Examinando por Autor "Anglada, G."

Mostrando 1 - 1 de 1

Acceso Abierto
Tidal Interaction between the UX Tauri A/C Disk System Revealed by ALMA
(The Institute of Physics (IOP), 2020-06-19) Zapata, L.; Rodríguez, L. F.; Fernández López, M.; Palau, A.; Estalella, R.; Osorio, M.; Anglada, G.; Huélamo, N.; Consejo Nacional de Ciencia y Tecnología (CONACYT); Universidad Nacional Autónoma de México (UNAM); Agencia Estatal de Investigación (AEI); Zapata, L. [0000-0003-2343-7937]; Rodríguez, L. F. [0000-0003-2737-5681]; Palau, A. [0000-0002-9569-9234]; Fernández López, M. [0000-0001-5811-0454]; Estalella, R. [0000-0001-7341-8641]; Osorio, M. [0000-0002-6737-5267]; Anglada, G. [0000-0002-7506-5429]; Huelamo, N. [0000-0002-2711-8143]; Unidad de Excelencia Científica María de Maeztu Centro de Astrobiología del Instituto Nacional de Técnica Aeroespacial y CSIC, MDM-2017-0737; Centros de Excelencia Severo Ochoa, INSTITUTO DE ASTROFISICA DE ANDALUCIA (IAA), SEV-2017-0709
We present sensitive and high angular-resolution (similar to 02-03) (sub)millimeter (230 and 345 GHz) continuum and CO(2-1)/CO(3-2) line archive observations of the disk star system in UX Tauri carried out with the Atacama Large Millimeter/Submillimeter Array. These observations reveal the gas and dusty disk surrounding the young star UX Tauri A with a large signal-to-noise ratio (>400 in the continuum and >50 in the line), and for the first time we detect the molecular gas emission associated with the disk of UX Tauri C (with a size for the disk of <56 au). No (sub)millimeter continuum emission is detected at the 5 sigma level (0.2 mJy at 0.85 mm) associated with UX Tauri C. For the component UX Tauri C, we estimate a dust disk mass of <= 0.05M(circle plus). Additionally, we report a strong tidal disk interaction between both disks, UX Tauri A/C, separated 360 au in projected distance. The CO line observations reveal marked spiral arms in the disk of UX Tauri A and an extended redshifted stream of gas associated with the UX Tauri C disk. No spiral arms are observed in the dust continuum emission of UX Tauri A. Assuming a Keplerian rotation we estimate the enclosed masses (disk+star) from their radial velocities in 1.4 0.6Mfor UX Tauri A, and 70 30/siniJupiter masses for UX Tauri C (the latter coincides with the mass upper limit value for a brown dwarf). The observational evidence presented here lead us to propose that UX Tauri C has a close approach of a possible wide, evolving, and eccentric orbit around the disk of UX Tauri A, causing the formation of spiral arms and a stream of molecular gas falling toward UX Tauri C.