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Characterizing 51 Eri b from 1 to 5 μm: A Partly Cloudy Exoplanet

  • Authors: Abhijith Rajan, Julien Rameau, Robert J. De Rosa, Mark S. Marley, James R. Graham, Bruce Macintosh, Christian Marois, Caroline Morley, Jennifer Patience, Laurent Pueyo, Didier Saumon, Kimberly Ward-Duong, S. Mark Ammons, Pauline Arriaga, Vanessa P. Bailey, Travis Barman, Joanna Bulger, Adam S. Burrows, Jeffrey Chilcote, Tara Cotten, Ian Czekala, Rene Doyon, Gaspard Duchêne, Thomas M. Esposito, Michael P. Fitzgerald, Katherine B. Follette, Jonathan J. Fortney, Stephen J. Goodsell, Alexandra Z. Greenbaum, Pascale Hibon, Li-Wei Hung, Patrick Ingraham, Mara Johnson-Groh, Paul Kalas, Quinn Konopacky, David Lafrenière, James E. Larkin, Jérôme Maire, Franck Marchis, Stanimir Metchev, Maxwell A. Millar-Blanchaer, Katie M. Morzinski, Eric L. Nielsen, Rebecca Oppenheimer, David Palmer, Rahul I. Patel, Marshall Perrin, Lisa Poyneer, Fredrik T. Rantakyrö, Jean-Baptiste Ruffio, Dmitry Savransky, Adam C. Schneider, Anand Sivaramakrishnan, Inseok Song, Rémi Soummer, Sandrine Thomas, Gautam Vasisht, J. Kent Wallace, Jason J. Wang, Sloane Wiktorowicz, and Schuyler Wolff

2017 The Astronomical Journal 154 10.

  • Provider: AAS Journals

Caption: Figure 16.

Luminosity of imaged planetary-mass companions as a function of age. For 51 Eri b, the red star is the inferred luminosity from the iron/silicate model grid, while the green square is the inferred luminosity from the sulfide/salt model grid. Also plotted are evolutionary tracks assuming different starting conditions: the “hot-start” (dotted lines) and “cold-start” (solid lines) models of Marley et al. (2007) and Fortney et al. (2008). 51 Eri b is consistent with both hot- and cold-start formation models. A subset of known, directly imaged companions are plotted in the figure, illustrating the difference between 51 Eri b and other imaged planets. Data for the companions, 2M1207 b, HR8799 bcde, HD 95086 b, and GJ 504 b, were taken from Patience et al. (2010), Rajan et al. (2015), Zurlo et al. (2016), De Rosa et al. (2016), and Skemer et al. (2016), respectively.

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