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Probing Planetary Gap Formation in Protoplanetary Disks: Insights from TW Hya Observations

Dr. Hannah Jang-Condell explores the phenomenon of gap opening in protoplanetary disks due to planet formation, focusing on the TW Hya system. This research leverages observations from Hubble Space Telescope (HST) and other instruments to analyze gaps' characteristics and their implications for planet mass and formation epochs. The study utilizes thermal emission models and examines the impact of scattering light at various wavelengths, providing crucial insights into the dynamics within these young, gas-dominated disks and the conditions for giant planet formation.

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Probing Planetary Gap Formation in Protoplanetary Disks: Insights from TW Hya Observations

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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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