On the Impact Origin of Phobos and Deimos. IV. Volatile Depletion

Ryuki Hyodo (1) , Hidenori Genda (2) , Sébastien Charnoz (3, 4) , Francesco C Pignatale (3, 4) , Pascal Rosenblatt (5)

1 TITECH - Tokyo Institute of Technology [Tokyo]
2 ELSI - Earth-Life Science Institute [Tokyo]
3 IPGP - Institut de Physique du Globe de Paris
4 IPGP (UMR_7154) - Institut de Physique du Globe de Paris
5 ACRI-ST - Analytic and Computational Research, Inc. - Earth Sciences

Recent works have shown that the Martian moons Phobos and Deimos may have accreted within a giant impact-generated disk whose composition is about an equal mixture of Martian material and impactor material. Just after the giant impact, the Martian surface heated up to ∼3000-6000 K and the building blocks of moons, including volatile-rich vapor, were heated up to ∼2000 K. In this paper, we investigate the volatile loss from the building blocks of Phobos and Deimos by hydrodynamic escape of vapor and radiation pressure on condensed particles. We show that a non-negligible amount of volatiles (>10% of the vapor with temperature >1000 K via hydrodynamic escape, and moderately volatile dusts that condense at ∼700-2000 K via radiation pressure) could be removed just after the impact during their first single orbit from their pericenters to apocenters. Our results indicate that bulk Phobos and Deimos are depleted in volatile elements. Together with future explorations such as the Japan Aerospace eXploration Agency's Martian Moons eXploration mission, our results could be used to constrain the origin of Phobos and Deimos.

Keywords: planets and satellites: composition; planets and satellites: formation; planets and satellites: individual (Phobos Deimos)

Domains: Earth and Planetary Astrophysics [astro-ph.EP]

Ryuki Hyodo, Hidenori Genda, Sébastien Charnoz, Francesco C Pignatale, Pascal Rosenblatt. On the Impact Origin of Phobos and Deimos. IV. Volatile Depletion. The Astrophysical Journal, 2018, 860 (2), pp.150. ⟨10.3847/1538-4357/aac024⟩. ⟨insu-02559771⟩