Stellar rotation and variability in the Orion Nebula Cluster

By W. Herbst, Coryn A. L. Bailer-Jones, R. Mundt, K. Meisenheimer, R. Wackermann. 2002

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In Astronomy and Astrophysics

Citations in the corpus

Magnetospheric accretion-ejection processes in the classical T Tauri star AA Tauri (2006, methodology): “The False Alarm Probability (FAP) was computed following the Monte Carlo method described in Herbst et al. (2002).”
THE DISTANCE TO NGC 2264 (2009, background): “In some cases, confounding factors such as aliasing in the light curves or the presence of multiple starspots can increase these errors dramatically (e.g. Herbst et al. 2002).”
Improved angular momentum evolution model for solar-like stars (2013, methodology): “ONC The Orion Nebula Cluster is a very young cluster, with an age of 0.8-2 Myr (Herbst et al. 2002; Hillenbrand 1997) and located at a distance of about 450 pc (Herbst et al. 2002; Hillenbrand 1997).”
THE MASS-DEPENDENCE OF ANGULAR MOMENTUM EVOLUTION IN SUN-LIKE STARS (2014, result): “The left panel of Figure 2 shows this initial distribution, compared with the ∼ 2 Myr-old cluster ONC (data from Stassun et al. 1999; Herbst et al. 2001, 2002; Rodŕıguez-Ledesma et al. 2009).”
Accretion-powered Stellar Winds. II. Numerical Solutions for Stellar Wind Torques (2008, background): “Recent studies have shown a correlation between slow rotation and the presence of an a accretion disk (see especially Cieza & Baliber 2007), though this idea has been controversial in the past (e.g., Stassun et al. 1999; Herbst et al. 2000; Stassun et al. 2001; Herbst et al. 2002).”
Accretion to magnetized stars through the Rayleigh–Taylor instability: global 3D simulations (2008, background): “This of relevance to young stars, whose light curves often lack clear periodicity (e.g. Herbst et al. 2000, 2002).”
The Formation and Early Evolution of Low-Mass Stars and Brown Dwarfs (2012, background): “For stars at ages of a few Myr, the largest studies of rotation periods have been conducted in the ONC and NGC 2264 (τ ∼ 1 and 2Myr, Herbst, Bailer-Jones & Mundt 2001; Herbst et al. 2002; Lamm et al. 2005, 2004; Stassun et al. 1999).”
Lithium depletion and the rotational history of exoplanet host stars (2008, unknown): “…NGC 2547 40 0.35 6.8 15 5 Pleiades 120 0.44 6.1 11 6 M50 130 0.59 8.7 74 7 M34 200 0.89 7.2 22 8 M37 550 3.6 7.3 145 9 Hyades 625 5.4 9.1 15 10 (1) Herbst et al. (2002), (2) Lamm et al. (2005), (3) Makidon et al. (2004), (4) Irwin et al. (2008b), (5) Irwin et al. (2008a), (6) Compilation (see…”
RADIUS-DEPENDENT ANGULAR MOMENTUM EVOLUTION IN LOW-MASS STARS. I (2011, methodology): “Stellar periods are taken from Herbst et al. (2002) (who have compiled data from both their own study and from Herbst et al. 2000 and Stassun et al. 1999).”
Stellar Rotation in Young Clusters: The First 4 Million Years (2004, background): “This initial condition is similar to that assumed by Herbst et al. (2002).”
YSOVAR: THE FIRST SENSITIVE, WIDE-AREA, MID-INFRARED PHOTOMETRIC MONITORING OF THE ORION NEBULA CLUSTER (2011, methodology): “Many other groups subsequently obtained time series photometry of other portions of the ONC, using optical (Stassun et al. 1999; Rebull 2001; Herbst et al. 2002; Irwin et al. 2007) and near-IR (Carpenter et al. 2001) imaging data.”