A SECOND GIANT PLANET IN 3:2 MEAN-MOTION RESONANCE IN THE HD 204313 SYSTEM

Journal Article · Fri Jul 20 00:00:00 EDT 2012 · Astrophysical Journal

DOI:https://doi.org/10.1088/0004-637X/754/1/50· OSTI ID:22039295

Robertson, Paul; Endl, Michael; Cochran, William D; MacQueen, Phillip J; Brugamyer, Erik J; Barnes, Stuart I; Caldwell, Caroline ^[1]; Horner, J; Wittenmyer, Robert A ^[2]

---

1. Department of Astronomy and McDonald Observatory, University of Texas at Austin, Austin, TX 78712 (United States)
2. Department of Astrophysics and Optics, School of Physics, University of New South Wales, Sydney, NSW 2052 (Australia)

We present eight years of high-precision radial velocity (RV) data for HD 204313 from the 2.7 m Harlan J. Smith Telescope at McDonald Observatory. The star is known to have a giant planet (Msin i = 3.5 M{sub J} ) on a {approx}1900 day orbit, and a Neptune-mass planet at 0.2 AU. Using our own data in combination with the published CORALIE RVs of Segransan et al., we discover an outer Jovian (Msin i = 1.6 M{sub J} ) planet with P {approx} 2800 days. Our orbital fit suggests that the planets are in a 3:2 mean motion resonance, which would potentially affect their stability. We perform a detailed stability analysis and verify that the planets must be in resonance.

• OSTI ID: 22039295
• Journal Information: Astrophysical Journal, Vol. 754, Issue 1; Other Information: Country of input: International Atomic Energy Agency (IAEA); ISSN 0004-637X
• Country of Publication: United States
• Language: English

Related Subjects

79 ASTROPHYSICS
COSMOLOGY AND ASTRONOMY
ACCURACY
ASTRONOMY
ASTROPHYSICS
MASS
ORBITS
PLANETS
RADIAL VELOCITY
RESONANCE
SATELLITES
STABILITY
STARS
TELESCOPES