Radiation Pressure Effects On The R1 And R2 Rings Of Uranus

Details Radiation Pressure Effects On The R1 And R2 Rings Of Uranus Radiation Pressure Effects On The R1 And R2 Rings Of Uranus

Sep 2008

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2008dps....40.3005s&link_type=abstract

American Astronomical Society, DPS meeting #40, #30.05; Bulletin of the American Astronomical Society, Vol. 40, p.446

Astronomy and Astrophysics

Astronomy

Scientific paper

Showalter & Lissauer (2006), through a careful analysis of several Hubble Space Telescope images, discovered two small satellites of Uranus, Mab and Cupid. These images also reveled the existence of two faint rings, R/2003 U1 (R1) and R/2003 U2 (R2). In this work we study the effects of the solar radiation pressure on small particles located in these two rings using numerical simulations, where each ring is represented by an ensemble of particles of several sizes, from 0.5 to 10 microns, under the influence of radiation pressure, Poynting-Robertson drag, planetary oblateness and the perturbation of the closest satellites (Puck and Mab for R1 and Portia and Rosalind for R2). Our results show that Poynting-Roberson drag causes the orbit collapse in a time scale of 105 to 106 years, while planetary oblateness prevent the eccentricity increases due to radiation pressure. A combination of all perturbations shows that, although Mab's size, the satellite is hit by some particles with impact velocity several times larger than the scape velocity what can result in ejection of material. The inner ring R2 does not have any evident material source and particles initially in the ring region oscillates before colliding with one of surrounding moon. Particles can remain within the region for more than 105 orbital periods, what allows collision with macroscopic bodies that may inhabit the region, leading to the production of new ring material for R2. Acknowledgment: RS and SMGW thanks FAPESP for the financial support.

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