THE HD 192263 SYSTEM: PLANETARY ORBITAL PERIOD AND STELLAR VARIABILITY DISENTANGLED

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

DOI:https://doi.org/10.1088/0004-637X/754/1/37· OSTI ID:22039306

Dragomir, Diana; Matthews, Jaymie M ^[1]; Kane, Stephen R; Ciardi, David R; Von Braun, Kaspar ^[2]; Henry, Gregory W ^[3]; Fischer, Debra A ^[4]; Howard, Andrew W ^[5]; Jensen, Eric L. N. ^[6]; Laughlin, Gregory ^[7]; Mahadevan, Suvrath; Pilyavsky, Genady; Wang, Sharon X

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1. Department of Physics and Astronomy, University of British Columbia, Vancouver, BC, V6T1Z1 (Canada)
2. NASA Exoplanet Science Institute, Caltech, MS 100-22, 770 South Wilson Avenue, Pasadena, CA 91125 (United States)
3. Center of Excellence in Information Systems, Tennessee State University, 3500 John A. Merritt Blvd., Box 9501, Nashville, TN 37209 (United States)
4. Department of Astronomy, Yale University, New Haven, CT 06511 (United States)
5. Department of Astronomy, University of California, Berkeley, CA 94720 (United States)
6. Department of Physics and Astronomy, Swarthmore College, Swarthmore, PA 19081 (United States)
7. UCO/Lick Observatory, University of California, Santa Cruz, CA 95064 (United States)

As part of the Transit Ephemeris Refinement and Monitoring Survey, we present new radial velocities and photometry of the HD 192263 system. Our analysis of the already available Keck-HIRES and CORALIE radial velocity measurements together with the five new Keck measurements we report in this paper results in improved orbital parameters for the system. We derive constraints on the size and phase location of the transit window for HD 192263b, a Jupiter-mass planet with a period of 24.3587 {+-} 0.0022 days. We use 10 years of Automated Photoelectric Telescope photometry to analyze the stellar variability and search for planetary transits. We find continuing evidence of spot activity with periods near 23.4 days. The shape of the corresponding photometric variations changes over time, giving rise to not one but several Fourier peaks near this value. However, none of these frequencies coincides with the planet's orbital period and thus we find no evidence of star-planet interactions in the system. We attribute the {approx}23 day variability to stellar rotation. There are also indications of spot variations on longer (8 years) timescales. Finally, we use the photometric data to exclude transits for a planet with the predicted radius of 1.09 R{sub J} , and as small as 0.79 R{sub J} .

• OSTI ID: 22039306
• 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
ASTRONOMY
ASTROPHYSICS
MASS
MONITORING
PHOTOMETRY
PLANETS
RADIAL VELOCITY
ROTATION
SHAPE
STARS
STARSPOTS
TELESCOPES
VARIATIONS