1. 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

2. Herbig Ae/Be Stars

3. Grady, et al. 1999 Fukagawa, et al. 2004 History of AB Aur Hashimoto, et al. 2011

4. Polarimetry of AB Aur Hashimoto, et al. 2011 See also: Perrin, et al 2009

5. Location of the Spirals? Tang et al. 2012 Hashimoto et al. 2011

6. Project Goals Trace movement of structures using 6 year baseline to determine the presence and location of possible planets. Hashimoto, et al. 2011 When does the envelope contribute to scattered light images?

7. HOCHUNK3D Modeling 10 -5 -10 -10 M ʘ yr -1 5°-75° Infall Rate: Bipolar Cavity Opening Angle :

8. Infall Rate and Opening Angle Opening angle is significant above 10 -7 M ʘ yr -1.

9. Model SEDs

10. Modeling the Morphology J Band PI Goal: Reproduce overall morphology- gap location and visibility Hashimoto, et al. 2011

11. Example Model Morphology The envelope has little effect on the PI images.

12. Location of Planetary Bodies Fukagawa, et al. 2004 Must be located >26 AU from central star Hashimoto, et al. 2011

13. Summary Tang, et al. 2012 Not reproducing the Tang et al. cartoon Hashimoto et al. 2011 Spirals suggest planetary body should be located >26 AU

16. Polarimetry of AB Aur Hashimoto, et al. 2011

17. Envelope Contribution High Infall, Large Opening High Infall, Small Opening Low Infall

18. Morphology Cross Cuts

19. Density

20. Future Work Radial profile comparisons Constrain rotation of spiral features to constrain location of planets

22. Model Images-Hershel PACS-1 PI

23. AB Aur Hashimoto, et al. 2011

24. AB Aur’s Envelope Grady, et al. 1999 How does the envelope affect what we see?

25. Envelope Size Envelope size isn’t significant. Grady, et al. 1999