Discovery of a Planetary-Mass Brown Dwarf with a Circumstellar Disk

2005 ◽  
Vol 635 (1) ◽  
pp. L93-L96 ◽  
Author(s):  
K. L. Luhman ◽  
Lucía Adame ◽  
Paola D'Alessio ◽  
Nuria Calvet ◽  
Lee Hartmann ◽  
...  
Keyword(s):  
Circumstellar Disk ◽  
Brown Dwarf ◽  
Planetary Mass

scholarly journals Spitzer Identification of the Least Massive Known Brown Dwarf with a Circumstellar Disk

2005 ◽  
Vol 620 (1) ◽  
pp. L51-L54 ◽  
Author(s):  
K. L. Luhman ◽  
Paola D'Alessio ◽  
Nuria Calvet ◽  
Lori E. Allen ◽  
Lee Hartmann ◽  
...  
Keyword(s):  
Circumstellar Disk ◽  
Brown Dwarf

scholarly journals Meridional Circulation of Dust and Gas in the Circumstellar Disk: Delivery of Solids onto the Circumplanetary Region

2022 ◽  
Vol 924 (1) ◽  
pp. 1
Author(s):  
J. Szulágyi ◽  
F. Binkert ◽  
C. Surville
Keyword(s):  
Meridional Circulation ◽  
Circumstellar Disk ◽  
Hydrodynamic Simulations ◽  
Planetary Mass ◽  
Accretion Rates ◽  
The Difference ◽  
Local Dust ◽  
Gas Accretion ◽  
The Hill ◽  
Gas Ratio

Abstract We carried out 3D dust + gas radiative hydrodynamic simulations of forming planets. We investigated a parameter grid of a Neptune-mass, a Saturn-mass, a Jupiter-mass, and a five-Jupiter-mass planet at 5.2, 30, and 50 au distance from their star. We found that the meridional circulation (Szulágyi et al. 2014; Fung & Chiang 2016) drives a strong vertical flow for the dust as well, hence the dust is not settled in the midplane, even for millimeter-sized grains. The meridional circulation will deliver dust and gas vertically onto the circumplanetary region, efficiently bridging over the gap. The Hill-sphere accretion rates for the dust are ∼10−8–10−10 M Jup yr−1, increasing with planet mass. For the gas component, the gain is 10−6–10−8 M Jup yr−1. The difference between the dust and gas-accretion rates is smaller with decreasing planetary mass. In the vicinity of the planet, the millimeter-sized grains can get trapped easier than the gas, which means the circumplanetary disk might be enriched with solids in comparison to the circumstellar disk. We calculated the local dust-to-gas ratio (DTG) everywhere in the circumstellar disk and identified the altitude above the midplane where the DTG is 1, 0.1, 0.01, and 0.001. The larger the planetary mass, the more the millimeter-sized dust is delivered and a larger fraction of the dust disk is lifted by the planet. The stirring of millimeter-sized dust is negligible for Neptune-mass planets or below, but significant above Saturn-mass planets.

scholarly journals The Substellar Population in σ Orionis

2003 ◽  
Vol 211 ◽  
pp. 111-118 ◽  
Author(s):  
M. R. Zapatero Osorio ◽  
D. Barrado y Navascués ◽  
V. J. S. Béjar ◽  
R. Rebolo ◽  
J. A. Caballero ◽  
...  
Keyword(s):  
Mass Range ◽  
Mass Function ◽  
Early Evolution ◽  
Brown Dwarf ◽  
Planetary Mass ◽  
Surface Temperatures ◽  
Mass Interval

The σ Orionis cluster (~3 Myr, 350 pc) is an ideal site to investigate the early evolution of substellar (brown dwarf and planetary mass) objects. To date, the cluster photometric and spectroscopic sequence of free-floaters is known for a wide mass range from 1 M⊙ down to roughly 3 MJup. The substellar domain covers spectral types that go from mid-M classes to the recently defined “methane” T-types, i.e., surface temperatures between ~3000K and 800 K. We derive a rising initial substellar mass function in the mass interval of 150–5 MJup (dN/dM ~ M-α, with α = 0.9 ± 0.4). We also find evidence for a extension of this mass function toward lower masses down to 2–3 MJup. This indicates that the population of isolated planetary mass objects with masses below the deuterium burning threshold is rather abundant in the cluster.

scholarly journals Searching for Planets of Brown Dwarfs

2003 ◽  
Vol 211 ◽  
pp. 225-232 ◽  
Author(s):  
Eike Guenther ◽  
Guenther Wuchterl
Keyword(s):  
High Probability ◽  
Brown Dwarfs ◽  
Surface Structures ◽  
Brown Dwarf ◽  
Low Mass Stars ◽  
Double Line ◽  
Normal Star ◽  
Spectroscopic Binary ◽  
Planetary Mass ◽  
Low Mass

