The effect of evaporation on the evolution of close-in giant planets

By Isabelle Baraffe, F. Selsis, G. Chabrier, Travis S. Barman, F. Allard, Peter Hauschildt, H. Lammer. 2004

191 citations recorded by the source corpus.

We include the effect of evaporation in our evolutionary calculations of close-in giant planets, based on a recent model for thermal evaporation taking into account the XUV flux of the parent star (Lammer et al. 2003). Our analysis leads to the existence of a critical mass for a given orbital distance mcrit(a) below which the evaporation timescale becomes shorter than the thermal timescale of the planet. For planets with initial masses below mcrit, evaporation leads to a rapid expansion of the outer layers and of the total planetary radius, speeding up the evaporation process. Consequently, the planet does not survive as long as estimated by a simple application of mass loss rates without following consistently its evolution. We find out that the transit planet HD 209458b might be in such a dramatic phase, although with an extremely small probability. As a consequence, we predict that, after a certain time, only planets above a value mcrit(a) should be present at an orbital distance a of a star. For planets with initial masses above mcrit, evaporation does not affect the evolution of the radius with time.

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

View Paper: https://www.semanticscholar.org/paper/853d2c416c676510c0f47dee78bfb5bf0b2053b8

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In Astronomy and Astrophysics

1. Jon Fortney
2. J. Owen
3. D. Charbonneau
4. N. Madhusudhan
5. C. Mordasini
6. Sara Seager
7. J. Winn
8. J. Southworth

In Instrumentation

1. Jon Fortney
2. J. Owen
3. D. Charbonneau
4. J. Southworth
5. J. Winn
6. Sara Seager
7. J. Johnson
8. N. Madhusudhan

In Statistical and Nonlinear Physics

1. J. Owen
2. Jon Fortney
3. Sara Seager
4. C. Mordasini
5. Yanqin Wu
6. Sheng Jin
7. Leslie A. Rogers
8. D. Charbonneau

Citations in the corpus

• THE IMPRINT OF EXOPLANET FORMATION HISTORY ON OBSERVABLE PRESENT-DAY SPECTRA OF HOT JUPITERS (2016, background): “Despite the rather low mass loss at 0.04 AU, the “wet Saturn” is actually quite close to the threshold where catastrophic runaway evaporation occurs (Baraffe et al. 2004; Kurokawa & Kaltenegger 2013; Jin et al. 2014): if this planet is evolved at 0.03 AU instead of 0.04 AU for otherwise nominal…”
• The minimum-mass extrasolar nebula: in situ formation of close-in super-Earths (2012, background): “…total planet mass, while equation (31) predicts that XUV radiation could have eroded away ∆Menvelope > 0.1M⊕ or >2% of the planet mass — this is a lower limit because Kepler-11b could have undergone “runaway” mass loss during which the planet stayed inflated for long duration (Baraffe et al. 2004).”
• A diagram to determine the evaporation status of extrasolar planets (2006, background): “Models of the time variation of this escape rate lead to slightly larger values for the total fraction of mass lost over the whole stellar life (see e.g., Lecavelier des Etangs et al. 2004; Baraffe et al. 2004).”
• The Interior Structure, Composition, and Evolution of Giant Planets (2009, background): “– Baraffe et al. (2004) found that HD 209458b could be in the midst of extreme envelope evaporation, leading to a large radius, and we are catching the planet at a special time in its evolution.”
• Compositional Imprints in Density–Distance–Time: A Rocky Composition for Close-in Low-mass Exoplanets from the Location of the Valley of Evaporation (2017, background): “…in the evolution model is the atmospheric escape due to the heating from stellar X-ray and extreme-ultraviolet (XUV) irradiation (e.g., Watson et al. 1981; Lammer et al. 2003; Baraffe et al. 2004; Yelle 2004; Tian et al. 2005; Murray-Clay et al. 2009; Owen & Jackson 2012; Owen & Alvarez 2016).”
