Atmospheric escape from hot Jupiters

By A. L. D. Etangs, A. Vidal-Madjar, J. C. McConnell, G. Paris, Cnrs, Paris, France, D. O. Earth, Atmospheric Science, York University and 3 more. 2004

275 citations recorded by the source corpus.

The extra-solar planet HD209458b has been found to have an extended atmosphere of escaping atomic hydrogen (Vidal-Madjar et al. 2003), suggesting that "hot Jupiters" closer to their parent stars could evaporate. Here we estimate the atmospheric escape (so called evaporation rate) from hot Jupiters and their corresponding life time against evaporation. The calculated evaporation rate of HD209458b is in excellent agreement with the H i Lyman-� observations. We find that the tidal forces and high temperatures in the upper atmosphere must be taken into account to obtain reliable estimate of the atmospheric escape. Because of the tidal forces, we show that there is a new escape mechanism at intermediate temperatures at which the exobase reaches the Roche lobe. From an energy balance, we can estimate plausible values for the planetary exospheric temperatures, and thus obtain typical life times of planets as a function of their mass and orbital distance.

Subfields: Astronomy and Astrophysics

View Paper: https://www.semanticscholar.org/paper/f4129dff310ab431f6e9f58fa4eef5ee0b47e5fc

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. Jon Fortney
2. N. Madhusudhan
3. J. Owen
4. D. Charbonneau
5. A. Showman
6. D. Sing
7. Sara Seager
8. C. Mordasini

Citations in the corpus

• Estimation of the XUV radiation onto close planets and their evaporation (2011, background): “An additional source of mass loss takes place through the Roche Lobe for close-in planets (Erkaev et al., 2007) (see also Lecavelier des Etangs et al., 2004; Jaritz et al., 2005,for detailed simulations of the escape through Roche Lobe).”
• MIGRATION THEN ASSEMBLY: FORMATION OF NEPTUNE-MASS PLANETS INSIDE 1 AU (2011, background): “It has been suggested by numerous authors that short-period planets may experience significant atmospheric mass loss driven by irradiation from the central star (e.g., Lammer et al. 2003; Yelle 2004; Lecavelier des Etangs et al. 2004; Tian et al. 2005; Murray-Clay et al. 2009).”
• The HARPS survey for southern extra-solar planets. II. A 14 Earth-masses exoplanet around μ Arae (2004, background): “…is supported by the fact that more massive planets exist orbiting much closer to stars with similar characteristics and by calculations by Baraffe et al. (2004) and Lecavelier des Etangs et al. (2004) which show that only planets significanly less massive than Jupiter would evaporate at 0.09 AU.”
• Temporal variations in the evaporating atmosphere of the exoplanet HD 189733b (2012, background): “…‘evaporation’) arises from the intense stellar X-ray and extreme ultraviolet energy input into the upper atmosphere (Lammeret al. 2003; Lecavelier des Etangs et al. 2004; Yelle 2004), leading to moderate escape rates for massive hot-Jupiters, or to formation of planetary remnants when strong…”
• Evaporation of the planet HD 189733b observed in H I Lyman-α (2010, methodology): “…that, in the case of planets with a mass of only a fraction of the mass of a hot Jupiter and orbiting close to their parent stars, evaporation can lead to significant modification of the nature of the planet, leading to the formation of planetary remnants (Lecavelier des Etangs et al. 2004).”
• ATMOSPHERIC ESCAPE FROM HOT JUPITERS (2008, background): “Jaritz et al. (2005) suggest that for such streamlines, mass loss occurs via “geometrical blow-off” and the Jeans escape criteria of Lecavelier des Etangs et al. (2004) should be applied.”
• Improving Stellar and Planetary Parameters of Transiting Planet Systems: The Case of TrES-2 (2007, background): “…as to compare observations with theoretical evaporation rates of insolated giant planets (Lammer et al. 2003; Baraffe et al. 2004; Lecavelier des Etangs et al. 2004, 2007), are severely affected by large uncertainties in the determination of stellar ages, which can become pathological for field…”
• Can Planets Survive Stellar Evolution? (2007, methodology): “[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).”
• DISEQUILIBRIUM CARBON, OXYGEN, AND NITROGEN CHEMISTRY IN THE ATMOSPHERES OF HD 189733b AND HD 209458b (2011, background): “…model-data comparisons show the atmosphere of HD 209458b to be escaping, with an overall mass loss rate that is low enough that exoplanets like HD 209458b would lose less than ∼1% of their mass over their lifetime (e.g., Lecavelier des Etangs et al. 2004; Tian et al. 2005; Murray-Clay et al. 2009).”
• A diagram to determine the evaporation status of extrasolar planets (2006, methodology): “It has been also suggested that evaporation can lead to significant modification of the planets’ nature in the case of planets with a mass only a fraction of the mass of the observed hot-Jupiter and orbiting close to their parent stars (Lecavelier des Etangs et al. 2004; Baraffe et al. 2005).”
• Temperature–pressure profile of the hot Jupiter HD 189733b from HST sodium observations: detection of upper atmospheric heating (2012, background): “Visible transmission spectroscopy and the sodium D doublet in particular should probe the upper atmosphere, at pres- sures below 150 mbar to as low as 10−9 bar, where we could see very high temperatures (Lecavelier des Etangs et al. 2004; Yelle 2004; Garćıa Muñoz 2007; Moses et al. 2011).”
• OBSERVATIONS OF MASS LOSS FROM THE TRANSITING EXOPLANET HD 209458b (2010, background): “…(2004); Koskinen et al. (2007); Holmström et al. (2008); Koskinen et al. (2010)] and hydrodynamic models [e.g., Lammer et al. (2003); Lecavelier des Etangs et al. (2004); Yelle (2004); Jaritz et al. (2005); Tian et al. (2005); Garcia Muñoz (2007); Schneiter et al. (2007); Murray-Clay et al.…”
• Composition and fate of short-period super-Earths: The case of CoRoT-7b (2009, unknown): “…the heating efficiency defined as the ratio of the net heating rate to the rate of stellar energy absorption, ρ̄p is the mean density of the planet, Ktide is a correction factor to include the Roche-lobe effect (Erkaev et al., 2007; Lecavelier des Etangs et al., 2004), and G is Newton’s constant.”