Debris Disk Phase
Spectroscopic searches for disk gas (steady state)
- CO emission (mm-wave measurements)
- H2 infrared features (ISO; ground)
- H2; CO ultraviolet absorption features
Results
- Significant differences between (uv; ground) and ISO
- Concensus: [gas/dust] << ISM value
- Not enough to build giant planets
- Could mitigate dust migration; quantitative study needed
- Suggestion that gas is ësecondaryí: evaporated volatiles
High priority for future work
- SIRTF observations of H2 spanning wide age range
- Knowledge of gas content key to modeling dust evolution
- Key Focus: young (5 ñ 20 Myr) debris disk stars
- Do post-accretion phase disks have gas sufficient to build giant planets?
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