Atmospheric Loss of Exoplanets Resulting from Stellar X-Ray and Extreme-Ultraviolet Heating

By H. Lammer, F. Selsis, I. Ribas, E. Guinan, S. Bauer, W. Weiss. 2003

499 citations recorded by the source corpus.

Subfields: Astronomy and Astrophysics

View Paper: https://www.semanticscholar.org/paper/28aec0ca886bc5443e875218ae43335edcc0c906

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In Astronomy and Astrophysics

1. Jon Fortney
2. J. Owen
3. C. Mordasini
4. N. Madhusudhan
5. Sara Seager
6. Yanqin Wu
7. E. Lopez
8. D. Charbonneau

Citations in the corpus

• JUPITER MODELS WITH IMPROVED AB INITIO HYDROGEN EQUATION OF STATE (H-REOS.2) (2011, background): “Absorbed XUV irradiation can lead to heating of and mass loss from the upper planetary atmosphere (Lammer et al. 2003) but absorption at high altitudes is not suspected to influence the energy balance of the in- terior (Guillot & Showman 2002).”
• Stellar winds on the main-sequence - II. The evolution of rotation and winds (2015, background): “For example, high levels of X-ray and EUV radiation incident on a planetary atmosphere lead to inflation of the atmosphere and in some cases, hydrodynamic escape (Lammer et al. 2003; Tian et al. 2008).”
• The Cosmic Shoreline: The Evidence that Escape Determines which Planets Have Atmospheres, and what this May Mean for Proxima Centauri B (2017, background): “cient: Mars intercepts about 300 grams of solar wind each second, which is comparable to the observed O +escape rate of 160 g s 1 (Brain et al. 2015) and to modeled O escape rates of 300 { 500 g s 1 (Lammer et al. 2003b). Apparently the solar wind impinging on Mars erodes roughly its own mass in mar”
• Evaporation of the planet HD 189733b observed in H I Lyman-α (2010, methodology): “These observational constraints have been used to develop several 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;…”
• 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).”
• BULK COMPOSITION OF GJ 1214b AND OTHER SUB-NEPTUNE EXOPLANETS (2013, background): “In reality the height at which the planet absorbs X-rays and the extreme UV are different and also larger than the planetary radius (Lammer et al. 2003).”
• The Climate of Early Mars (2016, background): “Mars’ reddish, hyperoxidised surface, which is extremely inhospitable to life, is a direct result of the escape of hydrogen to space over geologic time (Lammer et al. 2003).”
• 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 effect of tidal locking on the magnetospheric and atmospheric evolution of ``Hot Jupiters'' (2004, methodology): “It was found that large exospheric temperatures in the order of about 10 000 K for hydrogen dominated atmospheres develop, so that a hydrodynamic treatment must be considered (Watson et al. 1981; Lammer et al. 2003a).”
• LYα TRANSIT SPECTROSCOPY AND THE NEUTRAL HYDROGEN TAIL OF THE HOT NEPTUNE GJ 436b (2014, methodology): “When the thermal energy exceeds the gravitational potential energy (3kT/2 > GMm/r), the heated gas expands (Lammer et al. 2003) and likely escapes from the planet.”
• Hydrodynamic planetary thermosphere model: 1. Response of the Earth's thermosphere to extreme solar EUV conditions and the significance of adiabatic cooling (2008, background): “…planets [e.g., Watson et al., 1981; Kasting and Pollack, 1983; Chassefière, 1996; Tian et al., 2005b], those of close-in extrasolar planets [e.g., Lammer et al., 2003; Yelle, 2004; Tian et al., 2005a; Garcı́a-Muñoz, 2007], and that of Pluto [Krasnopolsky, 1999; Tian and Toon, 2005; Strobel,…”
• THE IMPRINT OF EXOPLANET FORMATION HISTORY ON OBSERVABLE PRESENT-DAY SPECTRA OF HOT JUPITERS (2016, background): “This can drive atmospheric escape (e.g. Lammer et al. 2003; Baraffe et al. 2004; Erkaev et al. 2007; Murray-Clay et al. 2009; Owen & Jackson 2012; Lopez & Fortney 2013).”
• TIDAL EVOLUTION OF CLOSE-IN PLANETS (2010, background): “The orbits of these planets might have been circularized as the planet lost mass (e.g. Lammer et al. 2003; Lecavelier Des Etangs 2007), or the planetary radius expanded due to tidal heating (e.g. Bodenheimer et al. 2001; Gu et al. 2003).”