Calculating the Tidal, Spin, and Dynamical Evolution of Extrasolar Planetary Systems

By Rosemary A. Mardling, D. Lin. 2002

168 citations recorded by the source corpus.

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In Astronomy and Astrophysics

Citations in the corpus

Long-term tidal evolution of short-period planets with companions (2007, methodology): “Note that this system is stable when the full three-body (non-secular) equations are integrated including post-Newtonian relativistic terms, tidal and spin bulges, as well as tidal damping (Mardling & Lin 2002).”
Tidal obliquity evolution of potentially habitable planets (2011, background): “A comprehensive tidal model would couple the orbital and structural evolution of the bodies since small perturbations inT can result in large variations inQ (Segatz et al. 1988; Mardling & Lin 2002; Efroimsky & Lainey 2007b).”
Tidal Dissipation in Rotating Giant Planets (2003, background): “…orbital evolution of a planetary or a stellar companion of a main-sequence star can be estimated by extrapolation, under the assumption of either a constant lag angle (Goldreich & Soter 1966), a constant lag time (Hut 1981; Eggleton et al. 1998), or an intermediate approach (Mardling & Lin 2002).”
Spin-Orbit Evolution of Short-Period Planets (2004, methodology): “In this paper, we adopt a conventional approach using frequency-independent Q0p; values to analyze the orbital evolution of a star-planet system (Mardling & Lin 2002).”
On the tidal evolution of Hot Jupiters on inclined orbits (2009, methodology): “Here we present the orbit-averaged tidal evolution equations (Eggleton et al. 1998; Eggleton & Kiseleva-Eggleton 2001; Mardling & Lin 2002) used in this work.”
IN SITU FORMATION AND DYNAMICAL EVOLUTION OF HOT JUPITER SYSTEMS (2015, background): “The acceleration arising from the quadrupolar component of the gravitational field of body i experienced by body j takes the form (Mardling and Lin 2002):”
Tidal locking of habitable exoplanets (2017, background): “…rotators around stars of any mass. 3.5 TESS projections The results of the previous section provide a foundation to interpret future discoveries from transit (Berta-Thompson et al. 2015; Gillon et al. 2016), radial velocity (Anglada-Escudé et al. 2016), and astrometric data (Malbet et al. 2016).”
The Effect of Tidal Inflation Instability on the Mass and Dynamical Evolution of Extrasolar Planets with Ultrashort Periods (2003, background): “…star with a mass M∗ and separation r is d2r dt2 = −GMt r3 r + N∑ i=1 fi (1) where Mt = Mp + M∗, and the acceleration fi includes the relativistic potential of the host star, the contribution from other planets, and the tidal and spin distortions of the star and the planet (Mardling & Lin 2002).”
Is tidal heating sufficient to explain bloated exoplanets? Consistent calculations accounting for finite initial eccentricity (2010, methodology): “(19) to rewrite the tidal equation and to keepQ′ constant instead of ∆t as done by, for example, Mardling & Lin (2002), Dobbs-Dixon et al. (2004) and Barker & Ogilvie (2009), one must keep in mind that this procedure is not equivalent either to the constant phase lag (i.e. constant Q) or time lag…”
On the Radii of Extrasolar Giant Planets (2003, background): “Relativistic apse precession, however, detunes the secular exchange and reduces the time-averaged e to 0.03 (see also Mardling & Lin 2002).”
Homogeneous studies of transiting extrasolar planets – IV. Thirty systems with space-based light curves (2011, background): “Coupled with the high eccentricity, this has bearing on its formation and evolution mechanisms (Naefet al. 2001; Mardling & Lin 2002; Matsuo et al. 2007).”
DISSIPATIVE DIVERGENCE OF RESONANT ORBITS (2012, methodology): “…curves stem from the fully analytical framework presented in this section, while the gray curves result from anN -body simulation, where tidal and general relativistic interactions are accounted for directly (Mardling & Lin 2002) and integrated using the BulirschStoer algorithm (Press et al. 1992).”