Topological Forcing Semantics with Settling Robert S. Lubarsky Florida Atlantic University.
Chemistry of Protoplanetary Disks with Grain Settling and Lyman α Radiation Jeffrey Fogel, Tom...
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Transcript of Chemistry of Protoplanetary Disks with Grain Settling and Lyman α Radiation Jeffrey Fogel, Tom...
Chemistry of Protoplanetary
Disks with Grain Settling and Lyman
α Radiation
Jeffrey Fogel, Tom Bethell and Edwin BerginUniversity of Michigan
Stellar Radiation Field
•UV Excess due to shock
•most models used a scaled up ISRF
•Full UV field from D’Alessio et al
•Analytical scattering calculation from Bergin et al. 2003
Gullbring et al 2000
Dust•Major heating agent in the disk due
to absorption
•SED depends on the dust grain settling
- ε = dust-to-gas ratio in the upper layers as compared with the ISM
•Observations by D’Alessio et al. 2006 indicate that the median SED in Taurus fits ε ~ 0.01
Lyman α• Dominates UV radiation field - in TW Hya
carries 75% of FUV flux (Herczeg et al 2004)
• Important for chemistry. e.g. HCN and H2O will be dissociated by Ly α photons -- CN is not (Bergin et al 2003).
Bergin et al. 2003
Red = BP TauBlue = TW Hya
dashed = scaled ISRF
Chemical Network• 639 Species
• 5902 Reactions
• Herbst’s gas-phase network plus:
- Photodissociation:
- X-ray ionization (Glassgold et al. 1997)
- UV Photolysis induced by X-rays (Gredel et al. 1989, Aikawa & Herbst 2001)
- Grain Reactions (freeze-out, evaporation, cosmic-ray desorption, photodesorption)
- H2, CO self-shielding
Conclusions• Important to include true stellar UV field
and calculate photodissociation rates from it
•Dust settling and Lyman α radiation play significant roles in the chemistry of protoplanetary disks
•Next step is to calculate column densities and show what can be observed now and in the future with ALMA