Phobos mass determination from the very close flyby of Mars Express in 2010

• Published in: Icarus (New York, N.Y. 1962) N.Y. 1962), 2014-02, Vol.229, p.92-98
• Main Authors: Pätzold, M., Andert, T.P., Tyler, G.L., Asmar, S.W., Häusler, B., Tellmann, S.
• Format: Article
• Language: English
• Subjects: Asteroids; Asteroids, composition; Bulk density; Disks; Geophysics; Mars Express (ESA); Mars, satellites; Mass distribution; Phobos; Porosity; Satellites, composition; Satellites, dynamics; Satellites, formation
• ISSN: 0019-1035; 1090-2643
• DOI: 10.1016/j.icarus.2013.10.021

•Closest spacecraft flby at the Mars moon Phobos.•Mass, bulk density determined.•Gravity field could not be resolved.•Phobos interior modeled.•Phobos probably not a captured asteroid. The global geophysical parameters GMPh=(0.7072±0.0013)×10-3km3s-2,C20,C22 and the bulk density 〈ρ〉=(1862±30)kg/m3 have been determined from the closest Mars Express flyby at the Mars moon Phobos on 3rd March 2010 at a distance of 77km. The second degree gravity field of Phobos (C20,C22) could not be solved for at sufficient accuracy. The low bulk density suggests a high porosity and an inhomogeneous mass distribution but the large errors of C20 and C22 are still consistent with a homogeneous as well as an inhomogeneous mass distribution. The modeling of the moon’s interior by a randomly selected mass distribution of given porosity and water ice content but constrained by the observed GMPh and 〈ρ〉 let a simulated C20 decrease with increasing porosity and water ice content indicating an increasingly inhomogeneous mass distribution. The high porosity together with an inhomogeneous mass distribution would be evidence that Phobos accreted in orbit about Mars from a debris disk and is not a captured asteroid.