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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 9.

The J vs. J − H brown dwarf and imaged exoplanet color–magnitude diagram reproduced from Figure 5. The photometry for 51 Eri b is shown with the red star. Also plotted on the CMD are the evolutionary tracks for 5 and 14 ﹩{M}_{\mathrm{Jup}}﹩ objects (Marley et al. 2012), with the solid red line and dashed black line, respectively. The models assume a simple gravity dependence for the initiation of the transition. A few ages for the 5 ﹩{M}_{\mathrm{Jup}}﹩ track have been overplotted. The L–T transition for the 5 ﹩{M}_{\mathrm{Jup}}﹩ planet starts at approximately 900 K and 20 Myr, but for a lower-mass planet such as 51 Eri b, it will occur at younger ages.

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