Results 1 to 10 of about 43,562 (319)
arXiv, 1998 After a discussion of the physical processes in brown dwarfs, we present a complete, precise definition of brown dwarfs and of planets inspired by the internal physics of objects between 0.1 and 0.001 M_sun. We discuss observational techniques for characterizing low-luminosity objects as brown dwarfs, including the use of the lithium test and cooling ...
Oppenheimer, Ben R. +2 more
arxiv +3 more sources
The Formation Mechanism of Brown Dwarfs [PDF]
Mon.Not.Roy.Astron.Soc. 332 (2002) L65, 2002 We present results from the first hydrodynamical star formation calculation to demonstrate that brown dwarfs are a natural and frequent product of the collapse and fragmentation of a turbulent molecular cloud. The brown dwarfs form via the fragmentation of dense molecular gas in unstable multiple systems and are ejected from the dense gas before they ...
Matthew R. Bate +4 more
arxiv +6 more sources
Exploring brown dwarf disks [PDF]
Astronomy & Astrophysics, 2001 4 pages, 4 figures, A&A Letters in ...
A. Natta, L. Testi
openalex +6 more sources
The "Extra-Solar Giant Planets" are Brown Dwarfs [PDF]
arXiv, 2001 After an M, K, G, or F star forms, it magnetically compresses the infall dregs to produce a close in brown dwarf.
Robert L. Kurucz
arxiv +3 more sources
The only inflated brown dwarf in an eclipsing white dwarf-brown dwarf binary: WD1032+011B [PDF]
arXivDue to their short orbital periods and relatively high flux ratios, irradiated brown dwarfs in binaries with white dwarfs offer better opportunities to study irradiated atmospheres than hot Jupiters, which have lower planet-to-star flux ratios. WD1032+011 is an eclipsing, tidally locked white dwarf-brown dwarf binary with a 9950 K white dwarf orbited ...
Jenni R French +11 more
arxiv +3 more sources
On the Formation of Brown Dwarfs [PDF]
The Astronomical Journal, 2004 AbstractThe observational properties of brown dwarfs pose challenges to the theory of star formation. Because their masses are much smaller than the typical Jeans mass of interstellar clouds, brown dwarfs are most likely formed through secondary fragmentation processes, rather than through the direct collapse of a molecular cloud core.
Douglas N. C. Lin +2 more
openaire +5 more sources
Brown dwarf accretion: Nonconventional star formation over very long timescales [PDF]
Serbian Astronomical Journal, 2005 We investigate the process of accretion of interstellar gas by the Galactic population of brown dwarfs over very long timescales typical for physical eschatology.
Ćirković Milan M.
doaj +1 more source
Disks around Young Planetary-mass Objects: Ultradeep Spitzer Imaging of NGC 1333
The Astronomical Journal, 2023 We report on a sensitive infrared search for disks around isolated young planetary-mass objects (PMOs) in the NGC 1333 cluster, by stacking 70 Spitzer/IRAC frames at 3.6 and 4.5 μ m.
Aleks Scholz +4 more
doaj +1 more source
Redder than Red: Discovery of an Exceptionally Red L/T Transition Dwarf
The Astrophysical Journal Letters, 2023 We present the discovery of CWISE J050626.96+073842.4 (CWISE J0506+0738), an L/T transition dwarf with extremely red near-infrared colors discovered through the Backyard Worlds: Planet 9 citizen science project. Photometry from UKIRT and CatWISE give a (
Adam C. Schneider +26 more
doaj +1 more source
The formation of brown dwarfs [PDF]
Astronomische Nachrichten, 2005 AbstractWe review four mechanisms for forming brown dwarfs: (i) turbulent fragmentation (producing very low‐mass prestellar cores); (ii) gravitational instabilities in discs; (iii) dynamical ejection of stellar embryos from their placental cores; and (iv) photo‐erosion of pre‐existing cores in HII regions.
Anthony Peter Whitworth +1 more
openaire +4 more sources