Imaging a Circumstellar Disk around a Star with a Radial-Velocity Planetary Companion

Details Imaging a Circumstellar Disk around a Star with a Radial-Velocity Planetary Companion Imaging a Circumstellar Disk around a Star with a Radial-Velocity Planetary Companion

Sep 1998

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1998dps....30.2303t&link_type=abstract

American Astronomical Society, DPS meeting #30, #23.03; Bulletin of the American Astronomical Society, Vol. 30, p.1056

Astronomy and Astrophysics

Astronomy

2

Scientific paper

Radial-velocity searches have indirectly detected that a planet with minimum mass 0.84 times that of Jupiter (M_J) orbits the star 55 Cancri, a 3 billion year old G8 star, with a period of 14.65 days and an orbital separation of 0.11 AU (Butler et al. 1997). Furthermore, the detection of excess far infrared emission from 55 Cancri is suggestive of circumstellar dust in that system (Dominik et al. 1998). We have reported results of an infrared coronagraphic search for a mature planetary system around 55 Cancri (Trilling and Brown 1998). We have found a circumstellar disk of material whose inferred mass is approximately 10 times that estimated for our Solar System's Kuiper Belt. The observed disk around 55 Cancri extends to at least 40 AU, consistent with the expected extent of our Solar System's Kuiper Belt (Weissman 1995). Our observations show that 55 Cancri's dust disk is relatively dark at 2.3 microns, consistent with absorption due to methane ice. Assuming that 55 Cancri's disk is coplanar with the radial-velocity planet's orbit, we measure the inclination of the system and find the planet's mass to be {1.9(+1.1}_{-0.4}) M_J. All the available evidence (a definite radial velocity companion; the suggestion of a second radial velocity companion in the system (Butler et al. 1997); the far infrared excess reported by Dominik et al.; and our imaging and characterization of a disk out to at least 40 AU) is suggestive of a mature planetary system around 55 Cancri.

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