Transonic Hydrodynamic Escape of Hydrogen from Extrasolar Planetary Atmospheres

By F. Tian, O. B. Toon, A. Pavlov, H. De Sterck. 2005

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In Astronomy and Astrophysics

Citations in the corpus

The escape of heavy atoms from the ionosphere of HD209458b. I. A photochemical–dynamical model of the thermosphere (2012, methodology): “With regard to the127 upper boundary conditions, we demonstrate that for HD209458b the extrap-128 olated ‘outflow’ boundary conditions (e.g., Tian et al., 2005) are consistent129 with recent results from kinetic theory (Volkov et al., 2011a,b) as long as130 the upper boundary is at a sufficiently…”
Temperature–pressure profile of the hot Jupiter HD 189733b from HST sodium observations: detection of upper atmospheric heating (2012, background): “Later models from Tian et al. (2005) and Garćıa Muñoz (2007) showed temperatures of a similar order of magnitude.”
MASS TRANSFER, TRANSITING STREAM, AND MAGNETOPAUSE IN CLOSE-IN EXOPLANETARY SYSTEMS WITH APPLICATIONS TO WASP-12 (2010, background): “…arises entirely from an irradiation-driven wind – such a wind has been studied extensively in the context of hot Jupiter HD 209458b (e.g., Yelle 2004; Tian et al. 2005; Garcia Munoz 2007; Murray-Clay et al. 2009): The wind is most strongly generated at the planet’s dayside, and would be…”
Estimation of the XUV radiation onto close planets and their evaporation (2011, background): “Other models include different effects of EUV radiation in the atmosphere, and infrared cooling (Yelle, 2004; Tian et al.,2005; Garcı́a Muñoz, 2007; Murray-Clay et al., 2009), usually yielding smaller escape rates than Eq.”
PLANETARY POPULATION SYNTHESIS COUPLED WITH ATMOSPHERIC ESCAPE: A STATISTICAL VIEW OF EVAPORATION (2014, methodology): “Furthermore, Tian et al. (2005) showed that, in the energylimited model, the assumption that the incoming irradiation is absorbed inside a single layer is inaccurate because the absorption depth of the incident radiation depends on the wavelength.”
Atmospheric Escape and the Evolution of Close-In Exoplanets (2018, background): “Yelle (2004) and Tian et al. (2005)’s approach of a constant heating efficiency has been adopted by a wide number of further calculations studying both hot-Jupiters (Garćıa Muñoz 2007) and super-Earth/mini-Neptune mass planets (Lammer et al. 2013, 2014, 2016; Erkaev et al. 2013, 2016).”
Infrared Transmission Spectra for Extrasolar Giant Planets (2006, background): “…photochemistry, thermal properties, three-dimensional (3D) circulation simulations, cloud and condensate height, and escaping processes (e.g. Fortney et al.2003; Burrows et al. 2003; Liang et al. 2003; Lecavelier et al. 2004; Yelle 2004; Tian et al. 2005; Iro et al. 2005; Seager et al. 2005).”
The Evaporation Valley in the Kepler Planets (2017, background): “Planets with H/He-rich envelopes can be strongly evaporated by this irradiation (e.g. Yelle 2004; Tian et al. 2005; Murray-Clay et al. 2009; Owen & Jackson 2012; Johnstone et al. 2015; Erkaev et al. 2016), and indeed H/He evaporation has been observed from the low-mass planet GJ 436b (Kulow et al.…”
DISEQUILIBRIUM CARBON, OXYGEN, AND NITROGEN CHEMISTRY IN THE ATMOSPHERES OF HD 189733b AND HD 209458b (2011, background): “Hydrodynamic models (Yelle 2004; Tian et al. 2005; Garćıa Muñoz 2007) show that the atmosphere should be close to hydrostatic equilibrium below 2-3Rp, with the base of the planetary wind usually being located near the 1-nbar level (see also the discussion in Koskinen et al. 2010).”
Can Planets Survive Stellar Evolution? (2007, methodology): “Note that Tian et al. (2005) have shown that the position of the exobase for the extended atmosphere of HD 209458b is close to ¼ 10.”
A diagram to determine the evaporation status of extrasolar planets (2006, background): “Different detailed models have been developed to understand the observed evaporation process and to estimate the escape rate (e.g., Yelle 2004; Tian et al. 2005; García Muñoz 2006), to be compared with the observational constrains (Vidal-Madjar et al. 2003, 2004).”
Planetary evaporation by UV and X‐ray radiation: basic hydrodynamics (2012, methodology): “…a streamline connecting planet and star in a frame co-rotating with the planet using similar model setups to previous hydrodynamic models (e.g. Tian et al. 2005; Penz et al. 2008; Murray-Clay et al. 2009), although we do not assume a fixed heating efficiency for the X-rays are rather…”
Origin and loss of nebula-captured hydrogen envelopes from ‘sub’- to ‘super-Earths’ in the habitable zone of Sun-like stars (2014, background): “…is exposed to an XUV flux which is ∼100 times higher compared to today’s solar value, the upper atmosphere will not be in hydrostatic equilibrium but will hydrodynamically expand up to several planetary radii (e.g., Watson et al. 1981; Tian et al. 2005; Erkaev et al. 2013a; Lammer et al. 2013a).”
Hydrodynamic planetary thermosphere model: 1. Response of the Earth's thermosphere to extreme solar EUV conditions and the significance of adiabatic cooling (2008, methodology): “The upper atmospheres of hydrogen-rich and water-rich early terrestrial planets [e.g., Watson et al. ,1 981;Kasting and Pollack ,1 983; Chassefie`re, 1996; Tian et al., 2005b], those of close-in extrasolar planets [e.g., Lammer et al., 2003; Yelle, 2004; Tian et al., 2005a; Garco´a-Mun˜oz, 2007], ”
The Cosmic Shoreline: The Evidence that Escape Determines which Planets Have Atmospheres, and what this May Mean for Proxima Centauri B (2017, unknown): “…et al. 2004; Yelle 2004; Tian et al. 2005; Erkaev et al. 2007; Garcia-Munoz 2007; Koskinen et al. 2009; Lammer et al. 2009; Murray-Clay et al. 2009; Tian 2009; Erkaev et al. 2013; Koskinen et al. 2013; Lammer et al. 2013; Owen and Wu 2013; Koskinen et al. 2014; Lammer et al. 2014; 1…”
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 reality, the regime of atmospheric escape for a specific planet, and the heating efficiencies in each regime would depend on the specific planetary mass, radius, atmospheric composition, and the stellar flux and would thus change with time (Yelle 2004; Tian et al. 2005; Owen & Jackson 2012).”
ATMOSPHERIC ESCAPE FROM HOT JUPITERS (2008, methodology): “For alternate numerical methods, see Tian et al. (2005) and Garćıa Muñoz (2007).”
Evaporation of the planet HD 189733b observed in H I Lyman-α (2010, background): “…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 2009; Murray-Clay et al. 2009).”