Seeing Through the Clouds: Thermal Emission and Reflected Light Spectra of Super-Earths with Flat Transmission Spectra

By C. Morley, Jon Fortney, M. Marley, K. Zahnle, M. Line, Eliza Miller-Ricci Kempton, N. Lewis, Kerri L. Cahoy. 2015

151 citations recorded by the source corpus.

View Paper: https://www.semanticscholar.org/paper/0048872636b83842711b0350186187f5a6b33936

How researchers see this paper

The researchers whose trusted networks rank it highest, strongest advocate first. Every researcher gets a different order.

1. N. Madhusudhan
2. M. Line
3. Jon Fortney
4. V. Parmentier
5. D. Sing
6. A. Showman
7. H. Wakeford
8. Paul Mollière

Citations in the corpus

• NO THERMAL INVERSION AND A SOLAR WATER ABUNDANCE FOR THE HOT JUPITER HD 209458B FROM HST/WFC3 SPECTROSCOPY (2016, methodology): “The CHIMERA emission forward model computes the upwelling disk-integrated thermal emission given a temperature structure and molecular abundances and has been validated against other models in two publications (Line et al. 2013; Morley et al. 2015).”
• Pale Orange Dots: The Impact of Organic Haze on the Habitability and Detectability of Earthlike Exoplanets (2016, background): “Charnay et al. (2015) and Morley et al. (2015) show what a ZnS haze would look like in a more realistic atmosphere for GJ 1214b.”
• HST PanCET Program: A Cloudy Atmosphere for the Promising JWST Target WASP-101b (2017, methodology): “We use a sedimentation efficiency fsed = 0.1 (Morley et al. 2015) for both atmospheres and compare the optical depth of enstatite clouds over the critical pressures probed in transmission (Fig.4b).”
• THE INFLUENCE OF NONUNIFORM CLOUD COVER ON TRANSIT TRANSMISSION SPECTRA (2015, methodology): “…altitude opaque cloud in order to substantially flatten the spectra, a reasonable cloud top pressure in lieu of recently observed flat transmission spectra (Kreidberg et al. 2014, Knutson et al. 2014, Morley et al. 2012;2015) and GCM tracer studies (Parmentier et al. 2013, Charnay et al. 2015b).”
• SPITZER PHASE CURVE CONSTRAINTS FOR WASP-43b AT 3.6 AND 4.5 μm (2016, background): “Atmospheric temperatures in these regions are favorable for the production of optically thick clouds/hazes, as shown by Morley et al. (2015), and GCMs of planets with orbital periods of .”
• Observing transiting planets with JWST. Prime targets and their synthetic spectral observations (2016, methodology): “The need for clouds has been studied in detail in Morley et al. (2013); Kreidberg et al. (2014); Morley et al. (2015), where Morley et al. (2013, 2015) found that high atmospheric enrichments are necessary to fit the data.”
• Observing the Atmospheres of Known Temperate Earth-sized Planets with JWST (2017, methodology): “We calculate thermal emission spectra using the model described in the Appendix of Morley et al. (2015).”