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- Direct exploration of Phobos was attempted by Phobos 1 (1988), Phobos 2 (1988–1989), and Phobos-Grunt (2011), but they failed except for limited data acquisition by Phobos 2 in the vicinity of Phobos (Duxbury et al. 2014 for a comprehensive summary of the past explorations of Phobos and Deimos).
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Three missions to land on Phobos have been launched; the Phobos program in the late 1980s saw the launch of Fobos 1 and Fobos 2, while the Fobos-Grunt sample return mission was launched in 2011. None of these missions were successful: Fobos 1 failed en route to Mars, Fobos 2 failed shortly before landing, and Fobos-Grunt never left low Earth ...
Feb 11, 2021 · Phobos-Grunt: (FAILED) Russia, launched Nov. 8, 2011 on a mission to return samples from the Mars moon Phobos. The $163 million robotic probe suffered a crippling malfunction shortly after...
- Mirs
- Orochi and Tengoo
- Megane
- MSA
- CMDM
- Lidar
QSO-H
One of MIRS objectives is to provide a spectral mapping as global as possible to determine Phobos’ surface composition and thermal inertia. Considering MIRS cross-track field-of-view of 3.3° and maximum Phobos polar angle from QSO-H of 10° (Table 1), three complete longitudinal coverages are necessary to obtain a global mapping, one with each of the cross-track angles − 3°, 0°, and 3°. Settings of current QSO-H are such that Sun-Phobos-Spacecraft angle is below 90° (i.e., spacecraft is locate...
QSO-M
For QSO-M we consider that five complete longitudinal coverages are necessary to obtain a global mapping by MIRS, one with each of the cross-track angles − 6, − 3°, 0°, 3°, and 6°. We add one longitudinal coverage to cover cross-track angles − 9° and 9° but only on half of the longitudes (around longitudes 0° and 180°) where Phobos polar angle is maximum. Figure 7b shows that around 90% of Phobos surface could be covered with a phase angle close to 10°. This value is better than that for QSO-...
QSO-Ls
The main objective on these QSOs is to characterize the landing site candidates as precisely as possible (Fig. 8a). The proximity to Phobos is an advantage for geometric resolution but it reduces the capacity to observe high latitude area. Also, the lower-altitude orbit has higher ground speed on Phobos (Fig. 8b) and in this case the MIRS along-track scanner will be used during observations to reduce the ground speed of MIRS line of sight projection on Phobos so that it is compatible with the...
QSO-H
Similar to MIRS, OROCHI observation aims to provide a global spectroscopic mapping by seven cameras with different band-pass filters with sufficient signal to noise level (> 100, Kameda et al. 2021) to understand visible spectral variation and material distribution of Phobos. Because OROCHI has a wide field of view (Table 2), each image can cover from south to north polar regions from QSO-H and at the same time OROCHI observes Phobos with a sufficient spatial resolution similar to MIRS (Fig....
QSO-M
For QSO-M, OROCHI will observe all latitudes of Phobos simultaneously with the same geometric resolution as MIRS (Fig. 7) and acquire spectral data at the same local time and phase angles as MIRS with a better spatial resolution than that from QSO-H. This makes it possible to connect OROCHI and MIRS spectra, and to obtain continuous visible and near-infrared spectra of each region of Phobos for more accurate identification of materials on the surface. TENGOO will be used also for constructing...
QSO-Ls
For TENGOO and OROCHI, the main observation objective on QSO-LA, LB, and LC is to characterize topographic and spectral features of the landing site candidates as precisely as possible for safe landing on a scientifically important site. From the viewpoint of the safe landing, TENGOO is the most important instrument because of its higher resolution to identify possible hazardous objects on the surface of Phobos. At 20 km altitude which is a typical altitude of QSO-LA, TENGOO resolution is 12...
QSO-H
During QSO-H, MEGANE will acquire measurements for the purpose of characterizing the gamma-ray and neutron background. These MEGANE background measurements are planned to occur for a duration of 15 days, both before and after MEGANE’s prime science measurements in the lower-altitude QSO-LB and QSO-LC. The MEGANE background measurements will occur simultaneously with other science observations. At QSO-M, no specific observation plan is scheduled.
QSO-Ls
During the lowest altitude QSO phase of the MMX mission, MEGANE will obtain gamma-ray and neutron measurements. These MEGANE measurements will determine the composition of Phobos and will contribute to determining Phobos’ formation and to understanding the processes that have affected the moon’s surface (Lawrence et al. 2019). The key measurements to be obtained by MEGANE during the low-altitude QSO phase of the MMX mission in 2026 are listed in Table 4. In addition to the required measuremen...
QSO-H
The Mass Spectrum Analyzer (MSA) consists of an ion energy mass spectrometer and two magnetometers, which measure velocity distribution functions and mass/charge distributions of low-energy ions and the magnetic field of the solar wind, respectively (Yokota et al. 2021). The MSA will perform in-situ observations of all the ions going towards and coming from Phobos to investigate the Phobos surface and related phenomena (e.g., space weathering). Figure 14 schematically shows the MSA observatio...
QSO-M
The MSA observation in the QSO-M is the same as that in the QSO-H, especially for solar wind ions. However, the opportunity of observing scattered solar wind ions and secondary ions from Phobos will increase as the distance between the spacecraft and Phobos decreases. Observations of scattered solar wind ions provide more information about the ions immediately after their scattering. The observation in the QSO-M increases the possibility of {\varvec{E}}directing from Phobos to the spacecraft...
QSO-Ls
In the QSO-LA, LB, and LC, the MSA will derive much more information on the Phobos surface from the observation of scattered solar wind ions and secondary ions from Phobos. The possibility of adequate {\varvec{E}} to observe secondary ions from Phobos in the QSO-Ls goes up to 10 s % for the spacecraft around the terminator. Thus, the QSO-Ls will ensure the observation period especially for secondary ions from Phobos. Moreover, the MSA observation in the QSO-Ls will provide the distribution ma...
The CMDM consists of a sensor with a sensitive area of 1 m2 and an electronics box, which measures the collisional momentum with which a dust particle impacts the sensor of the CMDM (Kobayashi et al. 2018) and its only observation mode is to wait for the signal from the dust particles in orbit to collide with the sensor. The main objective of the C...
The spatial resolution of LIDAR observation is decided by the laser footprint size on the Phobos’ surface. Because the beam divergence of LIDAR laser is 0.5 mrad (Table 2), the laser footprint size becomes 50 m when the altitude of spacecraft is 100 km (QSO-H), and less than 10 m when the altitude of spacecraft is below 20 km (QSO-L). From QSO-H, L...
- Tomoki Nakamura
Phobos 2 was designed to orbit Mars and land a "hopper" and a lander on the surface of Phobos. The spacecraft successfully went into orbit and began sending back preliminary data.
Jan 20, 2022 · To reveal the origin of the Martian moons and elucidate the evolution of Mars and the habitable terrestrial planets in the Solar System, the MMX mission has selected Phobos as the target for sampling and thus for detailed observations.
Nov 8, 2011 · Phobos-Grunt was be Russia's first interplanetary mission since the unsuccessful Mars 96 mission. After an 11-month voyage to Mars, Phobos-Grunt was to begin probing Mars' magnetosphere and atmosphere.
Sep 13, 2022 · Phobos 2 successfully entered orbit around Mars on Jan. 29, 1989, and returned 37 detailed images of Phobos, mapping 80% of the moon. Shortly before the deployment of the lander and hopper, the main computer aboard Phobos 2 failed, and the mission ended prematurely on March 27.
