Orbital Motion Of HR 8799 b, c, d Using Hubble Space Telescope Data From 1998: Constraints On Inclination, Eccentricity And Stability

Details Orbital Motion Of HR 8799 b, c, d Using Hubble Space Telescope Data From 1998: Constraints On Inclination, Eccentricity And Stability Orbital Motion Of HR 8799 b, c, d Using Hubble Space Telescope Data From 1998: Constraints On Inclination, Eccentricity And Stability

Jan 2012

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2012aas...21911007s&link_type=abstract

American Astronomical Society, AAS Meeting #219, #110.07

Astronomy and Astrophysics

Astronomy

Scientific paper

HR 8799 is currently the only multiple-planet system that has been detected with direct imaging, with four giant planets orbiting at large separations from this young late A star. Orbital motion provides insight into the stability, and possible formation mechanisms of this planetary system. Dynamical studies can also provide constraints on the planets’ masses, which help calibrate evolutionary models. Yet, measuring the orbital motion is a very difficult task because the long-period orbits (50-500 yr) require long time baselines and high-precision astrometry. We study the three planets HR 8799b, c and d in the archival data set of HR 8799 obtained with the Hubble Space Telescope (HST) NICMOS coronagraph in 1998. The detection of all three planets is made possible by a careful optimization of the LOCI algorithm, and we used a statistical analysis of a large number of reduced images. This work confirms previous astrometry for planet b, and presents new detections and astrometry for c and d. These HST images provide a ten-year baseline with the discovery images from 2008, and therefore offer a unique opportunity to constrain their orbital motion now. Recent dynamical studies of this system show the existence of a few possible stable solutions involving mean motion resonances, where the interaction between c and d plays a major role. We study the compatibility of a few of these stable scenarios (1d:1c, 1d:2c, or 1d:2c:4d) with the new astrometric data from HST. Our results are consistent with previously published results based on dynamical studies for a three-planet system prior to the discovery of the fourth planet.

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