observing how habitable conditions develop (or not) in protoplanetary disks
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Observing How Habitable Conditions Develop (Or Not) in Protoplanetary Disks. ?. Colette Salyk National Optical Astronomy Observatory. Credit: JPL-Caltech/T. Pyle (SSC). Credit: NASA. Why studying protoplanetary disks is important for understanding habitability. - PowerPoint PPT PresentationTRANSCRIPT
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Observing How Habitable Conditions Develop (Or Not) in Protoplanetary Disks
Colette SalykNational Optical Astronomy Observatory
Credit: JPL-Caltech/T. Pyle (SSC) Credit: NASA
?
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Why studying protoplanetary disks is important for understanding habitability
• Planet formation “laboratory” – ground truth for our ideas about how planets form and habitability develops
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Even if you don’t care how planets form…
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Milky way diameter: 40 kpc(120,000 light years)
Microlensing planets: 5 kpc
Kepler planets: 2 kpc
Imaged planets: 0.2 kpc
Credit: Exoplanet app
Planet detection remains difficult at large distances, and characterization even more so
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Why studying protoplanetary disks is important for understanding habitability
• Planet formation “laboratory” – ground truth for our ideas about how planets form and habitability develops
• Understanding formation process allows us to extrapolate to the rest of the galaxy/universe
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• Overview of what we do and don’t know about protoplanetary disks
• Current studies of development of Goldilocks properties:– Location– Planet size and type– Chemistry
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Composed of gas and (opaque) dust, Few 100 AU in size
CO velocity in HD 163296 (ALMA)
de Gregorio-Monsalvo et al. 2013
Opaque disks in Orion (Hubble)1800 AU
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Small (but evolved) dust, consistent with olivine composition
Spitzer spectra of Si-O stretch
Chondrule from American Museum of Natural History meteorite collection
Kessler-Silacci et al. 2006
Data
Models
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Small (but evolved) dust, consistent with olivine composition
Chondrule from American Museum of Natural History meteorite collection
Spitzer spectra of Si-O stretch
Kessler-Silacci et al. 2006
Data
Models
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Protoplanetary disks are ubiquitous*
Kraus & Ireland, 2011
*around sun-like stars in nearby star-forming regions
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Protoplanetary disks last a few Myr
Kraus & Ireland, 2011
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Masses are consistent with Minimum Mass Solar Nebula, or slightly lower
Ophiuchus data from Andrews et al. 2007
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Masses are consistent with Minimum Mass Solar Nebula, or slightly lower
Ophiuchus data from Andrews et al. 2007∨
small
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• Planet size and location: Snow lines and disk dispersal
• Chemistry: Chemical inventories of planet forming regions
Active research related to habitability
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What processes determine planetary size and location?
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Gas giantsTerrestrial planets
What processes determine planetary size and location?
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Gas giantsTerrestrial planets
The “snow line” – an increase in solid surface density
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What is the expected location of the snow line?
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What is the expected location of the snow line?
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Gas giantsTerrestrial planets
The “snow line”
Habitable zone
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Multi-wavelength observations of water vapor measure snow line locations
ice lineK. Pontoppidan
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First measured locations of snow lines in disks
Meijerink+ 2009Zhang+ 2013
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First measured locations of snow lines in disks
Meijerink+ 2009Zhang+ 2013
See poster by Sandra Blevins for an update!
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Gas giantsTerrestrial planets Ice giants (super Earths?)
Planet type affected by disk dispersal
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Dispersal of disk gas also affects planet migration
Snapshot of disk surface densitywith planet undergoing migration
P. Armitage
1 10 100
# of planets
Orbital Period [days]
Hot Jupiters
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How do disks evolve/disperse?Disk winds
Blandford & Payne 1982Pudritz & Norman 1983Cartoon inspired by Bai et al. 2013
B wind
accretion
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Molecular emission lineshapes and images – evidence for disk winds?
Pontoppidan+ 2009; also Bast+ 2011
Flux
Velocity
ALMA CO velocity field
Salyk+ in prepBrown+ 2013
Vibrational CO
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How do disks evolve/disperse?Photoevaporative winds wind
FUVEUVX-ray
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How do disks evolve/disperse?Photoevaporative winds wind
FUVEUVX-ray
?
Main open question: How quickly do disks dissipate at each disk radius?
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Observations of photoevaporation tracers measure location and mass-loss
[Ne II] emission from two disks + models
Pascucci & Sterzik 2009
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• Chemistry: Chemical inventories of planet forming regions
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Solar data from Grevesse et al. 2010Chondrite data from Allegre et al. 2001
CI chondrite abundances vs. solar abundances(R ~ 4 AU)
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Earth abundances vs. solar abundances(R = 1 AU)
Solar data from Grevesse et al. 2010Chondrite data from Allegre et al. 2001
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N2, HCN, NH3, organics ?
CO, CO2, organics, graphite?
Earth abundances vs. solar abundances(R = 1 AU)
Solar data from Grevesse et al. 2010Chondrite data from Allegre et al. 2001
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What is the correct chemical pathway? Inheritance or reset?
Maximum “reset”
Maximum “Inheritance”
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Resemblance between cometary and cloud ice compositions = an inheritance assumption
Data from Mumma & Charnley 2011 (and references therein)
Cometary abundance% relative to water
Cloud abundance% relative to water
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Evidence for reset in the solar system: CAIs and chondrules
Chondrule
Calcium Aluminum-rich Inclusion (CAI)
Thin sections from the American Museum of Natural History meteorite collection
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Carr & Najita 2008Also, Salyk+ 2008
The study of chemistry in inner disks was enabled by the Spitzer InfraRed Spectrograph (IRS)
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O,C,N inventory in inner disks is being measured
Pontoppidan+ 2014
O C N
Fraction
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Evidence for reset in disks: O,C,N inventory different from birth cloud
Salyk et al. 2011; Öberg et al. 2011
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Evidence for reset in disks: Variability in disk chemistry
Banzatti et al. 2012
See poster by Andrea Banzatti
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Current: Partial chemical inventory, evidence for reset
Yet to come: Chemical differences between disks, and as a function of radius
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• Basic protoplanetary disk properties have been characterized
• Studies of development of Goldilocks properties ongoing:– Location– Planet size and type– Chemistry
Conclusions
Measuring snow linesObserving disk evolution/dispersal
Chemical inventory in planet-forming regions, evidence for reset, details yet to come
Questions about observing disks?