Evolutionary models for cool brown dwarfs and extrasolar giant planets. The case of HD 209458

By Isabelle Baraffe, G. Chabrier, Travis S. Barman, F. Allard, Peter Hauschildt. 2003

1,344 citations recorded by the source corpus.

We present evolutionary models for cool brown dwarfs and extra-solar giant planets. The models re- produce the main trends of observed methane dwarfs in near-IR color-magnitude diagrams. We also present evolutionary models for irradiated planets, coupling for the first time irradiated atmosphere profiles and inner structures. We focus on HD 209458-like systems and show that irradiation effects can substantially affect the ra- dius of sub-jovian mass giant planets. Irradiation effects, however, cannot alone explain the large observed radius of HD 209458b. Adopting assumptions which optimise irradiation effects and taking into account the extension of the outer atmospheric layers, we still find � 20% discrepancy between observed and theoretical radii. An extra source of energy seems to be required to explain the observed value of the first transit planet.

Subfields: Astronomy and Astrophysics, Instrumentation, Statistical and Nonlinear Physics

View Paper: https://www.semanticscholar.org/paper/7c7c57ac90a187044700598786322963b5d0a879

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Citations in the corpus

New spectral types L and T (2005, methodology): “Interior models of low-mass stars and brown dwarfs have been constructed by Burrows et al. (1997), Chabrier et al. (2000), and Baraffe et al. (2003).”
Can Planets Survive Stellar Evolution? (2007, methodology): “In the calculation we have used mass-radius relations given by Baraffe et al. (2003) for nonirradiated extrasolar planets at 10 Gyr, and assumed that the exospheric temperature is given by equation (7).”
BANYAN. VII. A NEW POPULATION OF YOUNG SUBSTELLAR CANDIDATE MEMBERS OF NEARBY MOVING GROUPS FROM THE BASS SURVEY (2015, methodology): “The BT-Settl isochrones (Allard et al. 2013; Baraffe et al. 2003) do not reproduce this effect, as the young (≤ 100 Myr) and old (≥ 1 Gyr) isochrones do not cross in neither of the J, H or KS bands over the range of effective temperatures that correspond to the M and L spectral types (∼ 1300–3000…”
HD 147506b: A Supermassive Planet in an Eccentric Orbit Transiting a Bright Star (2007, background): “3 also shows a theoretical mass-radius relation for objects ranging from gas giant planets to stars (Baraffe et al. 1998, 2003).”
The Gemini Planet Imager Exoplanet Survey: Giant Planet and Brown Dwarf Demographics from 10 to 100 au (2019, methodology): “For all stars, using the COND models Baraffe et al. (2003), they find a 2σ upper limit of 25% on the occurrence rate of planets between 4–14MJup and 5–100 au, consistent with our results.”
A Moving Cluster Distance to the Exoplanet 2M1207b in the TW Hydrae Association (2005, methodology): “Using the constraints on luminosity and age (Chauvin et al. 2005), I interpolate masses from the non-gray evolutionary tracks of Burrows et al. (1997), the DUSTY tracks of Chabrier et al. (2000), and the COND tracks of Baraffe et al. (2003).”
The 3.6-8.0 μm Broadband Emission Spectrum of HD 209458b: Evidence for an Atmospheric Temperature Inversion (2007, background): “…planets are well-described by basic models of an irradiated hot Jupiter (Bodenheimer et al. 2001; Showman & Guillot 2002; Bodenheimer et al. 2003; Baraffe et al. 2003; Laughlin et al. 2005a; Burrows et al. 2007a), but there are currently four planets (HD 209458b, WASP-1b, TrES-2, and TrES-4)…”
AB INITIO EQUATIONS OF STATE FOR HYDROGEN (H-REOS.3) AND HELIUM (He-REOS.3) AND THEIR IMPLICATIONS FOR THE INTERIOR OF BROWN DWARFS (2014, methodology): “Given the measured masses we extracted the respective effective temperatures from the models of Baraffe et al. (2003).”
THE GEMINI/NICI PLANET-FINDING CAMPAIGN: THE FREQUENCY OF PLANETS AROUND YOUNG MOVING GROUP STARS (2013, methodology): “′′5, 1′′, 2′′, and 4′′ are presented in Figure 9 using the DUSTY models (Baraffe et al. 2002) and in Figure 10 using the COND models (Baraffe et al. 2003).”
THE EVOLUTION OF CATACLYSMIC VARIABLES AS REVEALED BY THEIR DONOR STARS (2011, methodology): “First, in K06 we adopted the M2–Teff relation suggested by the BCAH98 5 Gyr MS models down to Teff 2000 K, switching to the 1 Gyr “DUSTY” (Baraffe et al. 2002) and, ultimately, 1 Gyr “COND” (Baraffe et al. 2003) isochrones at lower temperatures.”
TWO WIDE PLANETARY-MASS COMPANIONS TO SOLAR-TYPE STARS IN UPPER SCORPIUS (2010, result): “The COND models (Baraffe et al. 2003) never predict sufficiently red J −K colors to match our observations, and indeed are not appropriate for objects with T > 1300K.”
The UKIRT Infrared Deep Sky Survey (UKIDSS) (2006, background): “…are 5 Myr theoretical isochrones shifted to a distance of 145pc, appropriate for the estimated age and distance of Upper Sco : BCAH98 or NextGen models (solid line; Baraffe et al. 1998), DUSTY or BCAH00 (dashed line; Chabrier et al. 2000), and COND03 (dotted line; Baraffe et al. 2003).”
The Field Substellar Mass Function Based on the Full-sky 20 pc Census of 525 L, T, and Y Dwarfs (2020, background): “Switching to the Baraffe et al. (2003) evolutionary code instead gives a similar result.”
MESA ISOCHRONES AND STELLAR TRACKS (MIST). I. SOLAR-SCALED MODELS (2016, methodology): “Torres et al. (2013) concluded that the predicted CMD locations of the four components in the Dartmouth models (Dotter et al. 2008) are better matched than those from the Lyon models (Baraffe et al. 2003), though their recently updated models (Baraffe et al. 2015) show good agreement with the observ”
New evolutionary models for pre-main sequence and main sequence low-mass stars down to the hydrogen-burning limit (2015, methodology): “Later generations of models included improved molecular linelists for various atmospheric absorbers, such as the AMES linelists used in the Dusty and Cond models (Chabrier et al., 2000; Allard et al., 2001; Baraffe et al., 2003), but they still show shortcomings (see §3.2).”