Short-term variability in pre-transtional disks around high-mass pre-main sequence stars
Abstract
We propose multi-epoch mid-infrared observations of 3 known pre-transitional disks around young high-mass stars (HAeBe and Be type). Transitional and pre-transitional disks are thought to represent stages in disk evolution from optically thick evolved disks to optically thin debris disks, during which central holes and gaps are created, possibly due to the planet formation process. The mid-infrared ``see-saw'' variability in pre-transitional disks is thought to be caused by vertical perturbations in the inner-disk, possibly due to the interaction between an unseen planetary companion and the inner disk wall. However, this model has only been tested/confirmed for low-mass young stellar objects (YSOs). Our aim is to further test this model by observing higher-mass pre-main sequence objects with known pre-transitional disks to look for variability on week to month-long timescales. If the vertical perturbation model is correct, then we expect to see the ``see-saw'' variability shift from weekly to monthly (or longer) timescales, due to the increased physical size of the circumstellar disk for high-mass stars. If the ``see-saw'' variability is observed on weekly timescales, then the model may need to be revisited and additional explanations explored. If the observed variability is different--or absent--this would indicate that the dynamics and energetics associated with pre-transitional disks around hot stars is quite different than for their low-mass cousins, despite the fact that they share very similar architectures.
- Publication:
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SOFIA Proposal
- Pub Date:
- 2016
- Bibcode:
- 2016sofi.prop..138S
- Keywords:
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- SOFIA 05_0138