Exoplanets and Stellar Physics

Research group

Research theme

Sub department

About

Related research groups

HYDROGEN GREENHOUSE PLANETS BEYOND THE HABITABLE ZONE

The Astrophysical Journal Letters American Astronomical Society 734:1 (2011) l13

Authors:

Raymond Pierrehumbert, Eric Gaidos
More details from the publisher

Climate of the Neoproterozoic

Annual Review of Earth and Planetary Sciences Annual Reviews 39:1 (2011) 417-460

Authors:

RT Pierrehumbert, DS Abbot, A Voigt, D Koll
More details from the publisher

Transiting exoplanets from the CoRoT space mission: XVI. CoRoT-14b: An unusually dense very hot Jupiter

Astronomy and Astrophysics 528 (2011)

Authors:

B Tingley, M Endl, JC Gazzano, R Alonso, T Mazeh, L Jorda, S Aigrain, JM Almenara, M Auvergne, A Baglin, P Barge, AS Bonomo, P Bordé, F Bouchy, H Bruntt, J Cabrera, S Carpano, L Carone, WD Cochran, S Csizmadia, M Deleuil, HJ Deeg, R Dvorak, A Erikson, S Ferraz-Mello, M Fridlund, D Gandolfi, M Gillon, EW Guenther, T Guillot, A Hatzes, G Hébrard, A Léger, A Llebaria, H Lammer, C Lovis, PJ MacQueen, C Moutou, M Ollivier, A Ofir, M Pätzold, F Pepe, D Queloz, H Rauer, D Rouan, B Samuel, J Schneider, A Shporer, G Wuchterl

Abstract:

In this paper, the CoRoT ExoplanetScience Team announces its 14th discovery. Herein, we discuss the observations and analyses that allowed us to derive the parameters of this system: a hot Jupiter with a mass of 7.6 ± 0.6 Jupiter masses orbiting a solar-type star (F9V) with a period of only 1.5 d, less than 5 stellar radii from its parent star. It is unusual for such a massive planet to have such a small orbit: only one other known higher mass exoplanet orbits with a shorter period. © ESO 2011.
More details from the publisher
More details
Details from ArXiV

Initiation of a Marinoan Snowball Earth in a state-of-the-art atmosphere-ocean general circulation model

Climate of the Past Copernicus Publications 7:1 (2011) 249-263

Authors:

A Voigt, DS Abbot, RT Pierrehumbert, J Marotzke
More details from the publisher

The gemini nici planet-finding campaign: Discovery of a substellar L dwarf companion to the nearby young M dwarf CD-35 2722

Astrophysical Journal 729:2 (2011)

Authors:

Z Wahhaj, MC Liu, BA Biller, F Clarke, EL Nielsen, LM Close, T Hayward, EE Mamajek, M Cushing, T Dupuy, M Tecza, N Thatte, M Chun, C Ftaclas, M Hartung, IN Reid, EL Shkolnik, SHP Alencar, P Artymowicz, A Boss, E De Gouveia Dal Pino, J Gregorio-Hetem, S Ida, M Kuchner, DNC Lin, DW Toomey

Abstract:

We present the discovery of a wide (67AU) substellar companion to the nearby (21pc) young solar-metallicity M1 dwarf CD-35 2722, a member of the ≈100Myr AB Doradus association. Two epochs of astrometry from the NICI Planet-Finding Campaign confirm that CD-35 2722B is physically associated with the primary star. Near-IR spectra indicate a spectral type of L4 ± 1 with a moderately low surface gravity, making it one of the coolest young companions found to date. The absorption lines and near-IR continuum shape of CD-35 2722B agree especially well the dusty field L4.5 dwarf 2MASS J22244381-0158521, while the near-IR colors and absolute magnitudes match those of the 5Myr old L4 planetary-mass companion, 1RXS J160929.1-210524 b. Overall, CD-35 2722B appears to be an intermediate-age benchmark for L dwarfs, with a less peaked H-band continuum than the youngest objects and near-IR absorption lines comparable to field objects. We fit Ames-Dusty model atmospheres to the near-IR spectra and find T eff= 1700-1900K and log(g)= 4.5 ± 0.5. The spectra also show that the radial velocities of components A and B agree to within ±10kms-1, further confirming their physical association. Using the age and bolometric luminosity of CD-35 2722B, we derive a mass of 31 ± 8 M Jup from the Lyon/Dusty evolutionary models. Altogether, young late-M to mid-L type companions appear to be overluminous for their near-IR spectral type compared with field objects, in contrast to the underluminosity of young late-L and early-T dwarfs. © 2011. The American Astronomical Society. All rights reserved.
More details from the publisher
More details
Details from ArXiV