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Stellar Obliquities in Exoplanetary Systems: Insights from MIT Research

This study presents a comprehensive analysis of stellar obliquities in exoplanetary systems based on research from the Massachusetts Institute of Technology (MIT). The work by Josh Winn and collaborators investigates the impacts of obliquity—from deviations in parallelism to correlations with eccentricity—in the dynamics of disk-planet interactions. Key findings include the identification of the Sanchis-Nutzman effect and its implications for understanding tidal dissipation and the behavior of exoplanets like HD 189733 and XO-3. Our observations reveal new insights into how stellar orientation can influence planetary systems.

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Stellar Obliquities in Exoplanetary Systems: Insights from MIT Research

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  1. Stellar obliquities in exoplanetary systems Massachusetts Institute of Technology Josh Winn • Simon Albrecht, Roberto Sanchis-Ojeda, Teruyuki Hirano • Andrew Howard, John Johnson,Geoff Marcy • Bill Cochran, Dan Fabrycky, the Keplerteam

  2. obliquity (n.) 1 : deviation from parallelism 2 : a deviation from moral rectitude or sound thinking

  3. Eccentricity Jupiter Semimajor axis [AU]

  4. Eccentricity Low obliquity Disk-planet interactions Semimajor axis [AU]

  5. Few-body dynamics High obliquity Tidal dissipation Eccentricity Low obliquity Disk-planet interactions Semimajor axis [AU]

  6. The Sanchis–Nutzman effect

  7. l = 0°

  8. l = 0°

  9. l = 0°

  10. l = 0°

  11. l = 0°

  12. l = 0°

  13. l = 100° l = 0°

  14. l = 100° l = 0°

  15. l = 100° l = 0°

  16. l = 100° l = 0°

  17. l = 100° l = 0° …

  18. l = 100° l = 0° …

  19. l = 100° l = 0° …

  20. l = 100° l = 0° Thestarspot-anomaly pattern reveals the stellar obliquity Sanchis-Ojeda et al. (2011 a,b) Nutzman, Fabrycky, & Fortney (2011) …

  21. Corot-2 Nutzman, Fabrycky, & Fortney (2011)

  22. Corot-2 Observed Calculated (l = 0°) l = 5 ± 12° Nutzman, Fabrycky, & Fortney (2011) — see also Désert et al. (2011)

  23. HAT-P-11 Sanchis-Ojeda & Winn (2011)

  24. Time from midtransit [days] Sanchis-Ojeda & Winn (2011)

  25. Sanchis-Ojeda & Winn (2011)

  26. Sanchis-Ojeda & Winn (2011)

  27. ChristophScheiner(1573-1650)

  28. Flux Time The Rossiter-McLaughlin effect

  29. Doppler shift Time The Rossiter-McLaughlin effect

  30. Doppler shift Time The Rossiter-McLaughlin effect

  31. Doppler shift Time The Rossiter-McLaughlin effect

  32. Doppler shift Time The Rossiter-McLaughlin effect

  33. Doppler shift Time The Rossiter-McLaughlin effect

  34. Measuring the projected obliquity Queloz et al. (2000); Ohta, Taruya, & Suto(2005); Gaudi &Winn (2007)

  35. Low obliquity HD 189733 l = –1.4° ± 1.1° Winn et al. (2006); see also Triaud et al. (2009)

  36. Moderate obliquity XO-3 l = 37.3° ± 3.0° Hirano et al. (2011); see also Hébrard et al. (2008), Winn et al. (2009)

  37. High obliquity (retrograde) Winn et al. (2009) Narita et al. (2009) Triaud et al. (2010)

  38. Valenti & Fischer (2005) Pinsonneault et al. (2001)

  39. (Zahn 1977)

  40. Problem: Orbit decays on same timescale as realignment

  41. Solution: Realign only the convective zone?

  42. Reality

  43. Constant-Q model

  44. Different Q’s for realignment and orbital decay (D. Lai, in preparation)

  45. KOI-63 1.0 M , 1.0 R P = 9.4 days Rp = 6.5 R

  46. Prot = 5.4 days ≈ (4/7) Porb

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