Magnetospheric accretion and pre-main-sequence stellar masses

Ian Alexander Bonnell, Kester W Smith, Michael R Meyer, Christopher A Tout, Daniel FM Folha, James P Emerson

Research output: Contribution to journalArticlepeer-review

7 Citations (Scopus)

Abstract

We present a method of determining lower limits on the masses of pre-main-sequence (PMS) stars and so constraining the PMS evolutionary tracks. This method uses the redshifted absorption feature observed in some emission-line profiles of T Tauri stars, indicative of infall, The maximum velocity of the accreting material measures the potential energy at the stellar surface, which, combined with an observational determination of the stellar radius, yields the stellar mass. This estimate is a lower limit owing to uncertainties in the geometry and projection effects. Using available data, we show that the computed lower limits can be larger than the masses derived from PMS evolutionary tracks for M less than or similar to 0.5 M-.. Our analysis also supports the notion that accretion streams do not impact near the stellar poles but probably hit the stellar surface at moderate latitudes.

Original languageEnglish
Pages (from-to)pp.1013-1018.
Number of pages6
JournalMonthly Notices of the Royal Astronomical Society
Volume299
Issue number4
Publication statusPublished - 1 Oct 1998

Keywords

  • accretion, accretion discs
  • stars : formation
  • stars : luminosity function, mass function
  • stars : pre-main-sequence
  • T-TAURI STARS
  • DISK ACCRETION
  • BINARY STARS
  • YOUNG STARS
  • BROWN DWARF
  • EVOLUTION
  • DISCOVERY
  • COYOTES
  • CLUSTER
  • SPOT

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