Principles of Planetary Climate

By R. Pierrehumbert. 2010

231 citations recorded by the source corpus.

Subfields: Astronomy and Astrophysics, Atmospheric Science

View Paper: https://www.semanticscholar.org/paper/3a2f5bd12831e768cd49da1184f2aeff82dff49c

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. E. Wolf
2. R. Kopparapu
3. J. Kasting
4. E. Gaidos
5. Giada N. Arney
6. J. Johnson
7. V. Meadows
8. T. Robinson

In Atmospheric Science

1. J. Kasting
2. T. Robinson
3. Jun Yang
4. Dorian S. Abbot
5. K. Zahnle
6. N. Cowan
7. R. Kopparapu
8. James Schottelkotte

Citations in the corpus

• Low simulated radiation limit for runaway greenhouse climates (2013, background): “Everything else being equal, a Mars size planet would be more susceptible to a runaway greenhouse and a so-called “superEarth” less[11].”
• Habitable Moist Atmospheres on Terrestrial Planets near the Inner Edge of the Habitable Zone around M Dwarfs (2017, background): “Several studies have shown that the variation in the non-condensable gas fraction in the atmosphere (specifically the N2 amount) can affect the OLR, and consequently the habitability limits through moist and runaway greenhouse (Nakajima et al. 1992; Pierrehumbert 2010; Wordsworth & Pierrehumbert 201”
• STABILIZING CLOUD FEEDBACK DRAMATICALLY EXPANDS THE HABITABLE ZONE OF TIDALLY LOCKED PLANETS (2013, methodology): “Cloud infrared scattering is not included as it is negligible (Fu et al. 1997) due to high infrared absorption by water clouds (Pierrehumbert 2010).”
• WATER LOSS FROM TERRESTRIAL PLANETS WITH CO2-RICH ATMOSPHERES (2013, unknown): “on at wavelengths below 91 nm with an ionization heating eciency of 0.15-0.3 (Chasseere 1996; Murray-Clay et al. 2009), and has a low collision cross-section, leading to high thermal conductivity (Pierrehumbert 2010). To calculate an upper limit on H escape below the adiabatic blowo temperature, we ”
• HABITABLE ZONES AROUND MAIN-SEQUENCE STARS: DEPENDENCE ON PLANETARY MASS (2014, methodology): “A similar calculation performed by Pierrehumbert (2010) shows a distinctive peak in the OLR for low pN2, whereas our model does not show this feature.”
• The Habitability of Planets Orbiting M-dwarf Stars (2016, background): “…of Rayleigh scattering then dominate over the greenhouse effect of increased CO2, and temperatures above the freezing point of water can no longer be maintained by increasing CO2 (Kasting et al., 1993; Underwood et al., 2003; Pierrehumbert, 2010; Kane & Gelino, 2012; Kopparapu et al., 2013a,b).”
• HYDROGEN GREENHOUSE PLANETS BEYOND THE HABITABLE ZONE (2011, background): “As expected for a gas with frequency-dependent absorptivity, the stratospheric temperature is somewhat (few K) below the grey-gas skin temperature Teff/2 1/4, where σT 4eff = OLR = 1 4 (1− α)L (Pierrehumbert (2010), Chapter 4).”
• HABITABLE ZONES AROUND MAIN-SEQUENCE STARS: NEW ESTIMATES (2013, background): “4.37 of Pierrehumbert (2010) for a planet saturated with pure water vapor atmosphere and with a surface gravity of 10ms−2.”