The TW Hydrae Association: Discovery of T Tauri Star Members Near HR 4796

By B. Zuckerman, R. A. Webb, M. Schwartz, E. Becklin. 2001

264 citations recorded by the source corpus.

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In Astronomy and Astrophysics

Citations in the corpus

A catalogue of young runaway Hipparcos stars within 3 kpc from the Sun (2010, background): “…(1997) (for individual stars see also König 2003; Cutispoto et al. 2002; Neuhäuser et al. 2002; Song et al. 2002; Lawson et al. 2001; Montes et al. 2001; Zuckerman et al. 2001; De Medeiros et al. 2000; Gaidos et al. 2000; Strassmeier et al. 2000; Teixeira et al. 2000; Torres et al. 2000;…”
New Members of the TW Hydrae Association, β Pictoris Moving Group, and Tucana/Horologium Association (2003, methodology): “…(TWA;Kastner et al. 1997; de la Reza et al. 1989;Webb et al. 1999; Zuckerman et al. 2001c), Pic moving group (Barrado y Navascués et al. 1999; Zuckerman et al. 2001a), and Tucana/Horologium association (Tucana/HorA; Zuckerman & Webb 2000; Torres et al. 2000; Zuckerman, Song, & Webb 2001b)…”
Brown Dwarfs and the TW Hydrae Association (2002, background): “1) was chosen to encompass the TWA members listed by Webb et al. (1999), Sterzik et al. (1999), and Zuckerman et al. (2001).”
Evidence for Accretion: High-Resolution X-Ray Spectroscopy of the Classical T Tauri Star TW Hydrae (2001, background): “The TW Hydrae Association (TWA; Kastner et al. 1997, Webb et al. 1999, Zuckerman et al. 2001) holds great potential for spectral studies of X-ray emission from TTS. Due to the proximity of the association (D ∼ 50 pc) and the lack of intervening, ambient cloud material, the X-ray flux of a typical…”
AN OPTICAL SPECTROSCOPIC STUDY OF T TAURI STARS. I. PHOTOSPHERIC PROPERTIES (2014, methodology): “The binary systems TWA 3Aab, TWA 5Aab, TWA 16AB, TWA 23 AB, and TWA 32AB are roughly equal mass (Muzerolle et al. 2000; Zuckerman et al. 2001; Shkolnik et al. 2011; Weinberger et al. 2013), so the luminosities used for this analysis are divided by 2.”
HAZMAT. I. THE EVOLUTION OF FAR-UV AND NEAR-UV EMISSION FROM EARLY M STARS (2014, unknown): “…Torres et al. (2006), 7: Webb et al. (1999), 8: Shkolnik et al. (2011), 9: Song et al. (2003), 10: Reid (2003), 11: Jayawardhana et al. (2006), 12: Zuckerman et al. (2001), 13: Looper et al. (2010), 14: Shkolnik et al. (2012), 15: Kraus et al. (2014), 16: Montes et al. (2001), 17: Zuckerman et…”
BANYAN. II. VERY LOW MASS AND SUBSTELLAR CANDIDATE MEMBERS TO NEARBY, YOUNG KINEMATIC GROUPS WITH PREVIOUSLY KNOWN SIGNS OF YOUTH (2013, background): “The main ones that are well-defined and younger than 120 Myr include TW Hydrae (TWA; 8 - 12 Myr; Zuckerman & Song 2004), β Pictoris (βPMG; 12 - 22 Myr; Zuckerman et al. 2001a), Tucana-Horologium (THA; 20 - 40 Myr; Torres et al. 2000, Zuckerman 2001), Carina (CAR; 20 - 40 Myr; Torres et al. 2008),…”
THE TUCANA/HOROLOGIUM, COLUMBA, AB DORADUS, AND ARGUS ASSOCIATIONS: NEW MEMBERS AND DUSTY DEBRIS DISKS (2011, methodology): “As in our previous papers on these and other young, nearby, moving groups (e.g., Song et al 2003, Zuckerman et al 2004, Zuckerman et al 2001a and 2001b), we rely on a combination of techniques – including Galactic space motions UVW, location on color-magnitude diagrams, lithium abundance, and X-ray…”
BAYESIAN ANALYSIS TO IDENTIFY NEW STAR CANDIDATES IN NEARBY YOUNG STELLAR KINEMATIC GROUPS (2012, methodology): “— (k) Torres et al. 2006; (l) magnitude without binary correction; Torres et al. 2006; (m) ; (n) van Leeuwen 2007; (o) thiswork; (p) Zuckerman et al. 2001c; (q) Reid et al. 2003; (r) Reid & Cruz 2002; (s) Koen et al. 2010; (t) Casagrande et al. 2008; (u) Reid et al. 2004; (v) SDSS-DR8;…”
THE GEMINI/NICI PLANET-FINDING CAMPAIGN: THE FREQUENCY OF PLANETS AROUND YOUNG MOVING GROUP STARS (2013, background): “Zuckerman et al. (2001a) cemented the existence of the β Pic moving group with the confirmation of 18 additional members on the basis of their Galactic space motions.”
Young Stars Near the Sun (2004, methodology): “Zuckerman et al. (2001a) considered ∼22, 000 stars whose Galactic space motion UVW could be calculated from data available in the literature, a procedure often employed by Eggen.”
An Empirical Criterion to Classify T Tauri Stars and Substellar Analogs Using Low-Resolution Optical Spectroscopy (2003, unknown): “These results are depicted in Figure 4, which includes the Orion population (from Herbig & Bell 1988; Alcalá et al. 1996, 1998, 2000), Taurus (Briceño et al. 1993, 1998, 1999, 2002; Alencar & Basri 2001; Mart́ın et al. 2001a; Luhman et al. 2003a; White & Basri 2003; Muzerolle et al. 2003) IC348 (H”