The direct detection of the irradiated brown dwarf in the white dwarf–brown dwarf binary SDSS J141126.20+200911.1

Casewell, Sarah L.; Littlefair, S. P.; Parsons, S. G.; Marsh, T. R.; Fortney, Jonathan J.; Marley, Mark S.

doi:10.1093/mnras/sty2599

Cited by 28 publications

(51 citation statements)

References 43 publications

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“…In both phase curves, 0 and 1 represent the times when the brown dwarf's dayside is aimed toward Earth, whereas phase 0.5 and 1.5 represent times when its nightside is aimed toward Earth. From EPIC 21223532 (Casewell et al 2018a), WD1202-024 (Rappaport et al 2017) and SDSS J141126.20+200911.1 (Littlefair et al 2014;Casewell et al 2018b).…”

Section: Irradiated Brown Dwarfsmentioning

confidence: 99%

“…Future endeavors beyond the above idealized work are needed to obtain a completed understanding on the 3D atmospheres of this group of objects. The spectrum of white dwarfs peak at UV, and significant photochemistry are expected to occur in atmospheres of the com-panion BDs (Longstaff et al 2017;Casewell et al 2018b). Effects of photochemical products and radiative heating on the thermal structures and circulation, along with the effects of hydrogen thermal dissociation/recombination similar to those found in ultra-hot Jupiter atmospheres (Bell and Cowan 2018;Komacek and Tan 2018;Tan and Komacek 2019), are worth to explored in a thorough manner.…”

Section: Irradiated Brown Dwarfsmentioning

confidence: 99%

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Atmospheric Dynamics of Hot Giant Planets and Brown Dwarfs

2020

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Groundbased and spacecraft telescopic observations, combined with an intensive modeling effort, have greatly enhanced our understanding of hot giant planets and brown dwarfs over the past ten years. Although these objects are all fluid, hydrogen worlds with stratified atmospheres overlying convective interiors, they exhibit an impressive diversity of atmospheric behavior. Hot Jupiters are strongly irradiated, and a wealth of observations constrain the day-night temperature differences, circulation, and cloudiness. The intense stellar irradiation, presumed tidal locking and modest rotation leads to a novel regime of strong day-night radiative forcing. Circulation models predict large day-night temperature differences, global-scale eddies, patchy clouds, and, in most cases, a fast eastward jet at the equator—equatorial superrotation. The warm Jupiters lie farther from their stars and are not generally tidally locked, so they may exhibit a wide range of rotation rates, obliquities, and orbital eccentricities, which, along with the weaker irradiation, leads to circulation patterns and observable signatures predicted to differ substantially from hot Jupiters. Brown dwarfs are typically isolated, rapidly rotating worlds; they radiate enormous energy fluxes into space and convect vigorously in their interiors. Their atmospheres exhibit patchiness in clouds and temperature on regional to global scales—the result of modulation by large-scale atmospheric circulation. Despite the lack of irradiation, such circulations can be driven by interaction of the interior convection with the overlying atmosphere, as well as self-organization of patchiness due to cloud-dynamical-radiative feedbacks. Finally, irradiated brown dwarfs help to bridge the gap between these classes of objects, experiencing intense external irradiation as well as vigorous interior convection. Collectively, these diverse objects span over six orders of magnitude in intrinsic heat flux and incident stellar flux, and two orders of magnitude in rotation rate—thereby placing strong constraints on how the circulation of giant planets (broadly defined) depend on these parameters. A hierarchy of modeling approaches have yielded major new insights into the dynamics governing these phenomena.

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Section: Irradiated Brown Dwarfsmentioning

confidence: 99%

Section: Irradiated Brown Dwarfsmentioning

confidence: 99%

Atmospheric Dynamics of Hot Giant Planets and Brown Dwarfs

2020

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“…1 in [46]). White dwarf-brown dwarf binaries can be seen as analogues to short-period giant gas planets [27]. The ionization processes in brown dwarf and exoplanet atmospheres are determined by their individual environments and more locally by the objects' character (size, mass, age) itself.…”

Section: Ionization Processes On Exoplanets and Brown Dwarfsmentioning

confidence: 99%

Lightning and charge processes in brown dwarf and exoplanet atmospheres

Helling

Rimmer

2019

Phil. Trans. R. Soc. A.

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The study of the composition of brown dwarf atmospheres helped to understand their formation and evolution. Similarly, the study of exoplanet atmospheres is expected to constrain their formation and evolutionary states. We use results from three-dimensional simulations, kinetic cloud formation and kinetic ion-neutral chemistry to investigate ionization processes that will affect their atmosphere chemistry: the dayside of super-hot Jupiters is dominated by atomic hydrogen, and not H 2 O. Such planetary atmospheres exhibit a substantial degree of thermal ionization and clouds only form on the nightside where lightning leaves chemical tracers (e.g. HCN) for possibly long enough to be detectable. External radiation may cause exoplanets to be enshrouded in a shell of highly ionized, H 3 + -forming gas and a weather-driven aurora may emerge. Brown dwarfs enable us to study the role of electron beams for the emergence of an extrasolar, weather system-driven aurora-like chemistry, and the effect of strong magnetic fields on cold atmospheric gases. Electron beams trigger the formation of H 3 + in the upper atmosphere of a brown dwarf (e.g. LSR-J1835), which may react with it to form hydronium, H 3 O + , as a longer lived chemical tracer. Brown dwarfs and super-hot gas giants may be excellent candidates to search for H 3 O + as an H 3 + product. This article is part of a discussion meeting issue ‘Advances in hydrogen molecular ions: H 3 + , H 5 + and beyond’.

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“…Often, the brown dwarf atmospheres in these systems are affected by the intense irradiation from their host star, resulting in large atmospheric differences between the day and night sides (Beatty et al 2019) which can include emission lines from a chromosphere on the brown dwarf (e.g. Longstaff et al 2017), or signs of photochemistry (Casewell et al 2018(Casewell et al , 2015. In many of these brown dwarfs orbiting main sequence stars, the brown dwarf is also inflated, meaning these binaries are unsuitable to use as benchmark systems to test the brown dwarf mass-radius relation.…”

Section: Introductionmentioning

confidence: 99%

WD1032 + 011, an inflated brown dwarf in an old eclipsing binary with a white dwarf

Casewell

Belardi

Parsons

et al. 2020

Monthly Notices of the Royal Astronomical Society

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We present the discovery of only the third brown dwarf known to eclipse a non-accreting white dwarf. Gaia parallax information and multi-colour photometry confirm that the white dwarf is cool (9950±150 K) and has a low mass (0.45±0.05 M⊙), and spectra and lightcurves suggest the brown dwarf has a mass of 0.067 ±0.006 M⊙ (70 MJup) and a spectral type of L5±1. The kinematics of the system show that the binary is likely to be a member of the thick disk and therefore at least 5 Gyr old. The high cadence lightcurves show that the brown dwarf is inflated, making it the first brown dwarf in an eclipsing white dwarf-brown dwarf binary to be so.

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The direct detection of the irradiated brown dwarf in the white dwarf–brown dwarf binary SDSS J141126.20+200911.1

Cited by 28 publications

References 43 publications

Atmospheric Dynamics of Hot Giant Planets and Brown Dwarfs

Atmospheric Dynamics of Hot Giant Planets and Brown Dwarfs

Lightning and charge processes in brown dwarf and exoplanet atmospheres

WD1032 + 011, an inflated brown dwarf in an old eclipsing binary with a white dwarf

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