TY - JOUR
T1 - RESOLVING PROTOPLANETARY DISKS at MILLIMETER WAVELENGTHS with CARMA
AU - Kwon, Woojin
AU - Looney, Leslie W.
AU - Mundy, Lee G.
AU - Welch, William J.
N1 - Publisher Copyright:
© 2015. The American Astronomical Society. All rights reserved.
PY - 2015/7/20
Y1 - 2015/7/20
N2 - We present continuum observations at λ = 1.3 and 2.7 mm using the Combined Array for Research in Millimeter-wave Astronomy toward six protoplanetary disks in the Taurus molecular cloud: CI Tau, DL Tau, DO Tau, FT Tau, Haro 6-13, and HL Tau. We constrain physical properties of the disks with Bayesian inference using two disk models: the flared power-law disk model and flared accretion disk model. Comparing the physical properties, we find that the more extended disks are less flared and that the dust opacity spectral index (β) is smaller in the less massive disks. In addition, disks with a steeper mid-plane density gradient have a smaller β, which suggests that grains grow and radially move. Furthermore, we compare the two disk models quantitatively and find that the accretion disk model provides a better fit overall. We also discuss the possibilities of substructures on three extended protoplanetary disks.
AB - We present continuum observations at λ = 1.3 and 2.7 mm using the Combined Array for Research in Millimeter-wave Astronomy toward six protoplanetary disks in the Taurus molecular cloud: CI Tau, DL Tau, DO Tau, FT Tau, Haro 6-13, and HL Tau. We constrain physical properties of the disks with Bayesian inference using two disk models: the flared power-law disk model and flared accretion disk model. Comparing the physical properties, we find that the more extended disks are less flared and that the dust opacity spectral index (β) is smaller in the less massive disks. In addition, disks with a steeper mid-plane density gradient have a smaller β, which suggests that grains grow and radially move. Furthermore, we compare the two disk models quantitatively and find that the accretion disk model provides a better fit overall. We also discuss the possibilities of substructures on three extended protoplanetary disks.
KW - circumstellar matter
KW - protoplanetary disks
KW - radio continuum: stars
KW - stars: pre-main sequence
KW - techniques: interferometric
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U2 - 10.1088/0004-637X/808/1/102
DO - 10.1088/0004-637X/808/1/102
M3 - Article
AN - SCOPUS:84937849381
SN - 0004-637X
VL - 808
JO - Astrophysical Journal
JF - Astrophysical Journal
IS - 1
M1 - 102
ER -