Abstract
We study the dynamical behavior of small dust particles ejected from martian satellites, taking into account the mass–velocity relation of ejecta estimated from laboratory measurements, and several kinds of perturbation forces on the particles. The combination of dynamical effects caused by Mars's oblateness with those of solar radiation pressure plays an important role in the formation of dust rings around Mars. From numerical simulations and analytical estimates for the orbital evolution of ring particles, we have found that dust rings with asymmetrical structure exist along the satellite's orbit; i.e., Phobos's dust ring has a thin disk-like shape whereas Deimos's is vertically extended. Typical masses of ring particles and their number density, respectively, are about 10−7g and 10−9m−3for Phobos dust rings and nearly 10−8g and 10−8m−3for Deimos dust rings.
Sign-in/Register to access full text options 
Talk to us
Join us for a 30 min session where you can share your feedback and ask us any queries you have
Schedule a callDisclaimer: All third-party content on this website/platform is and will remain the property of their respective owners and is provided on "as is" basis without any warranties, express or implied. Use of third-party content does not indicate any affiliation, sponsorship with or endorsement by them. Any references to third-party content is to identify the corresponding services and shall be considered fair use under The CopyrightLaw.
