Magnetic Channeling and Confinement in the Hypersonic Winds of Massive, Luminous Stars - PowerPoint PPT Presentation

shannon-anthony
magnetic channeling and confinement in the hypersonic winds of massive luminous stars n.
Skip this Video
Loading SlideShow in 5 Seconds..
Magnetic Channeling and Confinement in the Hypersonic Winds of Massive, Luminous Stars PowerPoint Presentation
Download Presentation
Magnetic Channeling and Confinement in the Hypersonic Winds of Massive, Luminous Stars

play fullscreen
1 / 43
Download Presentation
Magnetic Channeling and Confinement in the Hypersonic Winds of Massive, Luminous Stars
80 Views
Download Presentation

Magnetic Channeling and Confinement in the Hypersonic Winds of Massive, Luminous Stars

- - - - - - - - - - - - - - - - - - - - - - - - - - - E N D - - - - - - - - - - - - - - - - - - - - - - - - - - -
Presentation Transcript

  1. Rich Townsend University of Delaware Stan Owocki Asif ud-Doula Mary Oksala David Cohen Marc Gagné Steve Skinner Magnetic Channeling and Confinement in the Hypersonic Winds of Massive, Luminous Stars ESO Chile ̶ November 2006

  2. Overview - σ Ori E - θ1 Ori C

  3. Luminous

  4. Radiation-driven wind

  5. CNO cycle

  6. Convective core

  7. Radiative envelope

  8. magnetic field ? No * 1978 2002 2005

  9. Plasma Physics Stellar Evolution Compact Objects Circumstellar Environment

  10. θ1 Orionis C

  11. - θ1 Ori C (O5.5) θ Ori - Chandra ACIS-S Feigelson et al. (2002)

  12. 107 K / 1 keV / 1,000 km s-1 θ1 Ori C ζ Pup Wojdowski & Schulz (2005)

  13. Magnetically Confined Wind Shock Babel & Montmerle (1997)

  14. ZEUS - Density ud-Doula & Owocki (unpub.)

  15. ZEUS - Temperature ud-Doula & Owocki (unpub.)

  16. 107 K / 1 keV / 1,000 km s-1 Gagné et al. (2005)

  17. ZEUS - Density ZEUS - Temperature ud-Doula & Owocki (unpub.)

  18. . η = [B*R*/Mv∞] (r/R*) -4 2 2 η* rA/R* = η* 1/4 Magnetic Confinement η = B2/8π / ρv2/2

  19. ZEUS - Density ZEUS - Temperature ud-Doula & Owocki (unpub.)

  20. ! Field Strength Rotation Rate Mass-Loss Rate

  21. σOrionis E

  22. - σ Ori E (B2) σ Ori D (B2) - - σ Ori AB (O9.5 + B0.5) σ Ori - Chandra ACIS-S Skinner et al. (2004)

  23. 107 K / 1 keV / 1,000 km s-1 σ Ori AB σ Ori E σ Ori - Chandra ACIS-S Skinner et al. (2004)

  24. Landstreet & Borra (1978) Bohlender et al. (1987) Hesser et al. (1977)

  25. Kaufer et al. (1999)

  26. “ two more or less isolated clouds … near the intersection of the magnetic and rotational equator ” Groote & Hunger (1982)

  27. Field lines are almost rigid Field lines are almost rigid

  28. Rigidly Rotating Magnetosphere Townsend & Owocki (2005)

  29. Townsend, Owocki & Groote (2005)

  30. Townsend, Owocki & Groote (2005)

  31. Rigid Field Hydrodynamics Townsend, Owocki & ud-Doula (in prep.)

  32. Townsend, Owocki & ud-Doula (in prep.)

  33. Townsend, Owocki & ud-Doula (in prep.)

  34. Summary • New approaches for modeling magnetic confinement in massive stars • MHD • RRM • RF-HD • Rewarding success in reproducing optical & X-ray properties

  35. Ongoing & Future Work • Confrontation between RF-HD and UV, X-ray (& interferometric) observations • Hybrid RF-HD/MHD models to simulate centrifugal breakout • Laboratories for understanding magnetic-radiation-rotation interaction • Synergies with other classes of magnetic object – Polar, AB Dor, Magnetar

  36. http://shayol.bartol.udel.edu/massivewiki/

  37. Sanz-Forcada et al. (2004)

  38. Centrifugal Breakout ZEUS - Density ud-Doula, Townsend & Owocki (2006)

  39. ZEUS - Temperature ud-Doula, Townsend & Owocki (2006)