THE SPITZER INFRARED SPECTROGRAPH SURVEY OF T TAURI STARS IN TAURUS

By E. Furlan, K. Luhman, Catherine C. Espaillat, P. D’Alessio, L. Adame, P. Manoj, K. H. Kim, D. Watson, W. Forrest, M. McClure and 4 more. 2011

142 citations recorded by the source corpus.

Subfields: Astronomy and Astrophysics, Spectroscopy

View Paper: https://www.semanticscholar.org/paper/b913869e1d283eca3f0235f0379ab37abccb1e3d

How researchers see this paper

The researchers whose trusted networks rank it highest, strongest advocate first. Every researcher gets a different order.

In Astronomy and Astrophysics

1. K. Luhman
2. G. Herczeg
3. L. Hillenbrand
4. J. Owen
5. C. Clarke
6. N. Calvet
7. Barbara Ercolano
8. Catherine C. Espaillat

In Spectroscopy

1. K. Luhman
2. C. Clarke
3. J. Owen
4. G. Herczeg
5. Barbara Ercolano
6. N. Calvet
7. L. Hillenbrand
8. Catherine C. Espaillat

Citations in the corpus

• The Formation and Early Evolution of Low-Mass Stars and Brown Dwarfs (2012, background): “The silicate feature is weaker at later spectral types (Furlan et al. 2011, Kessler-Silacci et al. 2007, Morrow et al. 2008, Scholz et al. 2007), indicating that grain growth may occur faster in disks around brown dwarfs than in disks around stars.”
• On the theory of disc photoevaporation (2011, background): “The frequency of these ‘transition/pretransition’ discs compared to those of primordial discs suggests that approximately 10–20 per cent of discs are in this stage (Strom et al. 1989; Skrutskie et al. 1990; Luhman et al. 2010; Ercolano et al. 2011a; Furlan et al. 2011).”
• RESOLVING THE LUMINOSITY PROBLEM IN LOW-MASS STAR FORMATION (2011, result): “While this is consistent with the upper range of the observed fraction of Class II sources with transition disk SEDs (3% – 12%; Meŕın et al. 2010; Furlan et al. 2011), the models clearly overpredict this fraction, as described above.”
• THE MASS DEPENDENCE BETWEEN PROTOPLANETARY DISKS AND THEIR STELLAR HOSTS (2013, unknown): “…classifications were collated from the following references: 1 = Luhman et al. (2010), 2 = Hartigan & Kenyon (2003), 3 = Hernández et al. (2004), 4 = Furlan et al. (2011), 5 = White & Ghez (2001), 6 = Itoh et al. (2005), 7 = Espaillat et al. (2010), 8 = Duchêne et al. (1999), 9 = Kraus &…”
• ACCRETION RATES FOR T TAURI STARS USING NEARLY SIMULTANEOUS ULTRAVIOLET AND OPTICAL SPECTRA (2013, methodology): “For consistency, we use the AV estimates from Furlan et al. (2009, 2011) when correcting Taurus and Chameleon I sources for extinction.”
• AN OPTICAL SPECTROSCOPIC STUDY OF T TAURI STARS. I. PHOTOSPHERIC PROPERTIES (2014, methodology): “However, subsequent near-IR analyses have revised extinctions upward (e.g. White & Ghez 2001; Fischer et al. 2011; Furlan et al. 2011).”