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dc.contributor.authorRicci, L.
dc.contributor.authorRome, H.
dc.contributor.authorPinilla, P.
dc.contributor.authorFacchini, Stefano
dc.contributor.authorBirnstiel, T.
dc.contributor.authorTesti, L.
dc.date.accessioned2017-10-02T23:10:37Z
dc.date.available2017-10-02T23:10:37Z
dc.date.issued2017-08-25
dc.identifier.citationVLA Observations of the Disk around the Young Brown Dwarf 2MASS J044427+2512 2017, 846 (1):19 The Astrophysical Journalen
dc.identifier.issn1538-4357
dc.identifier.doi10.3847/1538-4357/aa81bf
dc.identifier.urihttp://hdl.handle.net/10150/625755
dc.description.abstractWe present multi-wavelength radio observations obtained with the VLA of the protoplanetary disk surrounding the young brown dwarf 2MASS J04442713+2512164 (2M0444) in the Taurus star-forming region. 2M0444 is the brightest known brown dwarf disk at millimeter wavelengths, making this an ideal target to probe radio emission from a young brown dwarf. Thermal emission from dust in the disk is detected at 6.8 and 9.1 mm, whereas the 1.36 cm measured flux is dominated by ionized gas emission. We combine these data with previous observations at shorter sub-mm and mm wavelengths to test the predictions of dust evolution models in gas-rich disks after adapting their parameters to the case of 2M0444. These models show that the radial drift mechanism affecting solids in a gaseous environment has to be either completely made inefficient, or significantly slowed down by very strong gas pressure bumps in order to explain the presence of mm/cm-sized grains in the outer regions of the 2M0444 disk. We also discuss the possible mechanisms for the origin of the ionized gas emission detected at 1.36 cm. The inferred radio luminosity for this emission is in line with the relation between radio and bolometric luminosity valid for for more massive and luminous young stellar objects, and extrapolated down to the very low luminosity of the 2M0444 brown dwarf.
dc.description.sponsorshipEuropean Research Council (ERC) under the European Union's Horizon research and innovation programme [714769]en
dc.language.isoenen
dc.publisherIOP PUBLISHING LTDen
dc.relation.urlhttp://stacks.iop.org/0004-637X/846/i=1/a=19?key=crossref.4276cf8d882c700ef4c062936739350fen
dc.rights© 2017. The American Astronomical Society. All rights reserved.en
dc.subjectbrown dwarfsen
dc.subjectcircumstellar matteren
dc.subjectplanets and satellites: formationen
dc.subjectprotoplanetary disksen
dc.subjectstars: individual (2M0444)en
dc.titleVLA Observations of the Disk around the Young Brown Dwarf 2MASS J044427+2512en
dc.typeArticleen
dc.contributor.departmentUniv Arizona, Dept Astron, Steward Observen
dc.identifier.journalThe Astrophysical Journalen
dc.description.collectioninformationThis item from the UA Faculty Publications collection is made available by the University of Arizona with support from the University of Arizona Libraries. If you have questions, please contact us at repository@u.library.arizona.edu.en
dc.eprint.versionFinal published versionen
refterms.dateFOA2018-06-12T04:10:29Z
html.description.abstractWe present multi-wavelength radio observations obtained with the VLA of the protoplanetary disk surrounding the young brown dwarf 2MASS J04442713+2512164 (2M0444) in the Taurus star-forming region. 2M0444 is the brightest known brown dwarf disk at millimeter wavelengths, making this an ideal target to probe radio emission from a young brown dwarf. Thermal emission from dust in the disk is detected at 6.8 and 9.1 mm, whereas the 1.36 cm measured flux is dominated by ionized gas emission. We combine these data with previous observations at shorter sub-mm and mm wavelengths to test the predictions of dust evolution models in gas-rich disks after adapting their parameters to the case of 2M0444. These models show that the radial drift mechanism affecting solids in a gaseous environment has to be either completely made inefficient, or significantly slowed down by very strong gas pressure bumps in order to explain the presence of mm/cm-sized grains in the outer regions of the 2M0444 disk. We also discuss the possible mechanisms for the origin of the ionized gas emission detected at 1.36 cm. The inferred radio luminosity for this emission is in line with the relation between radio and bolometric luminosity valid for for more massive and luminous young stellar objects, and extrapolated down to the very low luminosity of the 2M0444 brown dwarf.


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