High-resolution spectroscopy in TR 37: Gas accretion evolution in evolved dusty disks

Aurora Sicilia-Aguilar*, Lee W. Hartmann, Furesz Gabor, Thomas Henning, Cornelis Dullemond, Wolfgang Brandner

*Corresponding author for this work

Research output: Contribution to journalArticlepeer-review

105 Citations (Scopus)

Abstract

Using the Hectochelle multifiber spectrograph, we have obtained high-resolution (R similar to 34,000) spectra in the H alpha region for a large number of stars in the 4 Myr old cluster Tr 37, containing 146 previously known members and 26 newly identified ones. We present the H alpha line profiles of all members, compare them to our IR observations of dusty disks (Two Micron All Sky Survey JHK + IRAC + MIPS 24 mu m), use the radial velocities as a membership criterion, and calculate the rotational velocities. We find a good correlation between the accretion-broadened profiles and the presence of protoplanetary disks, noting that a small fraction of the accreting stars presents broad profiles with H alpha equivalent widths smaller than the canonical limit separating classical T Tauri stars (CTTSs) and weak-lined T Tauri stars (WTTSs). The number of strong accretors appears to be lower than in younger regions, and a large number of CTTSs have very small accretion rates (M

Original languageEnglish
Pages (from-to)2135-2155
Number of pages21
JournalAstronomical Journal
Volume132
Issue number5
Publication statusPublished - Nov 2006

Keywords

  • accretion, accretion disks
  • line : profiles
  • planetary systems : protoplanetary disks
  • stars : pre-main-sequence
  • stars : rotation
  • T-TAURI STARS
  • MAIN-SEQUENCE STARS
  • ORION-NEBULA CLUSTER
  • EMISSION-LINE DIAGNOSTICS
  • INTERMEDIATE-MASS STARS
  • CIRCUMSTELLAR DISKS
  • MAGNETOSPHERIC ACCRETION
  • PROTOPLANETARY DISK
  • ROTATION PERIODS
  • BROWN DWARFS

Fingerprint

Dive into the research topics of 'High-resolution spectroscopy in TR 37: Gas accretion evolution in evolved dusty disks'. Together they form a unique fingerprint.

Cite this