Can Planets Survive Stellar Evolution?

By Eva Villaver, M. Livio. 2007

160 citations recorded by the source corpus.

We study the survival of gas planets around stars with masses in the range 1-5 M☉, as these stars evolve off the main sequence. We show that planets with masses smaller than one Jupiter mass do not survive the planetary nebula phase if located initially at orbital distances smaller than 3-5 AU. Planets more massive than two Jupiter masses around low-mass (1 M☉ on the main sequence) stars survive the planetary nebula stage down to orbital distances of ~3 AU. As the star evolves through the planetary nebula phase, an evaporation outflow will be established at the planet's surface. Evaporating planets may be detected using spectroscopic observations. Planets around white dwarfs with masses MWD ≳ 0.7 M☉ are generally expected to be found at orbital radii r ≳ 15 AU. If gas planets are found at smaller orbital radii around massive white dwarfs, they had to form as the result of the merger of two white dwarfs.

Subfields: Astronomy and Astrophysics, Instrumentation, Statistical and Nonlinear Physics

View Paper: https://www.semanticscholar.org/paper/ab8da46a88cd6fe0d60290e8ba1f3919eed9f623

How researchers see this paper

The researchers whose trusted networks rank it highest, strongest advocate first. Every researcher gets a different order.

In Astronomy and Astrophysics

1. J. Farihi
2. A. Mustill
3. Amy Bonsor
4. B. Gänsicke
5. D. Veras
6. D. Koester
7. M. C. Wyatt
8. L. Kaltenegger

In Instrumentation

1. A. Mustill
2. J. Farihi
3. Amy Bonsor
4. M. C. Wyatt
5. L. Kaltenegger
6. B. Gänsicke
7. D. Koester
8. Eva Villaver

In Statistical and Nonlinear Physics

1. A. Mustill
2. Amy Bonsor
3. M. C. Wyatt
4. L. Kaltenegger
5. B. Gänsicke
6. Eva Villaver
7. D. Veras
8. M. Livio

Citations in the corpus

• FORETELLINGS OF RAGNARÖK: WORLD-ENGULFING ASYMPTOTIC GIANTS AND THE INHERITANCE OF WHITE DWARFS (2012, background): “Villaver & Livio (2007) estimated the radii of the innermost surviving planets by assuming that they would come from planets whose initial radius was at the maximum stellar radius.”
• 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).”
• How to Characterize Habitable Worlds and Signs of Life (2017, background): “…that corresponds to the HZ, which is based on stellar irradiance and the host star’s SED, moves outward with increasing stellar luminosity during a star’s evolution (see, e.g., Villaver & Livio 2007, Danchi & Lopez 2013, Rushby et al. 2013, Luger & Barnes 2015, Ramirez & Kaltenegger 2014, 2016).”
• THE ORBITAL EVOLUTION OF GAS GIANT PLANETS AROUND GIANT STARS (2009, background): “The temperature at the planet’s surface has been taken to be the maximum between the radiative equilibrium temperature of the planet (see, e.g., Equation (5) in L81 Villaver & Livio 2007) and the temperature of the shocked gas Tsh = (3mH/16kb)v2 (estimated from the Rankine–Hugoniot conditions for an”
• Distant future of the Sun and Earth revisited (2008, background): “A more general discussion of planetary survival during post-main-sequence evolution has been given by Villaver & Livio (2007), who suggest that an initial distance of at least 3au is needed for the survival of a terrestrial-size planet when one also takes into account the possible evaporation of…”
• Dynamical effects of stellar mass-loss on a Kuiper-like belt (2011, background): “Many closein planets will be swallowed by the expanding stellar envelope whilst the star is on the giant branch (e.g. Villaver & Livio 2007).”
• 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, background): “Villaver & Livio (2007, 2009) and Villaver (2011) treat this effect in detail with additional physics such as frictional drag, planet accretion, planet evaporation and Downloaded from https://academic.oup.com/mnras/article-abstract/431/2/1686/1463884 by guest on 30 July 2018 spin.”
• 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).”