Disk Accretion at 10 Myr: Results from the TW Hydrae Association

Simple item page
dc.creatorMuzerolle, James
dc.creatorHillenbrand, Lynne
dc.creatorCalvet, Nuria
dc.creatorHartmann, Lee
dc.creatorBriceno, Cesar
dc.date2001-06-29
dc.date.accessioned2026-07-07T01:59:08Z
dc.date.available2026-07-07T01:59:08Z
dc.descriptionWe present an analysis of the accretion properties of the members of the TW Hydrae association. The Halpha emission line profile provides explicit evidence of an active accretion flow in 3 out of 23 observed members of the association; we use radiative transfer models to derive approximate accretion rates for these 3 objects. The resulting accretion rates for these 10 Myr-old stars (<10^-9 Msun/yr) are well over an order of magnitude lower than typical values in 1 Myr-old T Tauri stars. The small fraction of TW Hydrae association objects still accreting (13%, compared with ~70% in 1 Myr-old regions like Taurus), along with the very small accretion rates, points to significant disk evolution over 10 Myr, providing an important constraint on the timescales for planet formation.
dc.description5 pages, 1 inline ps figure. To appear in "Young Stars Near Earth: Progress and Prospects", ASP conference series, R. Jayawardhana and T. Greene, eds. uses PASP style file "newpasp.sty" (included)
dc.identifierhttps://arxiv.org/abs/astro-ph/0106572
dc.identifierhttp://arxiv.org/abs/astro-ph/0106572
dc.identifier.urihttp://salesiana.dossiersoluciones.com/handle/123456789/2991
dc.subjectAstrophysics
dc.titleDisk Accretion at 10 Myr: Results from the TW Hydrae Association
dc.typetext

Files

Collections

arXiv