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Verfasst von:Joergens, Viki [VerfasserIn]   i
 Bonnefoy, M. [VerfasserIn]   i
 Liu, Y. [VerfasserIn]   i
 Bayo, A. [VerfasserIn]   i
 Wolf, S. [VerfasserIn]   i
 Chauvin, G. [VerfasserIn]   i
 Rojo, P. [VerfasserIn]   i
Titel:OTS 44: disk and accretion at the planetary border
Verf.angabe:V. Joergens, M. Bonnefoy, Y. Liu, A. Bayo, S. Wolf, G. Chauvin, and P. Rojo
E-Jahr:2013
Jahr:25 October 2013
Umfang:5 S.
Teil:volume:558
 year:2013
 month:10
 elocationid:L7
 pages:1-5
 extent:5
Fussnoten:Gesehen am 08.04.2021 ; Letter to the editor
Titel Quelle:Enthalten in: Astronomy and astrophysics
Ort Quelle:Les Ulis : EDP Sciences, 1969
Jahr Quelle:2013
Band/Heft Quelle:558(2013) vom: Okt., Artikel-ID L7, Seite 1-5
ISSN Quelle:1432-0746
Abstract:We discover that the very low-mass brown dwarf OTS 44 (<i>M<i/>9.5, ~12 <i>M<i/><sub>Jup<sub/>) has significant accretion and a substantial disk, which demonstrates that the processes that accompany canonical star formation occur down to a central mass of a few Jupiter masses. We discover in VLT/SINFONI spectra that OTS 44 has strong, broad, and variable Pa <i>β<i/> emission that is evidence for active accretion at the planetary border. We also detect strong H<i>α<i/> emission of OTS 44 in a literature spectrum and determine an H<i>α<i/> EW of −141 Å, which indicates active accretion. Both the Pa <i>β<i/> and H<i>α<i/> emission lines have broad profiles with wings extending to velocities of about ±200 km s<sup>-1<sup/>. We determine the mass accretion rate of OTS 44 based on H<i>α<i/> to 7.6 × 10<sup>-12<sup/> . This result shows that OTS 44 has a relatively high mass-accretion rate considering its small central mass. This mass rate is nevertheless consistent with the general decreasing trend found for stars of several solar masses down to brown dwarfs. Furthermore, we determine the properties of the disk surrounding OTS 44 through radiative transfer modeling of flux measurement from the optical to the far-IR (<i>Herschel<i/>) by applying a Bayesian analysis. We find that OTS 44 has a highly flared disk (<i>β<i/> > 1.2) with a mass of 9.1 , i.e. ~0.1 or 30 <i>M<i/><sub>Earth<sub/>. We show that the ratio of the disk-to-central-mass of about 10<sup>-2<sup/> found for objects between 0.03 and 14 is also valid for OTS 44 at a mass of ~0.01 . Our observations are in line with an isolated star-like mode of the formation of brown dwarfs down to 0.01 .
DOI:doi:10.1051/0004-6361/201322432
URL:Bitte beachten Sie: Dies ist ein Bibliographieeintrag. Ein Volltextzugriff für Mitglieder der Universität besteht hier nur, falls für die entsprechende Zeitschrift/den entsprechenden Sammelband ein Abonnement besteht oder es sich um einen OpenAccess-Titel handelt.

Volltext ; Verlag: https://doi.org/10.1051/0004-6361/201322432
 Volltext: https://www.aanda.org/articles/aa/abs/2013/10/aa22432-13/aa22432-13.html
 DOI: https://doi.org/10.1051/0004-6361/201322432
Datenträger:Online-Ressource
Sprache:eng
K10plus-PPN:1753334721
Verknüpfungen:→ Zeitschrift

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