Disk Evolution in Cep OB2: Results from the Spitzer Space Telescope

By A. Sicilia-Aguilar, L. Hartmann, N. Calvet, S. Megeath, J. Muzerolle, L. Allen, P. D’Alessio, B. Mer'in, J. Stauffer, E. Young and 1 more. 2006

218 citations recorded by the source corpus.

Subfields: Astronomy and Astrophysics

View Paper: https://www.semanticscholar.org/paper/d5ac005e8cbe11db5960d6e6f7e90d913db2ffa5

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In Astronomy and Astrophysics

1. K. Luhman
2. N. Evans II
3. L. Hartmann
4. Eric Mamajek
5. P. Myers
6. L. Hillenbrand
7. S. Andrews
8. N. Calvet

Citations in the corpus

• THE DISK POPULATION OF THE TAURUS STAR-FORMING REGION (2009, methodology): “Tr 37 For Trumpler 37 (Tr 37, τ ∼ 4 Myr, Sicilia-Aguilar et al. 2005), we have adopted the membership list, extinction estimates, and spectral types that were presented by Sicilia-Aguilar et al. (2005), the Spitzer photometry measured by Sicilia-Aguilar et al. (2006), and the Ks data from 2MASS.”
• The Spitzer c2d Survey of Weak-Line T Tauri Stars. II. New Constraints on the Timescale for Planet Building (2007, background): “In fact, Sicilia-Aguilar et al. (2006) define transition disks as objects with 8.0 µm excess but no 4.5 µm excess.”
• Protoplanetary Disks and Their Evolution (2011, background): “%) in regions such as the TW Hydra, σ Ori, and NGC 7160 associations (Hernández et al. 2007, Sicilia-Aguilar et al. 2006).”
• ALMA OBSERVATIONS OF CIRCUMSTELLAR DISKS IN THE UPPER SCORPIUS OB ASSOCIATION (2016, background): “…an exposed stellar photosphere (e.g. Gutermuth et al. 2004; Hartmann et al. 2005; Megeath et al. 2005; Carpenter et al. 2006; Lada et al. 2006; Sicilia-Aguilar et al. 2006; Balog et al. 2007; Barrado y Navascués et al. 2007; Cieza & Baliber 2007; Dahm & Hillenbrand 2007; Hernández et al.…”
• GLOBAL SIMULATIONS OF PROTOPLANETARY DISKS WITH OHMIC RESISTIVITY AND AMBIPOLAR DIFFUSION (2015, background): “For example, PPDs are known to accrete gas onto their host stars at a typical rate of 10−8±1M yr−1 (Gullbring et al. 1998; Hartmann et al. 1998) and have life times in the range∼ 3–10 Myr (Sicilia-Aguilar et al. 2006).”
• A Spitzer View of Protoplanetary Disks in the γ Velorum Cluster (2008, background): “…& Muzerolle 2007), Taurus (Hartmann et al. 2005), NGC 7129 (Gutermuth et al. 2004), Chameleons (Megeath et al. 2005a), Tr 37 and NGC 7160 (Sicilia-Aguilar et al. 2006), IC 348 (Lada et al. 2006), NGC 2244 (Balog et al. 2007), NGC 2264 (Cieza & Baliber 2007), σ Ori (Hernández et al.…”
• WIND-DRIVEN ACCRETION IN PROTOPLANETARY DISKS. I. SUPPRESSION OF THE MAGNETOROTATIONAL INSTABILITY AND LAUNCHING OF THE MAGNETOCENTRIFUGAL WIND (2013, background): “The gas in PPDs are found to be rapidly accreting to the protostar with accretion rate of 10−8±1 M yr−1, with typical disk lifetime of about 1–10 Myr (e.g., Hartmann et al. 1998; Sicilia-Aguilar et al. 2006).”
• WIDE-FIELD INFRARED SURVEY EXPLORER OBSERVATIONS OF THE EVOLUTION OF MASSIVE STAR-FORMING REGIONS (2012, background): “Contreras et al. (2002) derived a distance of 0.9 kpc to the region and the Spitzer study of Sicilia-Aguilar et al. (2006) found an age of 4 Myr for Tr 37.”
• Spitzer Observations of IC 348: The Disk Population at 2-3 Million Years (2005, background): “Thus, in IC 348 the conditions for planet building may be most favorable around stars with masses similar to that of our Sun.”
