[PCG21-P13] Investigation of the Solar System Structure using the Solar Power Sail: OKEANOS
Keywords:OKEANOS, solar system disc, zodiacal light, dust, plasma
Zodiacal light observed at visible and near-infrared wavelengths is thought to be sunlight scattered by interplanetary dust. The two-dimensional distribution of zodiacal light reflects the three-dimensional structure of interplanetary dust. However, it is still controversial that how the ratio of asteroid-origin to comet-origin changes by the heliocentric distance. Therefore, the comparison of the radial distribution of zodiacal light and the in-situ dust observation will help clarify the distribution and components of solid particles in our solar system. These results are expected to provide precise distribution of the interplanetary dust in our solar-system discs.
The temperature of the solar wind, which depends on the heliocentric distance, has been observed to be greater than that predicted by the adiabatic model. Therefore, the existence of heating processes, such as plasma turbulence or magnetic reconnection, could be predicted. The observation of the magnetic field by the devices separated in the scale of the membrane of the Solar Power Sail provides the resolution of the plasma turbulence on the electron scale. Thus, the intermittent observation of the magnetic field between the Earth and Jupiter would determine the heating mechanism of the solar wind. The synergy of the magnetic field and dust observation may show the interaction between interplanetary dust and solar wind. By analyzing the environments on the dust surface, the chemical evolutions of molecules caused by solar wind and cosmic radiation can be investigated. We are investigating the possibilities to detect gamma-rays and particles from the solar-system shocks.