Star and Protoplanetary Disk Properties in Orion's Suburbs

By M. Fang, R. van Boekel, Wei Wang, A. Carmona, A. Sicilia-Aguilar, Th. Henning. 2009

209 citations recorded by the source corpus.

Context. Knowledge of the evolution of circumstellar accretion disks is pivotal to our understanding of star and planet formation; and yet despite intensive theoretical and observational studies, the disk dissipation process is not well understood. Infrared observations of large numbers of young stars, as performed by the Spitzer Space Telescope, may advance our knowledge of this inherently complex process. While infrared data reveal the evolutionary status of the disk, they hold little information on the properties of the central star and the accretion characteristics.

Subfields: Astronomy and Astrophysics

View Paper: https://www.semanticscholar.org/paper/132f5e7b3cfc1f586a18a02615ca7d4819762a1e

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Citations in the corpus

Dust Evolution and the Formation of Planetesimals (2016, background): “They were thought to be in the act of clearing the disk from the inside out, therefore called transition disks (Marsh & Mahoney 1993; Fang et al. 2009; Cieza et al. 2010; Muzerolle et al. 2010; Cieza et al. 2012; Fang et al. 2013; Espaillat et al. 2014).”
RESOLVED IMAGES OF LARGE CAVITIES IN PROTOPLANETARY TRANSITION DISKS (2011, background): “Instead, the transition disks (in our adopted meaning) are typically identified with a set of specialized infrared color criteria (Cieza et al. 2007, 2010; Fang et al. 2009; Muzerolle et al. 2010; Meŕın et al. 2010).”
Protoplanetary Disks and Their Evolution (2011, background): “…star-forming regions, there is a remarkable similarity in the average disk properties from region to region as demonstrated from mid-infrared colors (Fang et al. 2009) and spectra (Furlan et al. 2009) and also in their mass distributions and sub-millimeter colors (Andrews & Williams 2005, 2007a).”
Extrasolar planet population synthesis - IV. Correlations with disk metallicity, mass, and lifetime (2012, unknown): “This was made possible to a large measure thanks to new observational facilities like Spitzer (e.g. Fang et al. 2009).”
X-Shooter study of accretion in Chamaeleon I (2015, methodology): “…converting this Article published by EDP Sciences A136, page 1 of 18 into Lacc through calibrated Lacc–Lline relations (e.g., Muzerolle et al. 1998; Fang et al. 2009) can be efficiently used on spectra covering a relatively narrow wavelength range, such as those offered by multi-object…”
A STEEPER THAN LINEAR DISK MASS–STELLAR MASS SCALING RELATION (2016, background): “…was corroborated by the observation that stellar accretion rates (Ṁ ), tracing the gas disk component, display a steeper dependence with stellar mass when the population of lowmass stars is well sampled (e.g., Natta et al. 2006; Fang et al. 2009; Rigliaco et al. 2011; Alcalá et al. 2014).”
ACCRETION RATES FOR T TAURI STARS USING NEARLY SIMULTANEOUS ULTRAVIOLET AND OPTICAL SPECTRA (2013, background): “Hβ is less often used to trace accretion than Hα but has been shown to correlate with Ṁ (Muzerolle et al. 2001; Herczeg & Hillenbrand 2008; Fang et al. 2009).”
Accretion onto Pre-Main-Sequence Stars (2016, methodology): “…diamonds from Sicilia-Aguilar et al. 2010, Rigliaco et al. 2011, Venuti et al. 2014; cyan diamonds from the Orion Nebula Cluster sample of Manara et al. 2012; diamonds not shown in panel b); and from emission lines ( green squares from Fang et al. 2009, Antoniucci et al. 2014, Manara et al. 2015).”