On the Phase-Space Resolution for the Solar Wind Plasma Experiment on Board ESA-Solar Orbiter

Details On the Phase-Space Resolution for the Solar Wind Plasma Experiment on Board ESA-Solar Orbiter On the Phase-Space Resolution for the Solar Wind Plasma Experiment on Board ESA-Solar Orbiter

Dec 2002

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2002agufmsh21a0500d&link_type=abstract

American Geophysical Union, Fall Meeting 2002, abstract #SH21A-0500

Other

2164 Solar Wind Plasma, 2194 Instruments And Techniques, 7894 Instruments And Techniques

Scientific paper

Solar Orbiter is a space mission dedicated to study the solar surface, the corona and the solar wind by means of remote sensing and in-situ measurements, respectively. It will help us to understand in more detail the underlying nature of fundamental plasma kinetic processes acting in the Sun's atmosphere and in the extended corona as it will explore the inner regions of the Solar System with a perihelion of 0.21 AU. In particular, it will help us to understand the role of microinstabilities generated by non-Maxwellian features of the particle velocity distribution function. The best way to study these microinstabilities would be sampling the particle distribution function during their growth phase. In other words, we should be able to sample the whole 3-D velocity distribution function with a time resolution of the order of a few tens of msec, which is the time taken by the s/c to go across a scale length of the order of the typical Larmor gyroradius at 0.21 AU. This implies some restrictions on the maximum phase space resolution given a limited bit-rate for data transmission. In this paper we evaluate consequences of this limitation for solar wind distributions characterized by different values of the relative parameters.

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