The theory of brown dwarfs and extrasolar giant planets

By Adam Burrows, W. Hubbard, Jonathan I. Lunine, J. Liebert. 2001

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Straddling the traditional realms of the planets and the stars, objects below the edge of the main sequence have such unique properties, and are being discovered in such quantities, that one can rightly claim that a new field at the interface of planetary science and astronomy is being born. This article extends the previous review of Burrows and Liebert (1993) and describes the essential elements of the theory of brown dwarfs and giant planets. It discusses their evolution, atmospheric composition, and spectra, including the new spectroscopic classes L and T. Particular topics which are important for an understanding of the spectral properties include the effects of condensates, clouds, molecular abundances, and atomic opacities. Moreover, it discusses the distinctive features of these extrasolar giant planets that are irradiated by a central primary, in particular, their reflection spectra, albedos, and transits. Overall, the theory explains the basic systematics of substellar-mass objects over three orders of magnitude in mass and age, and a factor of 30 in temperature.

Subfields: Astronomy and Astrophysics

View Paper: https://www.semanticscholar.org/paper/53821394a8266f0835a616a11e66ff177a3232a2

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Citations in the corpus

THE HAWAII INFRARED PARALLAX PROGRAM. II. YOUNG ULTRACOOL FIELD DWARFS (2016, background): “Theory predicts that the radii of substellar objects cease contracting by ∼300 Myr (e.g. Burrows et al. 2001), but accurate predictions about the time-evolution of gravity-sensitive features leading up to this cessation are beyond current models.”
Formation of the Galilean Satellites: Conditions of Accretion (2002, background): “Recent models predict a full-mass Jupiter would require 106 yr to contract to Rp 1:9RJ, at which time it would have an effective temperature 800 K (e.g., Burrows et al. 1997, 2001); by 107 yr, Rp 1:5RJ and Teff 500 K (e.g., Hubbard, Burrows, & Lunine 2002).”
BANYAN. II. VERY LOW MASS AND SUBSTELLAR CANDIDATE MEMBERS TO NEARBY, YOUNG KINEMATIC GROUPS WITH PREVIOUSLY KNOWN SIGNS OF YOUTH (2013, background): “…old limit compared to the oldest NYA considered (ABDMG at 70 – 130 Myr) is that BDs (especially objects with masses around ∼ 80 MJup) significantly younger than 1 Gyr might not have reached their equilibrium radius yet (Burrows et al. 2001), which means that they could display signs of low-gravity.”
NEGLECTED CLOUDS IN T AND Y DWARF ATMOSPHERES (2012, background): “Burrows et al. (2001, 2002) noted that Na2S and KCl will condense in cool T dwarfs, but also noted that the indices of refraction are difficult to find.”
Toward Spectral Classification of L and T Dwarfs: Infrared and Optical Spectroscopy and Analysis (2001, background): “It is probably not due to continuum emission from dust (Allard et al. 2001 ; Marley & Ackerman 2001 ; Burrows et al. 2001 ; Tsuji 2001), which would dilute the strength of the band, because a similar e†ect is not seen in the nearby 2.2 km methane band.”
White Dwarf Donors in Ultracompact Binaries: The Stellar Structure of Finite-Entropy Objects (2003, background): “For H-rich objects, Burrows et al. (2001) summarize the work that has been done on the structure and evolution of brown dwarfs and related objects.”
Individual Dynamical Masses of Ultracool Dwarfs (2017, background): “…based on theoretical work over the last two decades (e.g., Saumon et al. 1994; Baraffe et al. 1995; Burrows et al. 1997; Chabrier & Baraffe 1997; Lodders 1999; Chabrier et al. 2000; Burrows et al. 2001; Baraffe et al. 2003; Saumon & Marley 2008; MacDonald & Mullan 2009; Baraffe et al. 2015).”
Hubble Space Telescope hot Jupiter transmission spectral survey: a detection of Na and strong optical absorption in HAT-P-1b (2013, background): “…assume solar metallicity and local thermodynamical chemical equilibrium accounting for condensation with no ionisation, using the opacity c© 2013 RAS, MNRAS 000, 1–?? database from Sharp & Burrows (2007) and the equilibrium chemical abundances from Burrows & Sharp (1999) and Burrows et al. (2001).”
Imaging Extrasolar Giant Planets (2016, background): “35; Burrows & Liebert 1993; Burrows et al. 2001).”
The Ages of Stars (2007, background): “Many papers and reviews have described the HK observations and their reduction to a physically relevant quantity, R′ HK , the ratio of the HK flux to Lbol, corrected for photospheric light in the bandpasses (hence the prime; see Noyes et al. (1984)).”
THE DEUTERIUM-BURNING MASS LIMIT FOR BROWN DWARFS AND GIANT PLANETS (2010, methodology): “…brown dwarfs were improved by the application of nongray radiative transfer theory (Burrows et al. 1997, 1998; Burrows & Sharp 1999; Burrows 1999; Burrows et al. 2001, 2003; Baraffe et al. 2002, 2003; Allard et al. 2003; Chabrier et al. 2000b,a; Chabrier & Baraffe 2000; Sharp & Burrows 2007;…”
MODULES FOR EXPERIMENTS IN STELLAR ASTROPHYSICS (MESA) (2010, background): “1997; Chabrier et al. 2000; Chabrier & Baraffe 2000; Burrows et al. 2001) has been studied extensively.”
The First Substellar Subdwarf? Discovery of a Metal-poor L Dwarf with Halo Kinematics (2003, methodology): “To test this hypothesis, we compared the estimated Teff of this object with subsolar metallicity evolutionary models from Burrows et al. (2001).”
Activity and Kinematics of Ultracool Dwarfs, Including an Amazing Flare Observation (2007, background): “Kinematics allow us to investigate the age distribution of our sample; the ages of L dwarfs are of particular interest because the spectral class encompasses both stellar and substellar objects (Burrows et al. 2001).”
The Cosmic Energy Inventory (2004, unknown): “We similarly obtain the substellar gravitational binding energy, ΩBE = −10 −9.6, where r is fixed at 0.096 r⊙ (Burrows et al. 2001).”