Aeronomy of extra-solar giant planets at small orbital distances

By R. Yelle. 2003

430 citations recorded by the source corpus.

View Paper: https://www.semanticscholar.org/paper/5cb0e4f01206164ca30435f6bc412b02c8e49927

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In Astronomy and Astrophysics

Citations in the corpus

OBSERVATIONS OF MASS LOSS FROM THE TRANSITING EXOPLANET HD 209458b (2010, methodology): “For example, Yelle (2004), as corrected in Yelle (2006), finds Ṁ = 4.7× 1010, Tian et al. (2005) find Ṁ < 6 × 1010, Garcia Muñoz (2007) finds Ṁ = 6.1 × 1010 for EUV flux similar to the low activity Sun but Ṁ = 1.5 × 1011 for EUV flux like the active Sun.”
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).”
Planetary evaporation by UV and X‐ray radiation: basic hydrodynamics (2012, background): “However, both Yelle (2004) and Tian et al. (2005) use fixed heating efficiencies (for photo-electric heating in the case of Yelle 2004 and the total heating efficiency in the case of Tian et al. 2005).”
A New Window into Escaping Exoplanet Atmospheres: 10830 Å Line of Helium (2017, background): “Several groups have developed theoretical models of escaping atmospheres (e.g. Lammer et al. 2003; Yelle 2004; Garćıa Muñoz 2007; Murray-Clay, Chiang & Murray 2009; Koskinen et al. 2010; Bourrier & Lecavelier des Etangs 2013; Tripathi et al. 2015; Salz et al. 2016; Carroll-Nellenback et al. 2017).”
KEPLER PLANETS: A TALE OF EVAPORATION (2013, background): “On the theoretical side, there is a large body of literature discussing planet evaporation, ever since the first hot Jupiters were discovered (e.g. Lammer et al. 2003; Yelle 2004; Tian et al. 2005; Hubbard et al. 2007a,b; MurrayClay et al. 2009; Koskinen et al. 2010; Owen & Jackson 2012).”
Two Classes of Hot Jupiters (2007, background): “Inspection of the exospheremodels of Yelle (2004) indicates that the evaporatingwind from an irradiated planet consists of ionized hydrogen but neutral helium (for the exosphere temperatures 104 K lie between the ionization temperatures of the two atoms).”
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).”
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.”
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).”
Temperature–pressure profile of the hot Jupiter HD 189733b from HST sodium observations: detection of upper atmospheric heating (2012, methodology): “Lecavelier des Etangs et al. (2004) and Yelle (2004), modelling the upper atmosphere and atmospheric escape of HD 209458b, showed that temperatures in the thermosphere could reach up to 10,000 K.”
The Sun in Time: Activity and Environment (2007, methodology): “The initial calculations by Lammer et al. (2003b) led to very high mass-loss rates, initially criticized by Yelle (2004) who derived 20 times smaller escape rates by also including atmospheric chemistry in their calculations; in particular, they considered thermospheric cooling by H+3 and the…”
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).”
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).”
Spectrally resolved detection of sodium in the atmosphere of HD 189733b with the HARPS spectrograph (2015, background): “Our results suggest that a part of the sodium absorption occurs in the (lower) thermosphere, where heating by the stellar X/EUV photons occurs (Lammer et al. 2003; Yelle 2004; Vidal-Madjar et al. 2011; Koskinen et al. 2013).”
The Cosmic Shoreline: The Evidence that Escape Determines which Planets Have Atmospheres, and what this May Mean for Proxima Centauri B (2017, background): “tion (I xuv). The intent is to address the popular XUV-driven escape hypothesis (e.g., Hayashi et al. 1979; Sekiya et al. 1980a, 1981; Watson et al. 1981; Lammer et al. 2003a; Lecavelier et al. 2004; Yelle 2004; Tian et al. 2005; Erkaev et al. 2007; Garcia-Munoz 2007; Koskinen et al. 2009; Lammer et”
LYα TRANSIT SPECTROSCOPY AND THE NEUTRAL HYDROGEN TAIL OF THE HOT NEPTUNE GJ 436b (2014, background): “Yelle (2004) (later revised in Yelle 2006) included chemical calculations to estimate a mass-loss rate.”
The Hubble Space Telescope PanCET Program: Exospheric Mg ii and Fe ii in the Near-ultraviolet Transmission Spectrum of WASP-121b Using Jitter Decorrelation (2019, background): “These photons ionize atmospheric species and deposit enormous heat through electron collisions, that can greatly expand the upper atmosphere and drive hydrodynamic outflow and mass escape (Yelle 2004; Garćıa Muñoz 2007; Murray-Clay et al. 2009; Owen & Jackson 2012).”