Infrared collision-induced and far-line absorption in dense CO2 atmospheres

By R. Wordsworth, Francois Forget, Vincent Eymet. 2010

144 citations recorded by the source corpus.

Subfields: Atmospheric Science, Global and Planetary Change

View Paper: https://www.semanticscholar.org/paper/bb75f181f5dd1e27c7a4e8b66a672a827d47dc11

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Citations in the corpus

Evolved Climates and Observational Discriminants for the TRAPPIST-1 Planetary System (2018, methodology): “Collision-induced absorption data are used for CO2–CO2 (Moore 1972; Kasting et al. 1984; Gruszka & Borysow 1997; Baranov et al. 2004; Wordsworth et al. 2010; Lee et al. 2016), N2–N2 (Schwieterman et al. 2015 based on Lafferty et al. 1996), and O2–O2 (Greenblatt et al. 1990; Hermans et al. 1999;…”
Modeling climate diversity, tidal dynamics and the fate of volatiles on TRAPPIST-1 planets (2017, methodology): “Minimum CO2 content required for surface habitability Using 3D and 1D (with our one-dimensional cloud-free climate model (Wordsworth et al. 2010c) that uses the same physical package than the 3-”
HABITABLE ZONES AROUND MAIN-SEQUENCE STARS: NEW ESTIMATES (2013, methodology): “Wordsworth et al. (2010) used 22 layers in their model, compared to 70 layers in our SMART comparison climate models.”
The faint young Sun problem (2012, background): “A further complication arises from uncertainties in radiative transfer calculations for atmospheres rich in carbon dioxide [Halevy et al., 2009; Wordsworth et al., 2010].”
GLIESE 581D IS THE FIRST DISCOVERED TERRESTRIAL-MASS EXOPLANET IN THE HABITABLE ZONE (2011, methodology): “Eccentricity was set to zero in the simulations we present here, with the stellar flux set to the true value at a = 0.22 and not increased to account for orbital averaging as in our 1D study (Wordsworth et al. 2010b).”
Comparison of “warm and wet” and “cold and icy” scenarios for early Mars in a 3‐D climate model (2015, methodology): “The latter is solved using a two-stream approach [Toon et al., 1989] with optical data derived from line-by-line calculations [Rothman et al., 2009] and interpolated collision-induced absorption data [Clough et al., 1989; Gruszka and Borysow, 1998; Baranov et al., 2004; Wordsworth et al., 2010a].”
Transient reducing greenhouse warming on early Mars (2016, unknown): “…Cohen and Roothaan , 1965; Clough et al. , 1992; Rothman et al. , 2013; Murphy and Koop , 2005; Gruszka and Borysow , 1997; Baranov et al. , 2004; Wordsworth et al. , 2010; Pierrehumbert , 2011; Hansen and Travis , 1974; Claire et al. , 2012; Béguier et al. , 2015; Goldblatt et al. , 2013;…”
The habitability of Proxima Centauri b II. Possible climates and Observability (2016, methodology): “The GCM includes an up-to-date generalized radiative transfer (Rothman et al. 2009; Wordsworth et al. 2010; Richard et al. 2012) for variable gaseous atmospheric compositions made of various cocktails of CO2, N2 and H2O, using the correlated-k method (Fu & Liou 1992; Eymet et al. 2016).”
Update of the HITRAN collision-induced absorption section (2019, unknown): “It was shown by Wordsworth et al. (2010), that many atmospheric models are sensitive to absorption in the 250 – 500cm − 1 window, particularly when the atmospheric abundance of H 2 O is low, as is the case on Venus and Mars.”
The Climate of Early Mars (2016, unknown): “While possible, this is unlikely, because such high 6 Robin Wordsworth mass loss is not observed in any nearby G or K class stars (Minton & Malhotra 2007).”
Habitable Moist Atmospheres on Terrestrial Planets near the Inner Edge of the Habitable Zone around M Dwarfs (2017, background): “There is an extensive literature on modeling and speculating on the potential habitability of terrestrial planets in the HZ (Selsis et al. 2007; Wordsworth et al. 2010; Abe et al. 2011; Haqq-Misra & Kopparapu 2015; Barnes et al. 2016; Meadows et al. 2016; Ribas et al. 2016; Turbet et al. 2016;…”
HABITABLE ZONES AROUND MAIN-SEQUENCE STARS: DEPENDENCE ON PLANETARY MASS (2014, background): “Several other recent studies used 3D global circulation models (GCMs) to study the po- tential habitability of specific systems (Wordsworth et al. 2010; Forget et al. 2013).”
WATER LOSS FROM TERRESTRIAL PLANETS WITH CO2-RICH ATMOSPHERES (2013, unknown): “Low atmosphere heating is generally even stronger around M-stars than G-stars, because the redshift in the stellar radiation increases absorption and decreases the importance of Rayleigh scattering (e.g., Kasting et al. 1993; Wordsworth et al. 2010b).”
Observing the Atmospheres of Known Temperate Earth-sized Planets with JWST (2017, background): “…molecule pairs including N2–N2, O2–O2, CO2–CO2, and N2–CH4 (Bezard et al. 1990; Borysow & Tang 1993; Lafferty et al. 1996; Gruszka & Borysow 1997; Baranov et al. 2004; Wordsworth et al. 2010; Lee et al. 2016; Hartmann et al. 2017), as well as hydrogen and helium CIA opacities (Richard et al. 2012).”
3D modelling of the early Martian Climate under a denser CO2 atmosphere: Temperatures and CO2 ice clouds. (2012, methodology): “The method is described and justified in Wordsworth et al. (2010).”