Exploring the formation and evolution of planetary systems : proceedings of the 299th symposium of the International Astronomical Union, held in Victoria, Canada, June 2-7, 2013

By M. Booth, B. Matthews, J. Graham. 2013

216 citations recorded by the source corpus.

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Citations in the corpus

HAZMAT. I. THE EVOLUTION OF FAR-UV AND NEAR-UV EMISSION FROM EARLY M STARS (2014, background): “…both ground- and space-based instruments including TESS, CARMENES, SPIROU, and NGTS (Ricker et al. 2014; Quirrenbach et al. 2012; Delfosse et al. 2013; Wheatley et al. 2014, respectively), for which the incident stellar highenergy spectrum will be critical to understanding the planets’ atmospheres.”
Discovery of a warm, dusty giant planet around HIP 65426 (2017, methodology): “They are the Exo-REM models (Baudino et al. 2015), the 2014 version of the PHOENIX BT-Settl atmospheric models described in Allard (2014) and Baraffe et al. (2015) and the thick AE cloud parametric models of Madhusudhan et al. (2011).”
The GALAH survey: observational overview and Gaia DR1 companion (2016, background): “We anticipate that the ongoing development of model atmospheres for cool stars (e.g., Allard 2014) will allow us to analyse those targets in the future.”
AN EMPIRICAL CALIBRATION TO ESTIMATE COOL DWARF FUNDAMENTAL PARAMETERS FROM H-BAND SPECTRA (2014, methodology): “We measured the same spectral features in BT-Settl model spectra (Allard 2014, available online4) as we do in our observed spectra.”
MAKE SUPER-EARTHS, NOT JUPITERS: ACCRETING NEBULAR GAS ONTO SOLID CORES AT 0.1 AU AND BEYOND (2014, background): “In 2D hydrodynamic simulations, Ormel & Shi (2014) and Ormel et al. (2014) vouch for the relevance of RB (when RB RH) to within factors of order unity.”
Compact Disks in a High-resolution ALMA Survey of Dust Structures in the Taurus Molecular Cloud (2019, methodology): “We use the BT-Settl models (version cifist2011 2015; Allard 2014) with solar metallicity and log g = 4.0 to identify regions at < 4300 Å and 5150-5200 Å that are most sensitive to temperature for FG spectral types.”
The Gemini Planet Imager Exoplanet Survey: Giant Planet and Brown Dwarf Demographics from 10 to 100 au (2019, methodology): “We utilize the CIFIST2011 BT-Settl atmosphere models (Caffau et al. 2011; Allard 2014; Baraffe et al. 2015)45, tied to the COND “hot-start” evolutionary model grid (Baraffe et al. 2003), to give absolute H magnitude and temperature as a function of mass and age.”