Up to now, most planet search projects have concentrated on G and K stars. In order to considerably widen the view, we have stated a survey for planets of old, nearby brown dwarfs and very low-mass stars. Using UVES, we have observed 26 brown dwarfs and very low-mass stars. As it turned out these objects are very inactive and thus highly suitable for such a project. For 19 objects, we can exclude a planet with the mass of 3 MJ, and a period of 100 days or less with a probability of more than 60%. For these objects, we can also exclude Pegasi-planets with a high probability. For another 4 objects, we can exclude at least a brown dwarf companion. One object is a double line spectroscopic binary, and one object shows significant radial-velocity variations that can not be caused by a normal stellar-spot. This object either has a planetary-mass companion, or the variations are caused by surface structures that are quite different from normal star-spots.

scholarly journals THE FIRST BROWN DWARF/PLANETARY-MASS OBJECT IN THE 32 ORIONIS GROUP

2016 ◽  
Vol 820 (1) ◽  
pp. 32 ◽  
Author(s):  
Adam J. Burgasser ◽  
Mike A. Lopez ◽  
Eric E. Mamajek ◽  
Jonathan Gagné ◽  
Jacqueline K. Faherty ◽  
...  
Keyword(s):  
Brown Dwarf ◽  
Planetary Mass

scholarly journals DISCOVERY OF A PLANETARY-MASS COMPANION TO A BROWN DWARF IN TAURUS

2010 ◽  
Vol 714 (1) ◽  
pp. L84-L88 ◽  
Author(s):  
K. Todorov ◽  
K. L. Luhman ◽  
K. K. McLeod
Keyword(s):  
Brown Dwarf ◽  
Planetary Mass

scholarly journals Near-infrared Spectroscopy of Brown Dwarf and Planetary-Mass Members in Upper Scorpius

2015 ◽  
Vol 10 (S314) ◽  
pp. 255-258
Author(s):  
Nicolas Lodieu
Keyword(s):  
Infrared Spectroscopy ◽  
Near Infrared Spectroscopy ◽  
Near Infrared ◽  
Brown Dwarf ◽  
Planetary Mass ◽  
Moving Groups

AbstractIn these proceedings, I present new VLT/X-shooter near-infrared spectroscopy of brown dwarf and planetary-mass candidates with masses below 30 Jupiter masses identified in a deep VISTA ZYJ survey of 13.5 square degrees in the Upper Scorpius (USco) association. These spectra represent new benchmarks at 5–10 Myr to compare with known and future discoveries of members in nearby moving groups and other young regions.

scholarly journals SpS1-The evolution of brown dwarf infrared spectroscopic properties

2009 ◽  
Vol 5 (H15) ◽  
pp. 543-544
Author(s):  
France Allard ◽  
Isabelle Baraffe
Keyword(s):  
Brown Dwarfs ◽  
Spectroscopic Properties ◽  
Interstellar Cloud ◽  
Formation Mechanisms ◽  
Brown Dwarf ◽  
Burning Temperature ◽  
Planetary Mass ◽  
Infrared Spectroscopic ◽  
Nuclear Burning ◽  
Definition Of

Brown dwarfs (hereafter BDs) are formed, like stars, by interstellar cloud collapse, but attaining masses of less then 0.075 M⊙ (Baraffe et al. 1998), i.e. too low core temperatures (< 3.5 × 106 K) to stabilize the nuclear burning of the hydrogen PP chain. Therefore, even the most massive BDs begin cooling after some 109 yrs. However, for masses above 0.06 M⊙, core temperatures become hotter than the lithium burning temperature (2.4 x 106 K). All BDs above 0.013 M⊙ (13 MJup) reach core temperatures above the 1.0 x 106 K necessary to burn deuterium from about 107 yrs. The IAU has adopted the definition of the planetary regime as objects having masses below the deuterium burning conditions. But BDs are likely to form well below this limit into the planetary mass regime down to some 5 MJup. It is therefore convenient, in the absence of indices on their formation mechanisms, to call them planetary mass objects or planemos.

scholarly journals A Wide Planetary-mass Companion to a Young Low-mass Brown Dwarf in Ophiuchus

2020 ◽  
Vol 905 (2) ◽  
pp. L14
Author(s):  
Clémence Fontanive ◽  
Katelyn N. Allers ◽  
Blake Pantoja ◽  
Beth Biller ◽  
Sophie Dubber ◽  
...  
Keyword(s):  
Brown Dwarf ◽  
Planetary Mass ◽  
Low Mass

scholarly journals Spectroscopy across the brown dwarf/planetary mass boundary

2012 ◽  
Vol 540 ◽  
pp. A85 ◽  
Author(s):  
J. Patience ◽  
R. R. King ◽  
R. J. De Rosa ◽  
A. Vigan ◽  
S. Witte ◽  
...  
Keyword(s):  
Brown Dwarf ◽  
Planetary Mass
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