The Dust Torus around Phobos Orbit

Холшевников, К. В.; Krivov, A. V.; Sokolov, L. L.; Titov, V. B.

doi:10.1006/icar.1993.1132

Cited by 31 publications

(7 citation statements)

References 0 publications

Supporting

Mentioning

Contrasting

Order By: Relevance

“…To estimate the total charge density, the particle density of dust grains of a specified size is required to be known. This knowledge is provided by a few of a number of simulation studies on the dynamics of dust ejecta from Phobos; a problem which attracted a great deal of interest in the past (Kholshevnikov et al, 1993;Ishimoto and Mukai, 1994;Krivov and Hamilton, 1997; a complete list of references can be found in the latest reference). Actually there is no commonly accepted estimate for the dust-induced charge density within the torus.…”

Section: Introductionmentioning

confidence: 99%

“Phobos events”—Signatures of solar wind interaction with a gas torus?

et al. 2014

View full text Add to dashboard Cite

Following recent simulations of the Phobos dust belt formation (Krivov and Hamilton, 1997), the effective dustinduced charge density as estimated is too small to account for the significant solar wind (sw) plasma and magnetic field perturbations observed by the Phobos-2 spacecraft in 1989 near the crossings of the Phobos orbit. In this paper the sw interaction with the Phobos neutral gas torus is re-investigated in a two-ion plasma model in which the newly created ions are treated as unmagnetized, forming a beam (not a ring beam) in the sw frame. A linear instability analysis based on both a cold fluid and a kinetic approach shows that electromagnetic ion beam waves in the whistler range of frequencies, driven most unstable at oblique propagation and appearing as almost purely growing waves in the beam frame, aquire high growth rates and provide a likely mechanism to cause the observed events.

show abstract

Section: Introductionmentioning

confidence: 99%

“Phobos events”—Signatures of solar wind interaction with a gas torus?

et al. 2014

View full text Add to dashboard Cite

show abstract

“…With ejection-larger than escape velocity (about 10 m/s for Phobos and about 6 m/s for Deimos), but smaller than the orbital speed of the moons (V Ph =2.1 km/s for Phobos and V D =1.35 km/s for Deimos), particles should remain trapped in the Martian satellite system. Theoretical models (Banaszkiewicz and Ip, 1991;Ip and Banaszkiewicz, 1990;Ishimoto and Mukai, 1994;Juhász and Horányi, 1995;Kholshevnikov et al, 1993;Krivov and Hamilton, 1997) suggest that these dust grains form rings or tori along the orbits of the satellites.…”

Section: Ejecta Production Re-accumulation and Ring Formationmentioning

confidence: 99%

DePhine – The Deimos and Phobos Interior Explorer

Oberst

Wickhusen

Willner

et al. 2018

Advances in Space Research

View full text Add to dashboard Cite

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.

show abstract

“…For the Deimos ring, interaction between the two asymmetries gives rise to a time-dependent structure that varies with martian season. The smaller particles eventually either impact Mars or are lost from the Mars system (Horanyi et al, 1990(Horanyi et al, , 1991Kholshevnikov et al, 1993;Juhasz and Horanyi, 1995;Sasaki, 1996;Hamilton, 1996;Krivov and Hamilton, 1997;Makuch et al, 2005;Krivov et al, 2006;Zakharov et al, 2014).…”

Section: Surface and Orbital Environmentmentioning

confidence: 99%

Phobos and Deimos

Murchie¹,

Thomas²,

Rivkin³

et al. 2015

Asteroids IV

View full text Add to dashboard Cite

Phobos and Deimos, the satellites of Mars, occupy a unique place in the solar system. They are the only terrestrial planet satellites besides the Moon, yet have traits in common with lowreflectance bodies more typical of the outer solar system. Understanding their composition, origin, and geologic evolution will provide insights into the earliest stages of terrestrial planet formation. Early exploration by the Viking and Mariner 9 missions, decades before the first "proper" asteroid encounters, hinted at several asteroidal properties yet to be discovered: lower than expected densities, abundant regolith even on relatively small bodies, and complicated geology. The first book in this series, Asteroids (1979), had an entire chapter on Phobos and Deimos. We have learned much about these objects in the last 35 years from telescopic and spacecraft observations.

show abstract

The Dust Torus around Phobos Orbit

Cited by 31 publications

References 0 publications

“Phobos events”—Signatures of solar wind interaction with a gas torus?

“Phobos events”—Signatures of solar wind interaction with a gas torus?

DePhine – The Deimos and Phobos Interior Explorer

Phobos and Deimos

Contact Info

Product

Resources

About