fluxes with their modulation due to varying ionization over the solar cycle. Considering the important role of the finite injection speed of ISN atoms and of adiabatic PUI cooling, we show that Ne and O always form an upwind crescent in the PUI flux, but that the crescent formation for He PUIs strongly depends on the integration boundaries for the PUI distribution. Because the crescent has been observed for all three species, we find that the classical model of PUI evolution by Vasyliunas & Siscoe (1976) may not be sufficient to reproduce the upwind structure of He PUIs. We also find that ecliptic longitude of the PUI peak in the focusing cone is a good proxy for the inflow direction of ISN He and Ne during solar minimum, but not for ISN O, which exhibits a systematic shift in the model. On the other hand, the peak location derived from the crescent may not be a good proxy to determine the inflow longitude because it is highly modulated by short-time (few months) variations in the ionization losses. These lead to a corrugated crescent structure and may shift the fitted position of the crescent peak used to determine the inflow direction by up to 10°, with the strongest effects for the species that are heavily affected by ionization, i.e., O and Ne. These findings are in a qualitative agreement with results of in-situ PUI measurements, which showed that the location of PUI maximum varies.