Growth of Grains in Brown Dwarf Disks

Meru, Farzana; Galvagni, Marina; Olczak, C.

doi:10.1088/2041-8205/774/1/l4

Cited by 38 publications

(17 citation statements)

References 17 publications

Supporting

Mentioning

Contrasting

Order By: Relevance

“…In many ways, these disks are similar to those found around young stellar objects (e.g., T Tauri stars), although BD disks are usually smaller (Hendler et al 2017). In both cases, the disks are typically flat (Scholz et al 2007), show signs of grain growth in their inner regions Apai et al 2005;Meru et al 2013;Pinilla et al 2013), and some show evidence of inner disk clearing (Muzerolle et al 2006). The disk fractions exhibited by stars are similar to the disk fractions observed for BDs, which may indicate a similar formation mechanism for the two populations (Luhman et al 2005).…”

Section: Introductionmentioning

confidence: 54%

Modeling the Protoplanetary Disks of Two Brown Dwarfs in the Taurus Molecular Cloud

Rilinger

Espaillat

Macías

2019

ApJ

View full text Add to dashboard Cite

Measuring the properties of protoplanetary disks around brown dwarfs is central to understanding the formation of brown dwarfs and their planetary companions. We present modeling of CFHT Tau 4 and 2M0444, two brown dwarfs with protoplanetary disks in the Taurus Molecular Cloud. By combining modeling of the spectral energy distributions and ALMA images, we obtain disk radii and masses for these objects; these parameters can be used to constrain brown dwarf formation and planet formation, respectively. We find that the disk around CFHT Tau 4 has a total mass of 0.42 M Jup and a radius of 80 au; we find 2M0444's disk to have a mass of 2.05 M Jup and a radius of 100 au. These radii are more consistent with those predicted by theoretical simulations of brown dwarf formation via undisturbed condensation from a mass reservoir than those predicted by ejection from the formation region. Furthermore, the disk mass of 2M0444 suggests that planet formation may be possible in this disk, although the disk of CFHT Tau 4 is likely not massive enough to form planets. The disk properties measured here provide constraints to theoretical models of brown dwarf formation and the formation of their planetary companions.

show abstract

Section: Introductionmentioning

confidence: 54%

Modeling the Protoplanetary Disks of Two Brown Dwarfs in the Taurus Molecular Cloud

Rilinger

Espaillat

Macías

2019

ApJ

View full text Add to dashboard Cite

show abstract

“…The study and characterization of brown dwarf disks is particularly relevant forinvestigatingthe potential of finding exoplanets around more evolved brown dwarfs (Payne & Lodato 2007;Ricci et al 2014), as well as fortesting theories of disk evolution and planet formation under physical conditions thatcan be very different from the conditionsprobed in disks surrounding young stars (Meru et al 2013;Pinilla et al 2013).…”

Section: Introductionmentioning

confidence: 99%

ALMA Observations of the Young Substellar Binary System 2M1207

Ricci

Cazzoletti

Czekala

et al. 2017

View full text Add to dashboard Cite

We present ALMA observations of the 2M1207 system, a young binary made of a brown dwarf with a planetarymass companion at a projected separation of about 40 au. We detect emission from dust continuum at 0.89 mm and from the J 3 2 = -rotational transition of CO from a very compact disk around the young brown dwarf. The small radius found for this brown dwarf disk may be due to truncation from the tidal interaction with the planetarymass companion. Under the assumption of optically thin dust emission, we estimatea dust mass of 0.1 M ⊕ for the 2M1207A diskand a 3σ upper limit of ∼1 M Moon for dust surrounding 2M1207b, which is the tightest upper limit obtained so far for the mass of dust particles surrounding a young planetary-mass companion. We discuss the impact of this and other non-detections of young planetary-mass companions for models of planet formation thatpredictcircumplanetary material tosurroundthese objects.

show abstract

“…Observations confirm that brown dwarfs possess the same protoplanetary disc fraction as T Tauri stars do (Scholz et al 2008). In addition Ricci et al (2012Ricci et al ( , 2013 found evidence of dust growth, which has also been theoretically explored (Meru, Galvagni & Olczak 2013). Planet formation is thus expected to occur within these discs (Payne & Lodato 2007).…”

Section: Forewordsmentioning

confidence: 71%

First limits on the occurrence rate of short-period planets orbiting brown dwarfs

Triaud

Gillon

2016

Mon. Not. R. Astron. Soc.

View full text Add to dashboard Cite

Planet formation theories predict a large but still undetected population of short-period terrestrial planets orbiting brown dwarfs. Should specimens of this population be discovered transiting relatively bright and nearby brown dwarfs, the Jupiter-size and the low luminosity of their hosts would make them exquisite targets for detailed atmospheric characterisation with JWST and future ground-based facilities. The eventual discovery and detailed study of a significant sample of transiting terrestrial planets orbiting nearby brown dwarfs could prove to be useful not only for comparative exoplanetology but also for astrobiology, by bringing us key information on the physical requirements and timescale for the emergence of life.In this context, we present a search for transit-signals in archival time-series photometry acquired by the Spitzer Space Telescope for a sample of 44 nearby brown dwarfs. While these 44 targets were not particularly selected for their brightness, the high precision of their Spitzer light curves allows us to reach sensitivities below Earth-sized planets for 75% of the sample and down to Europa-sized planets on the brighter targets. We could not identify any unambiguous planetary signal. Instead, we could compute the first limits on the presence of planets on close-in orbits. We find that within a 1.28 day orbit, the occurrence rate of planets with a radius between 0.75 and 3.25 R ⊕ is η < 67 ± 1%. For planets with radii between 0.75 and 1.25 R ⊕ , we place a 95% confident upper limit of η < 87±3%. If we assume an occurrence rate of η = 27% for these planets with radii between 0.75 and 1.25 R ⊕ , as the discoveries of the Kepler-42b and TRAPPIST-1b systems would suggest, we estimate that 175 brown dwarfs need to be monitored in order to guarantee (95%) at least one detection.

show abstract

Growth of Grains in Brown Dwarf Disks

Cited by 38 publications

References 17 publications

Modeling the Protoplanetary Disks of Two Brown Dwarfs in the Taurus Molecular Cloud

Modeling the Protoplanetary Disks of Two Brown Dwarfs in the Taurus Molecular Cloud

ALMA Observations of the Young Substellar Binary System 2M1207

First limits on the occurrence rate of short-period planets orbiting brown dwarfs

Contact Info

Product

Resources

About