The meteoroid environment and impacts on Phobos

Christou, Apostolos; Oberst, J.; Lupovka, V.; Dmitriev, V.; Gritsevich, Maria

doi:10.1016/j.pss.2013.07.012

Cited by 10 publications

(9 citation statements)

References 35 publications

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“…Though these are likely the most common impactor, comets are also possible. Long-period comets impact at typical speeds of 40 km/s, and Jupiter-Family comets, 20 km/s Christou et al (2014). These high impact speeds imply that the ejection of material from the martian moons to escape speeds is possible.…”

Section: Discussionmentioning

confidence: 99%

Meteorites from Phobos and Deimos at Earth?

Wiegert

Galiazzo

2017

Planetary and Space Science

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We examine the conditions under which material from the martian moons Phobos and Deimos could reach our planet in the form of meteorites. We find that the necessary ejection speeds from these moons (900 and 600 m/s for Phobos and Deimos respectively) are much smaller than from Mars' surface (5000 m/s). These speeds are below typical impact speeds for asteroids and comets (10-40 km/s) at Mars' orbit, and we conclude that the delivery of meteorites from Phobos and Deimos to the Earth can occur.

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Section: Discussionmentioning

confidence: 99%

Meteorites from Phobos and Deimos at Earth?

Wiegert

Galiazzo

2017

Planetary and Space Science

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“…Mars and its satellites should also intersect a number of meteoroid streams produced by comets. However, the predicted timing and geometry of the stream encounters (see Christou et al, (2014) and references therein) have not been observationally confirmed to-date. Such streams affect the Martian upper atmosphere in a measurable way (Grebowsky et al, 2002;Molina-Cuberos et al, 2003), as was directly observed during the recent close encounter of comet C/Siding Spring with Mars.…”

Section: Meteoroid Flux From Crater Statistics and Dust Impact Detectmentioning

confidence: 99%

“…Small and large meteoroids from various solar system sources intercept the Martian satellite system, as attested by the large numbers of impact craters on Mars, Phobos, and Deimos. While the impact craters represent a powerful tool to study surface ages, craters can also be used to study the characteristics of the impactor population (Christou et al, 2014). As Phobos and Deimos are both locked in their orbits, impact rates and speeds vary across the surfaces of the satellites.…”

Section: Meteoroid Flux From Crater Statistics and Dust Impact Detectmentioning

confidence: 99%

“…As Phobos and Deimos are both locked in their orbits, impact rates and speeds vary across the surfaces of the satellites. Christou et al, (2014) simulated the production of craters on Phobos from the sporadic flux of Marscrossing asteroids and comets predicting a significant difference in the crater production rate on the leading and trailing hemisphere of Phobos. While the current crater statistics (limited by strong observational biases in the image data) do not support such a difference, accurate global crater counts by DePhine down to the smallest sizes will constrain this important effect.…”

Section: Meteoroid Flux From Crater Statistics and Dust Impact Detectmentioning

confidence: 99%

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DePhine – The Deimos and Phobos Interior Explorer

Oberst

Wickhusen

Willner

et al. 2018

Advances in Space Research

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DePhine -Deimos and Phobos Interior Explorer -is a mission proposed in the context of ESA's Cosmic Vision program, for launch in 2030. The mission will explore the origin and the evolution of the two Martian satellites, by focusing on their interior structures and diversity, by addressing the following open questions: Are Phobos and Deimos true siblings, originating from the same source and sharing the same formation scenario? Are the satellites rubble piles or solid bodies? Do they possess hidden deposits of water ice in their interiors? The DePhine spacecraft will be inserted into Mars transfer and will initially enter a Deimos quasi-satellite orbit to carry out a comprehensive global mapping. The goal is to obtain physical parameters and remote sensing data for Deimos comparable to data expected to be available for Phobos at the time of the DePhine mission for comparative studies. As a highlight of the mission, close flybys will be performed at low velocities, which will increase data integration times, enhance the signal strength and data resolution. 10 -20 flyby sequences, including polar passes, will result in a dense global grid of observation tracks. The spacecraft orbit will then be changed into a Phobos resonance orbit to carry out multiple close flybys and to perform similar remote sensing as for Deimos. The spacecraft will carry a suite of remote sensing instruments, including a camera system, a radio science experiment, a high-frequency radar, a magnetometer, and a Gamma Ray / Neutron Detector. A steerable antenna will allow simultaneous radio tracking and remote sensing observations (which is technically not possible for Mars Express). Additional instrumentation, e.g. a dust detector and a solar wind sensor, will address ---further science goals of the mission. If Ariane 6-2 and higher lift performance are available for launch (the baseline mission assumes a launch on a Soyuz Fregat), we expect to have greater spacecraft mobility and possibly added payloads.

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“…Basilevsky et al 2014). The tidally locked rotation may induce heterogeneous evolution of the surface layer between leading and trailing hemispheres due to the different flux and approaching velocities of impactors (Christou 2014). The molecular flux from the Martian atmosphere may affect space weathering of the moons' surface along with the influx of solar wind and meteoroids (e.g., Stofer 1971; Poppe and Curry 2014).…”

Section: Mission Requirementsmentioning

confidence: 99%

Martian Moons Exploration MMX: Sample Return Mission to Phobos Elucidating Formation Processes of Habitable Planets

Kuramoto

Kawakatsu²,

Fujimoto³

et al. 2021

Preprint

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Martian moons exploration, MMX, is the new sample return mission planned by the Japan Aerospace Exploration Agency (JAXA) targeting the two Martian moons with a scheduled launch in 2024 and a return to the Earth in 2029. The major scientific objectives of this mission are to determine the origin of Phobos and Deimos, to elucidate the early Solar System evolution in terms of volatile delivery across the snow line to the terrestrial planets having habitable surface environments, and to explore the evolutionary processes of both moons and Mars surface environment. To achieve these objectives, during a stay in circum-Martian space over about 3 years MMX will collect samples from Phobos along with close-up observations of this inner moon and carry out multiple flybys of Deimos to make comparative observations of this outer moon. Simultaneously, successive observations of the Martian atmosphere will also be made by utilizing the advantage of quasi-equatorial spacecraft orbits along the moons’ orbits.

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The meteoroid environment and impacts on Phobos

Cited by 10 publications

References 35 publications

Meteorites from Phobos and Deimos at Earth?

Meteorites from Phobos and Deimos at Earth?

DePhine – The Deimos and Phobos Interior Explorer

Martian Moons Exploration MMX: Sample Return Mission to Phobos Elucidating Formation Processes of Habitable Planets

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