The evolution of stars in the Taurus-Auriga T association

Abstract

In a recent study, individual parallaxes were determined for many stars of the Taurus-Auriga T association that are members of the same moving group. We use these new parallaxes to re-address the issue of the relationship between classical T Tauri stars (CTTSs) and weak-emission line T Tauri stars (WTTSs). With the available spectroscopic and photometric information for 72 individual stars or stellar systems among the Taurus-Auriga objects with known parallaxes, we derived reliable photospheric luminosities, mainly from the Ic magnitude of these objects. We then studied the mass and age distributions of the stellar sample, using pre-main sequence evolutionary models to determine the basic properties of the stellar sample. Statistical tests and Monte Carlo simulations were then applied to studying the properties of the two T Tauri subclasses. We find that the probability of CTTS and WTTS samples being drawn from the same parental age and mass distributions is low; CTTSs are, on average, younger than WTTSs. They are also less massive, but this is due to selection effects. The observed mass and age distributions of both T Tauri subclasses can be understood in the framework of a simple disk evolution model, assuming that the CTTSs evolve into WTTSs when their disks are fully accreted by the stars. According to this empirical model, the average disk lifetime in Taurus-Auriga is 4 10**6 (Mstar/Msun)**0.75 yr.

accepted by A&A Letters

References in corpus (4)

• Why Do T Tauri Disks Accrete?
• A Survey for New Members of Taurus with the Spitzer Space Telescope
• A kinematic study of the Taurus-Auriga T association
• The stellar mass-accretion rate relation in T Tauri stars and brown dwarfs

Cited by in corpus (26)

• The Mass Budget of Planet Forming Discs: Isolating the Epoch of Planetesimal Formation
• Disk Dispersal and Planet Formation Time Scales
• An ALMA Continuum Survey of Circumstellar Disks in the Upper Scorpius OB Association
• New Constraints From Dust Lines On The Surface Densities Of Protoplanetary Disks
• Constraining the Sub-AU-Scale Distribution of Hydrogen and Carbon Monoxide Gas around Young Stars with the Keck Interferometer
• Multiplicity and clustering in Taurus star-forming region. I. Unexpected ultra-wide pairs of high-order multiplicity in Taurus
• A Tail Structure Associated with Protoplanetary Disk around SU Aurigae
• An assessment of Li abundances in weak-lined and classical T Tauri stars of the Taurus-Auriga association
• A semi-empirical model for magnetic braking of solar-type stars
• Consistent dust and gas models for protoplanetary disks IV. A panchromatic view of protoplanetary disks
• Near-IR High-Resolution Imaging Polarimetry of the SU Aur Disk: Clues for Tidal Tails?
• An upper limit on the mass of the circumplanetary disk for DH Tau b
• A Rotation Rate for the Planetary-Mass Companion DH Tau b
• Photometric determination of the mass accretion rates of pre-main sequence stars. VI. The case of LH 95 in the Large Magellanic Cloud
• The TW Hya Rosetta Stone Project IV: A hydrocarbon rich disk atmosphere
• HST UV Spectroscopy of the Planet-Hosting T Tauri Star PDS 70
• Constraints to the magnetospheric properties of T Tauri stars - II. The Mg II ultraviolet feature
• Residual Gas & Dust Around Transition Objects and Weak T Tauri Stars
• Disk Dissipation Timescale of Pre-main Sequence Stars in Taurus
• Benchmarking the IRDC G351.77-0.53: Gaia DR3 distance, mass distribution, and star formation content
• Imaging the warped dusty disk wind environment of SU Aurigae with MIRC-X
• Spectroscopic Survey of Hα Emission Line Stars Associated with Bright Rimmed Clouds
• Stellar Obliquity Excitation via Disk Dispersal-Driven Resonances in Binaries
• Formation of ring-like structures in flared α-discs with X-ray/FUV photoevaporation
• A CCD Search for Variable Stars in the Open Cluster NGC 6611
• MINDS survey of silicates in T Tauri disks: Correlation between dust and gas