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a External view and b the view from the solar direction (Z).
The difference from the solar direction is controlled around 15° (at most, within 4 20°).
The baffle is an important component because the solar direction is not far away from the line of sight during the nightside observation.
However, Arase's spin axis, which is set nearly parallel to the Solar direction, enabled us to obtain probe potential data not contaminated by the shadow on the sphere probes caused by the spacecraft spin motion.
It is designed to reduce the solar contamination less than 2 × 10−6 of the initial when the solar direction is 26° or more away from the line of sight and within ±8° from the reference plane.
This phenomenon demonstrates that more particles arrive from the solar direction as the mean free path increases because hardly any energetic particles are scattered back from behind the Earth.
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The image obtained in our observation shows the sodium exosphere extended to the anti-solar direction.
The large baffle of the camera is very useful for IPD observations, because it provides us with very wide coverage in the solar elongation angle from 180° (anti-solar direction) to 30°.
If the SW is purely radial (flows in the anti-solar direction) and the Earth's dipole is perpendicular to the ecliptic plane (dipole tilt Ψ GSM angle between the Z GSM axis and Earth's dipole axis is zero), we expect to have a planar current sheet and north south symmetric field lines.
The aberration angle of the solar wind direction, due to the Martian orbital motion, is excluded in our study, which means that the solar wind direction is assumed to be along the Mars-Sun line.
The energy generated by the PV systems depends on the environmental conditions such as temperature, solar irradiance, direction and spectrum of sunlight (Singh 2013; Motahhir et al. 2015).
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