Investigation of the Physical Properties of Protoplanetary Disks around T Tauri Stars by a 1 Arcsecond Imaging Survey: Evolution and Diversity of the Disks in Their Accretion Stage

By Y. Kitamura, M. Momose, S. Yokogawa, R. Kawabe, Motohide Tamura, Shigeru Ida. 2002

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Dust properties of protoplanetary disks in the Taurus-Auriga star forming region from millimeter wavelengths (2009, methodology): “However, all available high angular resolution observations performed so far suggest that p ≤ 1.5 (e.g. Dutrey et al. 1996, Wilner et al. 2000, Kitamura et al. 2002, Testi et al. 2003, Andrews & Williams 2007, Isella et al. 2009, Andrews et al. 2009).”
Protoplanetary Disks and Their Evolution (2011, background): “Further, the fraction of disks with at least a MMSN, 10MJup, within 60AU is similar, ∼ 11 − 13%, in Taurus, Ophiuchus, and Orion and, incidentally, comparable to the detection rate of Jupiter mass extrasolar planets (Mann & Williams 2009b).”
H2O and OH Gas in the Terrestrial Planet-forming Zones of Protoplanetary Disks (2008, methodology): “M⋆ and i were fixed to values taken from the literature (Clarke & Bouvier 2000; Kitamura et al. 2002; Eisner et al. 2005; Andrews & Williams 2007).”
MILLIMETER-WAVE POLARIZATION OF PROTOPLANETARY DISKS DUE TO DUST SCATTERING (2015, background): “Opt., 23, 1206 Weingartner, J. C., & Draine, B. T. 2001, ApJ, 548, 296 Wilner, D. J., Ho, P. T. P., Kastner, J. H., & Rodŕıguez, L. F. 2000, ApJ, 534, L101 APPENDIX SCATTERING MATRIX The scattering properties of dust grains are described by the scattering matrix Zij .”
FIRST RESULTS FROM HIGH ANGULAR RESOLUTION ALMA OBSERVATIO NS TOWARD THE HL TAU REGION (2015, background): “…at these wavelengths (Andrews & Williams 2005); hence HL Tau has been a favored interferometric target over the last two decades (Sargent & Beckwith 1991; Mundy et al. 1996; Lay et al. 1997; Kitamura et al. 2002; Looney et al. 2000; Guilloteau et al. 2011; Stephens et al. 2014, to name a few).”
Forming the cores of giant planets from the radial pebble flux in protoplanetary discs (2014, background): “Similarly, sub-mm/mm surveys find outer radii of ∼100 AU, with some protoplanetary discs much larger (Kitamura et al. 2002; Mohanty et al. 2013).”
Can Giant Planets Form by Direct Gravitational Instability? (2004, background): “10 2 K at 10 AU (e.g. Kitamura et al. 2002).”
PROTOPLANETARY DISK STRUCTURES IN OPHIUCHUS. II. EXTENSION TO FAINTER SOURCES (2010, background): “Interferometric observations of dust and trace gas species have helped quantify densities in the outer parts of circumstellar disks (Kitamura et al. 2002; Andrews & Williams 2007a; Hughes et al. 2008; Isella et al. 2009), clearly established the presence of vertical temperature and density…”
PROTOPLANETARY DISK STRUCTURES IN OPHIUCHUS (2009, methodology): “…been derived from such fits, based on the millimeter continuum data alone (Lay et al. 1994, 1997; Mundy et al. 1996) or in combination with the broadband spectral energy distribution (SED; Wilner et al. 2000; Testi et al. 2001; Akeson et al. 2002; Kitamura et al. 2002; Andrews & Williams 2007a).”
RESOLVED IMAGES OF LARGE CAVITIES IN PROTOPLANETARY TRANSITION DISKS (2011, background): “…on viscous evolution, based on tracking the decline of accretion rates with age (e.g., Sicilia-Aguilar et al. 2010) and characterizing disk sizes and surface density profiles with resolved millimeter observations (Kitamura et al. 2002; Andrews et al. 2009, 2010b; Isella et al. 2009, 2010a).”
Circumstellar Dust Disks in Taurus-Auriga: The Submillimeter Perspective (2005, background): “2 The inner and outer disk radii are typical values based roughly on the dust sublimation temperature (e.g., Dullemond, Dominik, & Natta 2001; Muzerolle et al. 2003) and direct disk size measurements (e.g., Dutrey et al. 1996; Kitamura et al. 2002; Akeson et al. 2005).”
Interpreting Spectral Energy Distributions from Young Stellar Objects. I. A Grid of 200,000 YSO Model SEDs (2006, background): “…in low-mass YSOs, whether during the early infall phase or during the T-Tauri phase (e.g. Beckwith et al. 1990; Terebey et al. 1993; Dutrey et al. 1996; Kitamura et al. 2002; Looney et al. 2003; Andrews & Williams 2005), higher disk masses around high-mass YSOs, and disk masses down to Mdisk/M⋆ =…”
STRUCTURE AND EVOLUTION OF PRE-MAIN-SEQUENCE CIRCUMSTELLAR DISKS (2009, background): “On the other hand our RY Tau results agree well with recent optical observations (St-Onge & Bastien 2008) suggesting that the discrepancies may be due to the lower S/N ratio of Andrews et al. (2007) observations compared with the new CARMA results.”
Evolution of protoplanetary disks: Constraints from DM Tauri and GM Aurigae (2005, methodology): “In order to account for the uncertainty on κ0 we hence consider cases for which the 100AU gas surface density is either multiplied or divided by a factor 3 compared to the values obtained by Kitamura et al. (2002).”
Spiral Structure in the Circumstellar Disk around AB Aurigae (2004, background): “…disk mass of 0.02 (Mannings & SargentM, 1997; Henning et al. 1998) and the radial dependence of surface density as , as observed for several T Tauri disks 0.5S ∝ r (Kitamura et al. 2002), with km s 1 ( K;c p 0.23 T p 15S Miroshnichenko et al. 1999) and the assumed Kepler rotation, we obtain at AU.”