Accretion of Phobos and Deimos in an extended debris disc stirred by transient moons

@article{Rosenblatt2016AccretionOP,
  title={Accretion of Phobos and Deimos in an extended debris disc stirred by transient moons},
  author={Pascal Rosenblatt and S{\'e}bastien Charnoz and Kevin M. Dunseath and Mariko Terao-Dunseath and Antony Trinh and Ryuki Hyodo and Hidenori Genda and St{\'e}ven Toupin},
  journal={Nature Geoscience},
  year={2016},
  volume={9},
  pages={581-583}
}
Mars has two small moons that may have formed in the aftermath of a giant impact. Simulations suggest that Phobos and Deimos accreted from the disperse outer region of the debris disc that was stirred up by short-lived larger moons. 
Rise and fall of the Martian moons
The two small satellites of Mars are thought to have accreted from a debris disk formed in a giant impact. Simulations suggest the moons were shepherded into formation by the dynamical influence of
Equipotential surfaces and geodetic implications on formation of Martian moons
We determine the normal ellipsoids for the Martian moons, Phobos and Deimos, that closely approximate the equipotential surfaces in the respective gravity fields. We compare the normal ellipsoids
An ongoing satellite-ring cycle of Mars and the origins of Phobos and Deimos
The Martian moons Phobos and Deimos may have accreted from a ring of impact debris, but explaining their origin from a single giant impact has proven difficult. One clue may lie in the orbit of
Mass wasting on Phobos triggered by an evolving tidal environment
The Martian moon Phobos is experiencing orbital decay, increasing tidal forces, and possible disruption in the near future. We suggest that this changing dynamic tidal environment has contributed to
Dynamical evidence for Phobos and Deimos as remnants of a disrupted common progenitor
<p>The origin of the Martian moons, Phobos and Deimos, remains elusive. While the morphology and their cratered surfaces suggest an asteroidal origin, capture has been questioned because of potential
Origin of Phobos and Deimos by the impact of a Vesta-to-Ceres sized body with Mars
TLDR
It is found that forming Phobos-Deimos requires an oblique impact by a Vesta-to-Ceres sized object with ~10−3 times Mars’ mass, a much less massive impactor than previously considered.
A dynamical context for the origin of Phobos and Deimos
We show that a model in which Mars grows near Earth and Venus but is then scattered out of the terrestrial region yields a natural pathway to explain the low masses of the Martian moons Phobos &
Equipotential Figure of Phobos Suggests Its Late Accretion Near 3.3 Mars Radii
The ellipsoidal figure of Phobos has been tentatively interpreted as resulting from accretion in a tidal environment close to its parent planet Mars. The issue is compounded by the rapid tidal decay
On the Impact Origin of Phobos and Deimos. I. Thermodynamic and Physical Aspects
Phobos and Deimos are the two small moons of Mars. Recent works have shown that they can accrete within an impact-generated disk. However, the detailed structure and initial thermodynamic properties
Mars in the aftermath of a colossal impact
...
...

References

SHOWING 1-10 OF 34 REFERENCES
The demise of Phobos and development of a Martian ring system
The moon Phobos will eventually either disintegrate to form a ring or crash into Mars. Observational constraints and geotechnical considerations suggest that Phobos will partially break apart into a
Formation of Phobos and Deimos via a giant impact
Tidal rigidity of Phobos
The origin of the Martian moons revisited
The origin of the Martian moons, Phobos and Deimos, is still an open issue: either they are asteroids captured by Mars or they formed in situ from a circum-Mars debris disk. The capture scenario
Evolution of a Circumterrestrial Disk and Formation of a Single Moon
Abstract We investigate the evolution of a circumterrestrial disk of debris generated by a giant impact on Earth and the dynamical characteristics of the moon accreted from the disk by using
The recent formation of Saturn's moonlets from viscous spreading of the main rings
TLDR
A hybrid simulation is reported in which the viscous spreading of Saturn’s rings beyond the Roche limit (the distance beyond which the rings are gravitationally unstable) gives rise to the small moons.
Contradictory clues as to the origin of the Martian moons
The meager available information that is pertinent to the origin and evolution of the Martian satellites is contradictory. The known physical properties of the Martian moons (density, albedo, color
Formation of Multiple-Satellite Systems From Low-Mass Circumplanetary Particle Disks
Circumplanetary particle disks would be created in the late stage of planetary formation either by impacts of planetary bodies or disruption of satellites or passing bodies, and satellites can be
...
...