Constraining the Envelope Properties and Locations of Planetary Bodies in the AB Aur System Jamie R Lomax (U of Oklahoma) John Wisniewski (OU) Carol Grady (Eureka/GSFC) and the SEEDS Team
Herbig Ae/Be Stars
Grady, et al Fukagawa, et al History of AB Aur Hashimoto, et al. 2011
Polarimetry of AB Aur Hashimoto, et al See also: Perrin, et al 2009
Location of the Spirals? Tang et al Hashimoto et al. 2011
Project Goals Trace movement of structures using 6 year baseline to determine the presence and location of possible planets. Hashimoto, et al When does the envelope contribute to scattered light images?
HOCHUNK3D Modeling M ʘ yr -1 5°-75° Infall Rate: Bipolar Cavity Opening Angle :
Infall Rate and Opening Angle Opening angle is significant above M ʘ yr -1.
Model SEDs
Modeling the Morphology J Band PI Goal: Reproduce overall morphology- gap location and visibility Hashimoto, et al. 2011
Example Model Morphology The envelope has little effect on the PI images.
Location of Planetary Bodies Fukagawa, et al Must be located >26 AU from central star Hashimoto, et al. 2011
Summary Tang, et al Not reproducing the Tang et al. cartoon Hashimoto et al Spirals suggest planetary body should be located >26 AU
Polarimetry of AB Aur Hashimoto, et al. 2011
Envelope Contribution High Infall, Large Opening High Infall, Small Opening Low Infall
Morphology Cross Cuts
Density
Future Work Radial profile comparisons Constrain rotation of spiral features to constrain location of planets
Model Images-Hershel PACS-1 PI
AB Aur Hashimoto, et al. 2011
AB Aur’s Envelope Grady, et al How does the envelope affect what we see?
Envelope Size Envelope size isn’t significant. Grady, et al. 1999