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dc.contributor.authorRicci, L.
dc.contributor.authorTesti, L.
dc.contributor.authorNatta, A.
dc.contributor.authorScholz, A.
dc.contributor.authorde Gregorio-Monsalvo, I.
dc.contributor.authorIsella, A.
dc.date.accessioned2016-04-13T10:30:04Z
dc.date.available2016-04-13T10:30:04Z
dc.date.issued2014-08-10
dc.identifier145105011
dc.identifier98bfe0f5-84d2-41c2-ab87-8e5e1921bf39
dc.identifier000339657700020
dc.identifier84905270182
dc.identifier.citationRicci , L , Testi , L , Natta , A , Scholz , A , de Gregorio-Monsalvo , I & Isella , A 2014 , ' Brown Dwarf Disks with ALMA ' , Astrophysical Journal , vol. 791 , no. 1 , 20 . https://doi.org/10.1088/0004-637X/791/1/20en
dc.identifier.issn0004-637X
dc.identifier.otherBibCode: 2014ApJ...791...20R
dc.identifier.otherArXiv: http://arxiv.org/abs/1406.0635v1
dc.identifier.urihttps://hdl.handle.net/10023/8607
dc.description15 pages, 10 figures, accepted for publication in ApJen
dc.description.abstractWe present Atacama Large Millimeter/submillimeter Array continuum and spectral line data at 0.89 mm and 3.2 mm for three disks surrounding young brown dwarfs and very low mass stars in the Taurus star forming region. Dust thermal emission is detected and spatially resolved for all the three disks, while CO(J = 3-2) emission is seen in two disks. We analyze the continuum visibilities and constrain the disks' physical structure in dust. The results of our analysis show that the disks are relatively large; the smallest one has an outer radius of about 70 AU. The inferred disk radii, radial profiles of the dust surface density, and disk to central object mass ratios lie within the ranges found for disks around more massive young stars. We derive from our observations the wavelength dependence of the millimeter dust opacity. In all the three disks, data are consistent with the presence of grains with at least millimeter sizes, as also found for disks around young stars, and confirm that the early stages of the solid growth toward planetesimals occur also around very low-mass objects. We discuss the implications of our findings on models of solids evolution in protoplanetary disks, the main mechanisms proposed for the formation of brown dwarfs and very low-mass stars, as well as the potential of finding rocky and giant planets around very low-mass objects.
dc.format.extent2140055
dc.language.isoeng
dc.relation.ispartofAstrophysical Journalen
dc.subjectbrown dwarfsen
dc.subjectcircumstellar matteren
dc.subjectplanets and satellites: formationen
dc.subjectstars: individual: 2M0444+2512 CIDA 1 CFHT Tau 4en
dc.subjectsubmillimeter: starsen
dc.subjectQC Physicsen
dc.subject.lccQCen
dc.titleBrown Dwarf Disks with ALMAen
dc.typeJournal articleen
dc.contributor.institutionUniversity of St Andrews. School of Physics and Astronomyen
dc.identifier.doi10.1088/0004-637X/791/1/20
dc.description.statusPeer revieweden
dc.identifier.urlhttp://adsabs.harvard.edu/abs/2014ApJ...791...20Ren


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