3D Hydrodynamics Simulations of Gravitational Instabilities in Irradiated Protoplanetary Disks

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3D Hydrodynamics Simulations of Gravitational
Instabilities in Irradiated Protoplanetary Disks
K. Cai et al. The Effects of Envelope
Irradiation
No Irr
Irr 25K
?A? 1.51, Peak Torq. 1.5 Global tcool 2.7
ORPs
?A? 1.01, Peak Torq. 2.2 Global tcool 5
ORPs
14 ORPs 3500 yr
Irr 50K
Irr 15K
?A? 1.16, Peak Torq. 2.0 Global tcool 3.2
ORPs
?A? ? 0.40, Peak Torq. 0.2 Global tcool 9 ORPs
Simulations compared during the asymptotic phase
Cai et al. (2007, in prep)
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DISC FRAGMENTATION FORMS BROWN DWARFS NOT
PLANETS Dimitris Stamatellos Anthony Whitworth
Formation of giant planets close to the star
(Rlt60 AU) by disc fragmentation is unlikely, but
discs can fragment at Rgt100 AU to form brown
dwarfs.
Disc does not fragment because it cannot cool fast
Disc does not fragment because it is too hot
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Turbulence and Dead Zones in Protostellar Disks
Neal Turner JPL/Caltech Takayoshi Sano Osaka U.
Natalia Dziourkevitch MPIA
Gammie 1996
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High Spatial Resolution SMA Imaging of
Transitional Disk LkH? 330
Joanna Brown, G. A. Blake, C. Qi, C.P. Dullemond,
D. Wilner C. Salyk

• Found in c2d Spitzer data to have mid-IR emission
  deficit
• SMA 340 GHz imaging confirms our SED modeling
  predictions of 50 AU gap in the disk
• Direct test of SED gap clearing interpretation

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AB Aur
TEXES/Gemini Survey for H2 in Protoplanetary Disks
M. Bitner (U. Texas)

• High-resolution (R100,000) observations at
  8,12,17 mm
• Observed range of source types (cTTs, wTTs,
  debris disk, Herbig Ae)
• So far, 5 of 20 sources observed show H2
  emission
• Mid-IR lines sensitive to gas temperatures
  between 200-800 K
• Simultaneous fit of all three lines from AB Aur
  gives T670 K and M0.5 Mearth
• Assuming i17o (Semenov et al., 2005), line
  widths imply emission located near 18 AU in disk.

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TEXES/Gemini Detection of Water in a Disk Around
RW Aur A Claudia Knez1, John Carr2, John Lacy3,
Matthew Richter4, Martin Bitner3, Dan Jaffe3,
Joan Najita5, Geoff Blake6, Joanna Brown6, Tom
Geballe7, Ewine van Dishoeck8 1. University of
Maryland , 2. Naval Research Laboratory, 3.
University of Texas at Austin, 4. University of
California, Davis, 5. NOAO, 6. Caltech, 7. Gemini
Observatory, 8. Leiden University
Hot water located in a disk within 1 AU of the
central star!!
Water emission as seen with Spitzer/IRS
TEXES resolved profile
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High-Resolution IR Spectroscopy A look inside
Transitional Disks
C. Salyk, G.A. Blake, J.M. Brown, A.C.A.
Boogert California Institute of Technology
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Probing protoplanetary disk evolution with the
HI 21cm line P3-9 I.Kamp, W. Freudling, M.
Robberto, J. Chengalur, E. Keto
HD141569 d99 pc

• b Pictoris
• blue HI 21cm
• red WFPC2

100 AU
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Disk evolution through a SED perspectiveOliveira,
Merín, Sicilia-Aguilar, van Dishoeck
Pontoppidan

Follow-up optical spectroscopic survey to
characterize central sources
Disk
Star
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Probing the Dust and Gas of Transitional Disks
in ChamaeleonCatherine Espaillat, Nuria Calvet,
Paola DAlessio, Edwin Bergin, Lee Hartmann, Dan
Watson, Elise Furlan, Joan Najita, William
Forrest, Melissa McClure, Ben Sargent, Chris
Bohac, Samuel Harrold
P3-11

• CS Cha has an optically thick disk truncated at
  43 AU, the largest hole modeled in a
  transitional disk.
• The disk of CS Cha has bigger grains and more
  settling than the previously modeled transitional
  disks DM Tau and GM Aur.
• The Spitzer IRS spectrum has Ne II 12.81?m
  fine-structure emission.

• We find a possible correlation of Ne II
  luminosity with accretion rate.
• - If confirmed, this would suggest that EUV
  fluxes due to accretion could be the main agent
  for formation of the Ne II line (Hollenbach
  Gorti, in prep).

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Dust dynamics during protoplanetary disc clearing
Richard Alexander Phil Armitage (JILA,
University of Colorado) astro-ph/0611821

• Model dust and gas evolution during clearing
  phase of evolution.
• Consider observations of inner hole sources,
  and how to discriminate between different models.

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Multiwavelength Imaging of Edge-on Circumstellar
DisksDeborah Padgett (SSC/Caltech) et al.
WFPC2/ACS
NICMOS

• Some of the clearest disk images are for the
  edge-on systems
• Project goals
• 1). Acquire high resolution optical and
  near-infrared images for a dozen young edge-on
  disks.
• 2). Use scattered light and SED modeling to
  derive disk structure and dust grain properties.

data
model
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The inner dust rim of Herbig Ae star - MWC275 A
view into the dust to gas transition region.
We have obtained near- IR Interferomtery (with
the CHARA array) on a YSO - MWC275, with
baselines greater than 300m (0.7 mas resolution)
for the first time.
IOTA
Keck Interferometer

• Results indicate the presence of near-IR gas
  emission from within the dust destruction radius.

CHARA
A. Tannirkulam, J. D. Monnier, Rafael
Millan-Gabet, Tim Harries Theo ten Brummelaar