• SUPER-EARTH ATMOSPHERES: SELF-CONSISTENT GAS ACCRETION AND RETENTION (2015, background): “We estimate the equilibrium temperature by T/T⊕ = (F/F⊕) 1/4, with the flux (relative to Earth’s) F/F⊕ estimated by Weiss & Marcy (2014), and with the Earth’s equilibrium temperature T⊕ ≈ 260 K.”
• Evaporation of the planet HD 189733b observed in H I Lyman-α (2010, background): “…theoretical models to explain and characterize the evaporation processes (Lammer et al. 2003; Lecavelier des Etangs et al. 2004, 2007, 2008a; Baraffe et al. 2004, 2005, 2006; Yelle 2004, 2006; Jaritz et al. 2005; Tian et al. 2005; Garćıa-Muñoz 2007; Holmström et al. 2008; Stone & Proga…”
• ATMOSPHERIC ESCAPE FROM HOT JUPITERS (2008, background): “What explains the factor of 100 discrepancy between our maximum mass loss rates and the mass loss rates given by Lammer et al. (2003) and Baraffe et al. (2004)?”
• Can Planets Survive Stellar Evolution? (2007, background): “[5]) and higher than the gas photoionization temperature (10,000 K), and is the characteristic planetary temperature for thermal escape (Moutou et al. 2001; Lammer et al. 2003; Baraffe et al. 2004; Lecavelier des Etangs et al. 2004).”
• A STUDY OF THE SHORTEST-PERIOD PLANETS FOUND WITH KEPLER (2014, background): “This absence of subNeptunes had been predicted by different simulations of mass loss of close-in planets (Baraffe et al. 2004; Valencia et al. 2009; Lopez & Fortney 2013a; Owen & Wu 2013).”
• Estimation of the XUV radiation onto close planets and their evaporation (2011, background): “Baraffe et al. (2004) consider that evaporation actually takes place at a point somewhere above the planet radiusRp, at the “expansion radius”R1.”
• Transonic Hydrodynamic Escape of Hydrogen from Extrasolar Planetary Atmospheres (2005, background): “On the basis of the Watson approach, recently Baraffe et al. (2004) defined a ‘‘critical mass’’ as the mass below which the mass-loss timescale through atmospheric escape becomes 1/10 of the Kelvin-Helmholtz timescale (tK-H ¼ 2Gm2=RL) after 5 billion yr of evolution.”
• TESTING IN SITU ASSEMBLY WITH THE KEPLER PLANET CANDIDATE SAMPLE (2013, background): “Alternatively, it has been proposed that intense stellar irradiation can evaporate the envelopes of hot Jupiter planets, leaving behind only the Neptune-mass stellar core (Baraffe et al. 2004).”
• HOW THERMAL EVOLUTION AND MASS-LOSS SCULPT POPULATIONS OF SUPER-EARTHS AND SUB-NEPTUNES: APPLICATION TO THE KEPLER-11 SYSTEM AND BEYOND (2012, methodology): “Similar approaches have also been used to study the coupled evolution of hot Jupiters (e.g., Baraffe et al. 2004, 2005; Hubbard et al. 2007a, 2007b) and hot Neptunes (Baraffe et al. 2006).”
• OBSERVATIONS OF MASS LOSS FROM THE TRANSITING EXOPLANET HD 209458b (2010, background): “…papers concerning the mechanisms for mass loss and lifetime of a Jupiter-like planet close to its host star [e.g., Vidal-Madjar et al. (2003); Baraffe et al. (2004); Koskinen et al. (2007); Holmström et al. (2008); Koskinen et al. (2010)] and hydrodynamic models [e.g., Lammer et al.…”
• Planetary evaporation by UV and X‐ray radiation: basic hydrodynamics (2012, methodology): “In addition, Baraffe et al. (2004) point out that a critical point may occur when a planet’s evaporation timescale becomes shorter than the thermal timescale.”
• Atmospheric Escape and the Evolution of Close-In Exoplanets (2018, background): “Baraffe et al. (2004, 2005) coupled Lammer et al. (2003)’s reformulation of the Watson et al. (1981) energylimited model to an evolutionary calculation.”
• Detection of a Neptune-Mass Planet in the ρ1 Cancri System Using the Hobby-Eberly Telescope (2004, background): “This tidal heating could have caused the radius of the planet to inflate, possibly overflowing the Roche radius of the star and resulting in significant planetary mass loss (4; Baraffe et al. 2004).”