• Dust Evolution and the Formation of Planetesimals (2016, background): “The Spitzer data generally confirm the previous results on disk lifetimes (Sicilia-Aguilar et al. 2006; Hernández et al. 2007).”
• Interpreting Spectral Energy Distributions from Young Stellar Objects. I. A Grid of 200,000 YSO Model SEDs (2006, background): “…molecular cloud (Megeath et al. 2005a), the Taurus molecular cloud (Hartmann et al. 2005), the LMC (Chu et al. 2005; Meixner et al. 2006) and SMC, and many other well-known star formation regions (e.g Gutermuth et al. 2004; Megeath et al. 2005b; Allen et al. 2006; Sicilia-Aguilar et al. 2006).”
• Demographics of Transition Objects (2007, unknown): “Our classification scheme is broader than that adopted in some recent studies in which only systems with no apparent excess anywhere shortward of a given wavelength are considered to be transition objects (Muzerolle et al. 2006; Sicilia-Aguilar et al. 2006).”
• The Disk Population of the Chamaeleon I Star-forming Region (2008, background): “…et al. 2007), Orion OB1b (Hernández et al. 2006), η Cha (Megeath et al. 2005), Chamaeleon II (Young et al. 2005; Allers et al. 2006; Porras et al. 2007), NGC 2362 (Dahm & Hillenbrand 2007), Upper Sco (Carpenter et al. 2006; Scholz et al. 2007), Tr 37, and NGC 7160 (Sicilia-Aguilar et al. 2006).”
• Star and Protoplanetary Disk Properties in Orion's Suburbs (2009, background): “Since the infrared spectral slopes trace M. Fang et al.: Star and protoplanetary disk properties in Oron’s suburbs 13 the disk geometry, our observations provide evidence for a crelation between disk geometry evolution and accretion evolution (see also e.g. Sicilia-Aguilar et al. 2006b).”
• THE DISK POPULATION OF THE UPPER SCORPIUS ASSOCIATION (2012, background): “Although Spitzer has focused on relatively compact clusters (∼ 1 deg2, Lada et al. 2006; Sicilia-Aguilar et al. 2006; Dahm & Hillenbrand 2007; Hernández et al. 2007; Luhman et al. 2008; Gutermuth et al. 2009), it has also imaged more widely distributed populations in areas as large as∼ 50 deg2…”
• Theory of Star Formation (2007, background): “%) for Solar-type stars than in those of higher or lower mass. Observations of other clusters are consistent with these results (Sicilia-Aguilar et al., 2006a).”
• GIANT PLANET MIGRATION, DISK EVOLUTION, AND THE ORIGIN OF TRANSITIONAL DISKS (2009, background): “We do not reproduce the long tail of the distribution observed in some older clusters (e.g., Lawson et al. 2004; Sicilia-Aguilar et al. 2006), but realistic dispersion in some of the parameters held constant in our models (α, Φ, H/R), or dispersion in the ages of stars in individual star-forming…”
• A Spitzer Space Telescope Study of Disks in the Young σ Orionis Cluster (2007, background): “Prior to the complete or nearly complete clearing seen in transition disks, onewould expect to observe optically thick but reduced infrared emission from the inner disk, for which there is some evidence (e.g., Sicilia-Aguilar et al. 2006; Lada et al. 2006).”
• Spitzer Observations of the Orion OB1 Association: Disk Census in the Low-Mass Stars (2007, background): “This suggests a more rapid decrease in dust emission in the inner disk, in agreement with results from Sicilia-Aguilar et al. (2006) in the Cepheus OB2 association.”