Japan Geoscience Union Meeting 2019

Presentation information

[E] Poster

P (Space and Planetary Sciences ) » P-CG Complex & General

[P-CG21] Future Missions and instrumentation for space and planetary science

Sun. May 26, 2019 3:30 PM - 5:00 PM Poster Hall (International Exhibition Hall8, Makuhari Messe)

convener:Mitsunori Ozaki(Faculty of Electrical and Computer Engineering, Institute of Science and Engineering, Kanazawa University), Satoshi Kasahara(The university of Tokyo), Shingo Kameda(School of Science, Rikkyo University), Kazuo Yoshioka(Graduate School of frontier Science, The University of Tokyo)

[PCG21-P18] Observation Plans in the Cruising-Phase of the Solar Power Sail: OKEANOS

*Takahiro Iwata1, Shuji Matsuura2, KOHJI TSUMURA3, Hajime Yano1, Takayuki Hirai4, Ayako Matsuoka1, Daisuke Yonetoku5, Tatehiro Mihara6, Tatsuaki Okada1, Osamu Mori1, Toshihiro Chujo1 (1.Institute of Space and Astronautical Science, Japan Aerospace Exploration Agency, 2.Kwansei Gakuin University, 3.Tohoku University, 4.Chiba Institute of Technology, 5.Kanazawa University, 6.RIKEN)

Keywords:OKEANOS, zodiacal light, dust, plasma, gamma-ray

The solar power sail mission: OKEANOS (Oversize Kite-craft for Exploration and AstroNautics in the Outer Solar system) is a Japanese candidate deep-space probe that will be powered by hybrid propulsion of solar photon acceleration and ion engines. The main scientific objectives are studies of Trojan asteroids in the Jovian L4 or L5 regions. The long distance and period from the launch to the swing-by at Jupiter will give us a good opportunity to explore the solar system between the Earth and the Jupiter to elucidate the solar system disc structure. We define the cruising-phase sciences of the OKEANOS mission as the scientific theme that will be explored or observed from the launch to the swing-by at Jupiter. Candidates of instruments for the cruising phase are: the EXo-Zodiacal Infrared Telescope (EXZIT), the Arrayed Large-area Dust detectors in INterplanetary space (ALADDIN)-2, the MaGnetic Field experiment (MGF), and the GAmma-ray burst Polarimeter (GAP)-2. In this paper, we report scientific purpose and observation plans of them.

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.