THE ORBITAL EVOLUTION OF GAS GIANT PLANETS AROUND GIANT STARS

By Eva Villaver, M. Livio. 2009

193 citations recorded by the source corpus.

Recent surveys have revealed a lack of close-in planets around evolved stars more massive than 1.2 M☉. Such planets are common around solar-mass stars. We have calculated the orbital evolution of planets around stars with a range of initial masses, and have shown how planetary orbits are affected by the evolution of the stars all the way to the tip of the red giant branch. We find that tidal interaction can lead to the engulfment of close-in planets by evolved stars. The engulfment is more efficient for more-massive planets and less-massive stars. These results may explain the observed semimajor axis distribution of planets around evolved stars with masses larger than 1.5 M☉. Our results also suggest that massive planets may form more efficiently around intermediate-mass stars.

View Paper: https://www.semanticscholar.org/paper/4023e17efdd0a3acf9575e6271eae4017b277a7e

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1. J. Farihi
2. A. Mustill
3. J. Winn
4. D. Veras
5. D. Koester
6. O. De Marco
7. B. Gänsicke
8. Amy Bonsor

Citations in the corpus

• The Apparently Decaying Orbit of WASP-12b (2017, background): “The absence of hot Jupiters around subgiant stars may be caused by an acceleration of orbital decay when a star leaves the main sequence (Villaver & Livio 2009; Hansen 2010; Schlaufman & Winn 2013).”
• The great escape: how exoplanets and smaller bodies desert dying stars (2011, background): “Villaver & Livio (2007, 2009), Massarotti (2008) and Nordhaus et al. (2010) use particular stellar evolutionary tracks to determine ranges of semimajor axes at which planets are likely to be engulfed.”
• Simulations of two-planet systems through all phases of stellar evolution: implications for the instability boundary and white dwarf pollution (2013, methodology): “Furthermore, the maximum radius at each phase might differ depending on the model used; see, for example, Villaver & Livio (2009).”
• Precise Radial Velocities of Giant Stars VII. Occurrence Rate of Giant Extrasolar Planets as a Function of Mass and Metallicity (2014, background): “The detailed predictions for the critical semi-major axis for survival are quite different between the models from Villaver & Livio (2009) and Kunitomo et al. (2011), presumably due to differences in their assumptions about stellar evolution.”
• FORETELLINGS OF RAGNARÖK: WORLD-ENGULFING ASYMPTOTIC GIANTS AND THE INHERITANCE OF WHITE DWARFS (2012, methodology): “This effect is larger the smaller th mass of the star, as seen also in Villaver & Livio (2009) for the RGB.”
• The frequency of planetary debris around young white dwarfs (2014, background): “…focusing on the future of the solar system (Sackmann et al. 1993; Duncan & Lissauer 1998), a number of theoretical studies have shown that a fraction of planets can survive the red- giant stage of their host stars (Villaver & Livio 2007, 2009; Nordhaus et al. 2010; Mustill & Villaver 2012).”
• The chemical diversity of exo-terrestrial planetary debris around white dwarfs (2012, background): “Recent years have seen a surge of interest in the evolution of extra-solar planetary systems through the late phases in the lifes of their host stars (e.g. Burleigh et al. 2002; Debes & Sigurdsson 2002; Villaver & Livio 2007, 2009; Nordhaus et al. 2010; Di Stefano et al. 2010).”
• Dawes Review 6: The Impact of Companions on Stellar Evolution (2016, background): “…into the star when the star is extended, the planet needs to be at initial orbital separation between two and four times the radius the star has during its giant phases (depending on the strength of tides; e.g., Villaver & Livio 2009, Mustill & Villaver 2012, Madappatt, De Marco, & Villaver 2016).”
• The Occurrence and Architecture of Exoplanetary Systems (2014, background): “…of close-in planets might be caused by the subgiants’ enhanced rate of tidal dissipation, which makes close-in planets vulnerable to orbit shrinkage and engulfment (Villaver & Livio 2009, Schlaufman & Winn 2013), but this would not explain the over-abundance of giant planets in wider orbits.”