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Matt Stevans Dr. Sean Brittain Clemson Universitystevans/presentation1.pdf · Herbig AeBe Stars...
Transcript of Matt Stevans Dr. Sean Brittain Clemson Universitystevans/presentation1.pdf · Herbig AeBe Stars...
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Matt Stevans Dr. Sean Brittain
Clemson University
7/27/11 SARA REU 2011
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Today I will talk about…
1. How planets form 2. How we study planet
formation by modeling disks 3. Results and conclusions of
my work
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Planet Formation
Not to scale
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Herbig AeBe Stars
7/27/11 SARA REU 2011
� Young; 2-10 Solar Masses � Flared Disks
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Herbig AeBe Observables Spectral Energy Distribution (SED)
CO Emission Line Profiles in IR Excess
Mafiat 1998 Mafiat 1998
Brittain 2009
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Thermal-Chemical Model Thermal Structure at Surface
Tem
pe
ratu
re (
K)
Column Density (powers of 10)
10000
5000
2000
500
200 100
18 19 20 21 22 23 24
Tgas
Tdust
α=0.01
α=2
Settled Dust at mid plane
Gaseous Surface
Disk Cross-Section Glassgold 2004
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My work
� Assembled list of Herbig AeBe stars that have both CO and Brγ flux measurements.
� Reduced 9 spectra from PHOENIX at the Gemini Observatory.
7/27/11 SARA REU 2011
Observatory: Gemini
Instrument: PHOENIX
Wavelength: 1-5 microns
Resolution: ~65,000
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Results � CO flux scales
with Brγ flux. � Scatter in
correlation plot can be reduced with simultaneous observations of Brγ and CO.
Brγ Flux = Mass Accretion
CO
Flu
x
Typical Error Bars
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Take Away
� We cannot see into disks. � Accretion/viscous heating plays a
role in disk surface heating in inner disk.
� This needs to be incorporated into models.
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Acknowledgements
7/27/11 SARA REU 2011
This project was funded by the National Science Foundation Research Experiences for Undergraduates (REU) program through grant NSF AST-1004872 Thanks to Dr. Brittain for working with me this entire summer. Thanks Thomas Rice and Charles Kurgatt for many useful discussions.
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Extras
7/27/11 SARA REU 2011