Millimeter-Wavelength Observations of Circumstellar Disks and what they can tell us about planets A. Meredith Hughes Miller Fellow, UC Berkeley David Wilner, Sean Andrews, Charlie Qi, Catherine Espaillat, Jonathan Williams, Nuria Calvet, Paola D’Alessio, Antonio Hales, Simon Casassus, Michael Meyer, John
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Millimeter-Wavelength Observations of Circumstellar Disks and what they can tell us about planets A. Meredith Hughes Miller Fellow, UC Berkeley David Wilner,
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Millimeter-Wavelength Observations of Circumstellar
Disks
and what they can tell us about planets
A. Meredith HughesMiller Fellow, UC Berkeley
David Wilner, Sean Andrews, Charlie Qi, Catherine Espaillat, Jonathan Williams, Nuria Calvet, Paola D’Alessio, Antonio Hales, Simon Casassus, Michael Meyer, John Carpenter, Michiel Hogerheijde
Star and Planet Formation Overview
cloud grav. collapseprotostar+ disk
+ envelope + outflow
PMS star+ disk
MS star+ debris disk+ planets?
Adapted from Shu et al. 1987
Circumstellar Disk Evolution
Protoplanetary
Pre-MS stars
Gas-rich
Primordial dust
Debris_____
Main sequence
No (or very little) gas
Dust must be replenished
planets?
Some Questions:What physical processes shape each stage?
What physical processes drive dispersal?When and how do planets form?
What are the properties of the planets?
AU Mic, Liu et al. 2004HH 30, Burrows et al. 1996
F
Circumstellar Disk Structure
star disk
Why Millimeter Interferometry?
• Optically thin dust emission• Molecular line emission• High spatial resolution
3. Resolution:• Measuring accurate cavity sizes• Gaps
4. Sensitivity + Resolution:• Planetary accretion luminosity• Gas in the cavity
log
log
F
duststar
“Pre-Transitional” SED
Wolf & D’Angelo (2005)
2. Resolving Debris Disk Structure
Debris DisksFomalhautKalas et al. (2005)
Weinberger et al. (1999)
PicFitzgerald et al. (2007)
HR 4796ASchneider et al. (1999)
Debris DisksIf debris disks were primordial, they wouldn’t be there
dust ≤10 Myr
Debris disks look different at different wavelengths
70 m; Su et al. (2005) 350 m; Marsh et al. (2006) 850 m; Holland et al. (2006)
At least 15% of nearby main-sequence stars have debris disks(Habing et al. 2001, Rieke et al. 2005, Trilling et al. 2008, Hillenbrand et al. 2008)
How Debris Disks Tell Us about Planets
1. Access to otherwise unobservable Uranus/Neptune analoguesQuickTime™ and aTIFF (Uncompressed) decompressor
are needed to see this picture.
QuickTime™ and aCinepak decompressor
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Courtesy M. Wyatt
Wilner et al. (2002)
How Debris Disks Tell Us about Planets
1. Access to otherwise unobservable Uranus/Neptune analoguesQuickTime™ and aTIFF (Uncompressed) decompressor
are needed to see this picture.
Hughes et al. (in prep)
Corder et al. (2009)CARMA 230 GHz
HD 107146
How Debris Disks Tell Us about Planets
2. Vertical structure of edge-on debris disksQuickTime™ and aTIFF (Uncompressed) decompressor
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From Thebault et al. (2009)
Wilner et al. (in prep)
How Debris Disks Tell Us about Planets
3. Constraints on the masses of directly-imaged planets
Chia
ng e
t al. (2
009)
QuickTime™ and aTIFF (Uncompressed) decompressor
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Kalas et al. (2008)
How Debris Disks Tell Us about Planets
3. Constraints on the masses of directly-imaged planets
Hughes et al. (in prep)
QuickTime™ and aTIFF (Uncompressed) decompressor
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What’s next?
QuickTime™ and aTIFF (Uncompressed) decompressor
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QuickTime™ and aTIFF (Uncompressed) decompressor
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What will ALMA do?
• (Some) debris disks will be roughly as easy to image as protoplanetary disks are now• Statistics - planet populations• Excellent linear resolution• (Molecular gas?)