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Cited by 195Astrophysics and Star Formation StudiesStellar, planetary, and galactic studiesAstrophysical Phenomena and Observations

A Spectroscopic Survey of Subarcsecond Binaries in the Taurus‐Auriga Dark Cloud with the Hubble Space Telescope

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Hartigan, Patrick, Kenyon, Scott J.·2003·The Astrophysical Journal
DOI 10.1086/345293
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Abstract

We report the results of a spectroscopic survey of 20 close T Tauri binaries in the Taurus-Auriga dark cloud where the separations between primaries and their secondaries are less than the typical size of a circumstellar disk around a young star. Analysis of low- and medium-resolution Space Telescope Imaging Spectrograph spectra yields the stellar luminosities, reddenings, ages, masses, mass accretion rates, IR excesses, and emission-line luminosities for each star in each pair. We examine the ability of IR color excesses, Hα equivalent widths, [O I] emission, and veiling to distinguish between weak emission and classical T Tauri stars. Four pairs have one classical T Tauri star (CTTS) and one weak-lined T Tauri star (WTTS); the CTTS is the primary in three of these systems. This frequency of mixed pairs among the close T Tauri binaries is similar to the frequency of mixed pairs in wider young binaries. Extinctions within pairs are usually similar; however, the secondary is more heavily reddened than the primary in some systems, where it may be viewed through the primary's disk. Mass accretion rates of primaries and secondaries are strongly correlated, and Hα luminosities, IR excesses, and ages also correlate within pairs. Primaries tend to have somewhat larger accretion rates than their secondaries do and are typically slightly older than their secondaries according to three different sets of modern pre-main-sequence evolutionary tracks. Age differences for XZ Tau and FS Tau, systems embedded in reflection nebulae, are striking: the secondary in each pair is less massive but more luminous than the primary. The stellar masses of the UY Aur and GG Tau binaries measured from their rotating molecular disks are about 30% larger than the masses inferred from the spectra and evolutionary tracks. This discrepancy can be resolved in several ways, among them a 10% closer distance for the Taurus-Auriga dark cloud.

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Authors
Hartigan, P., & Kenyon, S. J.
Affiliations
  • Rice University (US)
  • Kitt Peak National Observatory (US)
ORCID
Hartigan, Patrick
Venue
The Astrophysical Journal
Publisher
American Astronomical Society
Published
2003-01-20
Volume
583
Issue
1
Pages
334-357
ISSN
  • 0004-637X (ISSN-L)
  • 1538-4357
DOI
10.1086/345293
OpenAlex
W2015134861
Semantic Scholar
fa05a85c5be5893203a32beae24de3295ab00319
Cited by
195
References
52
Citations by year
2026: 4 · 2025: 4 · 2024: 6 · 2023: 3 · 2022: 4 · 2021: 7 · 2020: 8 · 2019: 4 · 2018: 5 · 2017: 8 · 2016: 16 · 2015: 6 · 2014: 10 · 2013: 12 · 2012: 9
FWCI
6.95
Type
journal article
Language
en
Open access
Locations
  • The Astrophysical Journal (publishedVersion)
  • arXiv (Cornell University) (submittedVersion)
  • CERN Document Server (European Organization for Nuclear Research) (submittedVersion)
  • arXiv (Cornell University)
Funders
National Aeronautics and Space Administration (NAS 526555)
Topics
  • Physical Sciences › Physics and Astronomy › Astronomy and Astrophysics › Astrophysics and Star Formation Studies
  • Physical Sciences › Physics and Astronomy › Astronomy and Astrophysics › Stellar, planetary, and galactic studies
  • Physical Sciences › Physics and Astronomy › Astronomy and Astrophysics › Astrophysical Phenomena and Observations
Keywords
T Tauri stars, young binary stars, accretion rate, circumstellar disks, infrared excess, H-alpha emission, [O I] emission, stellar ages, stellar mass, pre-main sequence evolution, reflection nebulae

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