Tidal Dissipation in Rotating Solar-Type Stars

By Gordon I. Ogilvie, D. Lin. 2007

267 citations recorded by the source corpus.

We calculate the excitation and dissipation of low-frequency tidal oscillations in uniformly rotating solar-type stars. For tidal frequencies smaller than twice the spin frequency, inertial waves are excited in the convective envelope and are dissipated by turbulent viscosity. Enhanced dissipation occurs over the entire frequency range rather than in a series of very narrow resonant peaks and is relatively insensitive to the effective viscosity. Hough waves are excited at the base of the convective zone and propagate into the radiative interior. We calculate the associated dissipation rate under the assumption that they do not reflect coherently from the center of the star. Tidal dissipation in a model based on the present Sun is significantly enhanced through the inclusion of the Coriolis force but may still fall short of that required to explain the circularization of close binary stars. However, the dependence of the results on the spin frequency, tidal frequency, and stellar model indicate that a more detailed evolutionary study including inertial and Hough waves is required. We also discuss the case of higher tidal frequencies appropriate to stars with very close planetary companions. The survival of even the closest hot Jupiters can be plausibly explained provided that the Hough waves they generate are not damped at the center of the star. We argue that this is the case because the tide excited by a hot Jupiter in the present Sun would marginally fail to achieve nonlinearity. As conditions at the center of the star evolve, nonlinearity may set in at a critical age, resulting in a relatively rapid inspiral of the hot Jupiter.

Subfields: Astronomy and Astrophysics

View Paper: https://www.semanticscholar.org/paper/1b64cac72ed654e94a2dcdfee0729ec81f3cd25e

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Citations in the corpus

WASP-19b: THE SHORTEST PERIOD TRANSITING EXOPLANET YET DISCOVERED (2010, background): “…modulating tidal dissipation in stars, since currently, there is no comprehensive theory that is able to explain observations of both main-sequence binary stars and close-in extrasolar planets with regard to their tidal evolution (Rasio et al. 1996; Sasselov 2003; Terquem 1998; Ogilvie & Lin 2007).”
INTERNAL GRAVITY WAVES IN MASSIVE STARS: ANGULAR MOMENTUM TRANSPORT (2013, methodology): “The above interpretation is based on the application of a model of the stellar tide by Zahn (1977), the quantitative details of which remain uncertain (Ogilvie & Lin 2007; Goodman & Lackner 2009; Barker & Ogilvie 2010).”
Is tidal heating sufficient to explain bloated exoplanets? Consistent calculations accounting for finite initial eccentricity (2010, background): “For example, Q′? values inferred from the circularization of close FGK binary stars (Meibom & Mathieu 2005), may be lower than the actual Q′? encountered in star-planet systems (Ogilvie & Lin 2007).”
The GAPS Programme with HARPS-N at TNG - XIV. Investigating giant planet migration history via improved eccentricity and mass determination for 231 transiting planets (2017, unknown): “…our values are also in general agreement with those theoretically expected in the case of stars hosting hot Jupiters according to the dynamic tide theory in Ogilvie & Lin (2007) that may account for the di ﬀ erences in the estimated Q s between close stellar binary systems and star-planet systems.”
Tidal Dissipation in Stars and Giant Planets (2014, background): “Studies of the dynamical tide in a solar model can then explain Q′ ≈ 107–108 (Ogilvie & Lin 2007), but this is still too inefficient to explain the observations.”
Tidal dissipation in planet-hosting stars: damping of spin-orbit misalignment and survival of hot Jupiters (2011, methodology): “Barker & Ogilvie (2009) reported the result of a calculation of the l = 2, m = 1 tidal dissipation for a specific F-type stellar model (appropriate for the hot Jupiter system XO-3) using the numerical method of Ogilvie & Lin (2007).”
Resonance locking as the source of rapid tidal migration in the Jupiter and Saturn moon systems (2016, background): “…inertial waves are focused onto attractors to create enhanced tidal dissipation (Rieutord et al. 2001; Ogilvie & Lin 2004; Papaloizou & Ivanov 2005; Ogilvie & Lin 2007; Ivanov & Papaloizou 2007; Goodman & Lackner 2009; Rieutord & Valdettaro 2010; Papaloizou & Ivanov 2010; Ivanov & Papaloizou 2010;…”
The Apparently Decaying Orbit of WASP-12b (2017, background): “It is also possible that orbital decay occurs in fits and starts, because of strong and erratic variations in the dissipation rate with the forcing period (see, e.g., Ogilvie & Lin 2007; Barker & Ogilvie 2010).”
OBSERVATIONAL EVIDENCE FOR TIDAL DESTRUCTION OF EXOPLANETS (2009, background): “Alternative assumptions are possible (Zahn 1977; Hut 1981; Ogilvie & Lin 2007; Penev et al. 2007), and may be important for the cases we consider here, where orbital and rotational frequencies may change rapidly.”
On internal wave breaking and tidal dissipation near the centre of a solar-type star (2010, background): “…by low-frequency tidal forcing and has received much recent interest with regard to its possible contribution to Q′ (Witte & Savonije 2002; Ogilvie & Lin 2004, hereafter OL04; Papaloizou & Ivanov 2005; Wu 2005; Ivanov & Papaloizou 2007; Ogilvie & Lin 2007, hereafter OL07; Goodman & Lackner 2009).”
On the tidal evolution of Hot Jupiters on inclined orbits (2009, background): “…calculations of the excitation and dissipation of internal waves have indicated that Q′ varies in a complicated way with the tidal frequency (see Savonije et al. 1995; Savonije & Papaloizou 1997; Papaloizou & Savonije 1997; Ogilvie & Lin 2004, hereafter OL04; Ogilvie & Lin 2007, hereafter OL07).”
Tidal Heating of Extrasolar Planets (2008, background): “Considerable progress is being made in this area (Ogilvie & Lin 2004, 2007).”
TIDAL EVOLUTION OF CLOSE-IN PLANETS (2010, background): “This is because tidal quality factors depend sensitively on the detailed interior structure of the body (either star or planet), as well as the tidal forcing frequency and amplitude, and are unlikely to be expressed as a simple constant value (e.g., Ogilvie & Lin 2004, 2007; Wu 2005).”
Observational Evidence for Tidal Interaction in Close Binary Systems (2007, background): “Very recently tidal interaction with inertial waves in convective envelopes of solar-type stars was also considered as a source for orbital evolution (Ogilvie & Lin 2007; see also Ivanov & Papaloizou 2007).”