DETERMINATION OF THE INCLINATION OF THE MULTI-PLANET HOSTING STAR HR 8799 USING ASTEROSEISMOLOGY
- Koninklijke Sterrenwacht van Belgie, Ringlaan 3, B-1180 Brussel (Belgium)
- Canadian Gemini Office, HIA/NRC of Canada, 5071 West Saanich Road, Victoria (BC), V9E 2E7 (Canada)
- National Research Council Canada, Herzberg Institute of Astrophysics, 5071 West Saanich Road, Victoria, BC V9E 2E7 (Canada)
- Laboratoire d'Astrophysique de Toulouse-Tarbes, Universite de Toulouse, CNRS, 57 avenue d'Azereix, F-65000 Tarbes (France)
- Lawrence Livermore National Laboratory, 7000 East Avenue, Livermore, CA 94550 (United States)
- Thueringer Landessternwarte Tautenburg, Sternwarte 5, D-07778 Tautenburg (Germany)
Direct imaging of the HR 8799 system was a major achievement in the study of exoplanets. HR 8799 is a {gamma} Doradus variable and asteroseismology can provide an independent constraint on the inclination. Using 650 high signal-to-noise, high-resolution, full visual wavelength spectroscopic observations obtained over two weeks at Observatoire de Haute Provence with the SOPHIE spectrograph, we find that the main frequency in the radial velocity data is 1.9875 day{sup -1}. This frequency corresponds to the main frequency as found in previous photometric observations. Using the FAMIAS software to identify the pulsation modes, we find that this frequency is a prograde l = 1 sectoral mode and obtain the constraint that inclination i {approx}> 40{sup 0}.
- OSTI ID:
- 21560498
- Journal Information:
- Astrophysical Journal Letters, Vol. 728, Issue 1; Other Information: DOI: 10.1088/2041-8205/728/1/L20; ISSN 2041-8205
- Country of Publication:
- United States
- Language:
- English
Similar Records
HAT-P-68b: A Transiting Hot Jupiter around a K5 Dwarf Star
COULD THE PLANETS AROUND HR 8799 BE BROWN DWARFS?