Planet-Star Interactions with Precise Transit Timing. II. The Radial-Velocity Tides and a Tighter Constraint on the Orbital Decay Rate in the WASP-18 System

• Autorzy: Maciejewski G. , Knutson H. A. , Howard A. W. , Isaacson H. , Fernández-Lajús E. , Di Sisto R. P. , Migaszewski C.

Identyfikatory

DOI

10.32023/0001-5237/70.1.1

• Języki publikacji: EN

Abstrakty

EN

From its discovery, the WASP-18 system with its massive transiting planet on a tight orbit was identified as a unique laboratory for studies on tidal planet-star interactions. In an analysis of Doppler data, which include five new measurements obtained with the HIRES/Keck-I instrument between 2012 and 2018, we show that the radial velocity signal of the photosphere following the planetary tidal potential can be distilled for the host star. Its amplitude is in agreement with both theoretical predictions of the equilibrium tide approximation and an ellipsoidal modulation observed in an orbital phase curve. Assuming a circular orbit, we refine system parameters using photometric time series from TESS. With a new ground-based photometric observation, we extend the span of transit timing observations to 28 yr in order to probe the rate of the orbital period shortening. Since we found no departure from a constant-period model, we conclude that the modified tidal quality parameter of the host star must be greater than 3.9×106 with 95% confidence. This result is in line with conclusions drawn from studies of the population of hot Jupiters, predicting that the efficiency of tidal dissipation is 1 or 2 orders of magnitude weaker. As the WASP-18 system is one of the prime candidates for detection of orbital decay, further timing observations are expected to push the boundaries of our knowledge on stellar interiors.

Słowa kluczowe

EN

planet-star interactions; stars: individual: WASP-18; planets: individual: WASP-18 b; satellites: individual: WASP-18 b

• Wydawca: Copernicus Foundation for Polish Astronomy
• Czasopismo: Acta Astronomica
• Rocznik: 2020
• Tom: Vol. 70, No. 1
• Strony: 1--18
• Opis fizyczny: Bibliogr. 48 poz., tab., wykr.

Twórcy

autor

Maciejewski G.

• Institute of Astronomy, Faculty of Physics, Astronomy and Informatics, Nicolaus Copernicus University, Grudziądzka 5, 87-100 Toruń, Poland

autor

Knutson H. A.

• Division of Geological and Planetary Sciences, California Institute of Technology, 1200 E. California Blvd., Pasadena, CA 91125, USA

autor

Howard A. W.

• Institute for Astronomy, University of Hawaii, Honolulu, HI 96822, USA

autor

Isaacson H.

• Department of Astronomy, University of California Berkeley, Berkeley CA 94720, USA

autor

Fernández-Lajús E.

• Facultad de Ciencias Astronómicas y Geofísicas, Universidad Nacional de La Plata, 1900 La Plata, Buenos Aires, Argentina
• Instituto de Astrofísica de La Plata (CCT La Plata C CONICET/UNLP), Paseo del Bosque s/n, La Plata, BA, B1900FWA, Argentina

autor

Di Sisto R. P.

• Facultad de Ciencias Astronómicas y Geofísicas, Universidad Nacional de La Plata, 1900 La Plata, Buenos Aires, Argentina
• Instituto de Astrofísica de La Plata (CCT La Plata C CONICET/UNLP), Paseo del Bosque s/n, La Plata, BA, B1900FWA, Argentina

autor

Migaszewski C.

• Institute of Astronomy, Faculty of Physics, Astronomy and Informatics, Nicolaus Copernicus University, Grudziądzka 5, 87-100 Toruń, Poland

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