9:00 AM - 9:15 AM
[PPS09-01] Progress of Martian Moons eXploration MMX for launch in 2026
Keywords:Martian moons exploration, Phobos, Deimos, sample return, Martian atmosphere
The development and preparation for the Martian Moons eXploration (MMX), the world's first sample return mission from a Martian moon, is progressing steadily toward its launch in the fall of 2026 and return to Earth in 2031. The primary scientific objectives of MMX are to elucidate the origin of Phobos and Deimos, the processes of water and volatile acquisition by rocky planets associated with material transport across the early solar system, and the evolution of the Mars atmosphere and surface environment through the integrated analysis of close-up and in-situ observations taken during the three-year stay in the Martian sphere and the advanced analyses of returned samples from Phobos. MMX was scheduled to launch in 2024, but delays in the development of the launch vehicle have pushed the overall schedule back by about two years. As MMX was originally designed to accommodate the 2026 launch case also, there are no changes to the spacecraft and onboard instruments as a result of the launch postponement. Currently, the spacecraft system, consisting of the propulsion module, the return module, and the exploration module, is being assembled, and various comprehensive tests are being conducted in sequence. At the same time, the ground system, including control, communication, tracking, data processing, and coordination with overseas stations, is also being developed.
The new operations plan after the 2026 launch is also being developed extensively. The landing operation, which aims to collect more than 10 grams of samples from two sites on Phobos, is planned to take place in the middle of MMX's three-year stay in the Martian sphere. This is because 1) Mars will be closer to the Earth during this period, which will minimize the delay in communication between the ground station and the spacecraft, 2) the spacecraft on landing will have good conditions for solar illumination and visibility to the Earth during this period, and 3) there will be a later operation window for a recovery landing after the contingency case of an unsuccessful landing. The pre-landing period in the Martian sphere will be devoted primarily to observations and analyses for landing site selection, both for the rover and the parent spacecraft. Based on the current knowledge of surface slope, solar illumination, Earth visibility, etc., several tens of landing candidate areas on Phobos will be assigned in advance. Then, MMX will perform close-up imaging at various altitudes and phase angle conditions and spectroscopic observations to constrain material distribution, to select the landing sites that satisfy both landing safety and the scientific value of the samples.
Scientific observation data of Phobos acquired by the telescope camera TENGOO, laser rangefinder LIDAR, wide-angle visible-band camera OROCHI, infrared spectroscopic imaging camera MIRS, neutron gamma-ray spectrometer MEGANE, mass spectrometer MSA, dust monitor CMDM, and rover IDEFIX will be fully accumulated during and after the landing operation period. The origin and evolution of Phobos will then be elucidated from these close-up and in-situ observation data, independently of sample analyses. Flyby observations of Deimos will be made immediately after the Mars orbit insertion and before the Mars orbit escape. Data from these observations, consisting of imaging, visible-band spectroscopy, and infrared spectroscopy, will be used to constrain the origin and evolution of Deimos in comparison with Phobos. In addition, MMX will conduct observations of the Martian atmosphere during these periods and between Phobos observations to study the transport processes of dust and water in the Martian atmosphere. Data taken by the mass spectrometer, which monitors the masses, kinetic energies, and motion directions of ions in the spacecraft orbit will also reveal the escape processes of the Martian atmosphere and constrain the evolution of the Martian surface environment.
The new operations plan after the 2026 launch is also being developed extensively. The landing operation, which aims to collect more than 10 grams of samples from two sites on Phobos, is planned to take place in the middle of MMX's three-year stay in the Martian sphere. This is because 1) Mars will be closer to the Earth during this period, which will minimize the delay in communication between the ground station and the spacecraft, 2) the spacecraft on landing will have good conditions for solar illumination and visibility to the Earth during this period, and 3) there will be a later operation window for a recovery landing after the contingency case of an unsuccessful landing. The pre-landing period in the Martian sphere will be devoted primarily to observations and analyses for landing site selection, both for the rover and the parent spacecraft. Based on the current knowledge of surface slope, solar illumination, Earth visibility, etc., several tens of landing candidate areas on Phobos will be assigned in advance. Then, MMX will perform close-up imaging at various altitudes and phase angle conditions and spectroscopic observations to constrain material distribution, to select the landing sites that satisfy both landing safety and the scientific value of the samples.
Scientific observation data of Phobos acquired by the telescope camera TENGOO, laser rangefinder LIDAR, wide-angle visible-band camera OROCHI, infrared spectroscopic imaging camera MIRS, neutron gamma-ray spectrometer MEGANE, mass spectrometer MSA, dust monitor CMDM, and rover IDEFIX will be fully accumulated during and after the landing operation period. The origin and evolution of Phobos will then be elucidated from these close-up and in-situ observation data, independently of sample analyses. Flyby observations of Deimos will be made immediately after the Mars orbit insertion and before the Mars orbit escape. Data from these observations, consisting of imaging, visible-band spectroscopy, and infrared spectroscopy, will be used to constrain the origin and evolution of Deimos in comparison with Phobos. In addition, MMX will conduct observations of the Martian atmosphere during these periods and between Phobos observations to study the transport processes of dust and water in the Martian atmosphere. Data taken by the mass spectrometer, which monitors the masses, kinetic energies, and motion directions of ions in the spacecraft orbit will also reveal the escape processes of the Martian atmosphere and constrain the evolution of the Martian surface environment.