Characterizing Magnetized Turbulence through Magnetic Field Dispersion Martin Houde The University of Western Ontario CC2YSO - 19 May 2010.

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Presentation transcript:

Characterizing Magnetized Turbulence through Magnetic Field Dispersion Martin Houde The University of Western Ontario CC2YSO - 19 May 2010

Collaborators: Roger H. Hildebrand (U of Chicago) Ramprasad Rao (ASIAA/SMA) John E. Vaillancourt (NASA Ames) Larry Kirby (U of Chicago) Shadi Chitsazzadeh (Western/U of Victoria) Jessie L. Dotson (NASA Ames) Other SHARP team members: Giles Novak (Northwestern U) C. Darren Dowell (Caltech/NASA JPL) CC2YSO - 19 May 2010

Outline Dispersion of magnetic fields No modeling of ordered field Turbulent/ordered field energy ratio Application/results Single-dish - OMC-1, CSO/SHARP Turbulence correlation length Turbulent/ordered field energy ratio (CF equation) Interferometry - NGC 1333 IRAS 4A, SMA Magnetized turbulent power spectrum CC2YSO - 19 May 2010

ordered + turbulent fields OMC-1 - SHARP/CSO, 350 and 450 µm “Dispersion” of Magnetic Fields CC2YSO - 19 May 2010 Vaillancourt et al., 2008, ApJ, 679, L25

The Angular Dispersion Function turbulent ordered + turbulent fields turbulent level ordered field CC2YSO - 19 May 2010

OMC-1 with SHARP at 350 µm Houde et al. 2009, ApJ, 706, 1504 CC2YSO - 19 May 2010

OMC-1 / SHARP - Results Houde et al. 2009, ApJ, 706, 1504 CC2YSO - 19 May 2010

NGC1333 IRAS 4A with SMA at 850 µm B-vectors beam: 1.6”x 1.0” sampling: 0.2” CC2YSO - 19 May 2010

NGC1333 IRAS 4A / SMA - Results CC2YSO - 19 May 2010Houde et al. 2010

NGC1333 / SMA - Turbulent Spectrum CC2YSO - 19 May 2010

NGC1333 / SMA - Turbulent Spectrum CC2YSO - 19 May 2010Houde et al. 2010

NGC Ambipolar Diffusion Cut-off CC2YSO - 19 May 2010 Houde et al Li & Houde (2008) 1.8 mpc in M17 using HCO + /HCN

Future Prospects CC2YSO - 19 May 2010

Summary Angular dispersion function allows the separation of the turbulent and ordered components of the magnetic field without assuming any model for the latter. We can also account for the signal integration process along the line of sight and across the telescope beam. Determination of turbulent correlation length, number of turbulent cells in the beam  improved magnetic field strength estimates from the CF equation. With high resolution data  determination of the magnetized turbulent power spectrum! But we need even higher resolution (ALMA) and “larger” single-dish observatories (SOFIA and CCAT). CC2YSO - 19 May 2010

Merci! CC2YSO - 19 May 2010

OMC-1 with SMA at 850 µm E-vectors beam: 3.1”x 2.0” sampling: 0.25” CC2YSO - 19 May 2010

OMC-1 / SMA - Results CC2YSO - 19 May 2010

OMC-1 / SMA - Turbulent Spectrum CC2YSO - 19 May 2010

IRAS with SMA at 850 µm B-vectors beam: 3”x 2” sampling: 0.25” CC2YSO - 19 May 2010

IRAS / SMA - Results CC2YSO - 19 May 2010

IRAS / SMA - Turbulent Spectrum CC2YSO - 19 May 2010

IRAS Ambipolar Diffusion Cut-off CC2YSO - 19 May 2010