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Observing Gap Opening By Planets

Observing Gap Opening By Planets. Dr. Hannah Jang-Condell Michelson Fellow University of Maryland NASA’s Goddard Space Flight Center. Protoplanetary Disks. TW Hya. T Tauri (F,G,K stars) or Herbig Ae /Be (A,B stars) Young (~ 1 Myr ) Optically thick Gas-dominated

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Observing Gap Opening By Planets

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  1. Observing Gap OpeningBy Planets Dr. Hannah Jang-Condell Michelson Fellow University of Maryland NASA’s Goddard Space Flight Center Jang-Condell

  2. Protoplanetary Disks TW Hya • T Tauri (F,G,K stars) or HerbigAe/Be (A,B stars) • Young (~1 Myr) • Optically thick • Gas-dominated • Era of Giant Planet formation AB Aur Debes, et al. in prep HST/STIS Fukagawa, et al. 2004 Jang-Condell

  3. Probing the Epoch of Formation Protoplanetary disk Jang-Condell

  4. Calculating Observables To observer =2/3 Flared disk Jang-Condell

  5. Scattered Light F* FincF*/r2 i =2/3 Thermally reprocessed: Td 3D RT model Jang-Condell 2009 Jang-Condell

  6. Thermal Emission dI/dl =  B(Td) exp(-) =2/3 Thermally reprocessed Jang-Condell 2009 Jang-Condell

  7. Simulated Images Shorter wavelengths, higher opacities, probe surface layers Longer wavelengths, lower opacities, probe deeper Flared disk Jang-Condell

  8. Gap Opening by Planets • Bate et al., 2003 • Gap-opening threshold: rHill= (Mcrit/3M*)1/3a = H • Mcrit = 0.38 MJ 1 MJ 0.3 MJ 0.1 MJ 10 ME Jang-Condell

  9. Gap Profiles 0.08 Mcrit 0.27 Mcrit 0.8 Mcrit 2.7 Mcrit Bate et al., 2003 Jang-Condell

  10. Shadow Feedback Aristarchus crater, the Moon Credit: NASA (Apollo 15) Jang-Condell

  11. 1/3 Jupiter Mass at 10 AU Jang-Condell

  12. No planet 37 MEarth 110 MEarth Gap At 10 AU 1 μm 30 μm 100 um Jang-Condell Jang-Condell,submitted

  13. Inclination dimmer brighter Jang-Condell

  14. No planet 37 MEarth 110 MEarth 45° Incl. 1 μm 30 μm 100 um Jang-Condell Jang-Condell, submitted

  15. LkCa 15 (Espaillat, et al. 2008) H-band scattered light Thalmann et al., 2010 < 6 MJ (Mulders, et al. 2010) Jang-Condell

  16. LkCa 15 models Jang-Condell, submitted Jang-Condell

  17. Lower mass limit: 1.5 MJ Jang-Condell

  18. LkCa 15 Radio Images Piétu, et al. 2006 (IRAM) 2.8 mm 1.4 mm 0.5 MJ 1.3 mm 1.5 MJ Isella, et al. (CARMA) Jang-Condell, submitted Jang-Condell

  19. LkCa 15 model SED Bigger gaps appear brighter Jang-Condell

  20. TW Hya • 56 AU • Hubble observations • STIS • NICMOS • 7 wavelengths • Debes, Jang-Condell, et al. (in prep) Jang-Condell

  21. Multi-wavelength Fit Fit parameters: • Gap depth • 30%, 50% • Gap width • 10, 20, 30 AU • Grain size • amin 0.005, 0.5, 5 um • Disk truncation • 60, 80, 100 AU • Gap depth 30% Debes, Jang-Condell, et al., in prep Jang-Condell

  22. rHill~H Partial Gaps 1 MJ 0.3 MJ • Gap-opening threshold: • rHill =(Mp/3M*)1/3a = H • for TW Hya, @ 80 AU: Mcrit = 0.9 MJup • 30% gap: ~0.3 MJup = Saturn mass 50% gap 0.1 MJ 10 ME 3 ME 1 ME Bate, et al. 2003 Jang-Condell

  23. TW HyaGap vs. Gapless Gap is apparent in the brightness profile from optical to far-IR wavelengths Thi et al. 2010 PACS observations of TW Hya “No extended emission has been found.” Jang-Condell

  24. Summary • Self-shadowing in gaps enhances the gap depth • Gaps are detectable in resolved disk images • May be detectable in SEDs also • Can infer planet masses from the observed gaps sizes Jang-Condell

  25. 7 degrees inclination Isotropic scattering Jang-Condell

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