Micro-Turbulence in Emission and Absorption in AGN. Steve Kraemer (Catholic Univ. of America). Via collaborations with: Mike Crenshaw (GSU), Mark Bottorff (Southwestern), Jane Turner (UMBC), Lance Miller (Oxford). Is Micro-Turbulence Present?.
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Steve Kraemer (Catholic Univ. of America)
Via collaborations with:
Mike Crenshaw (GSU), Mark Bottorff (Southwestern), Jane Turner (UMBC), Lance Miller (Oxford)
Why not in AGN?
convective acceleration: time independent acceleration of fluid w.r.t space
non-linear advection operator → distortion of velocity field
Q = ηνρ (vturb 3 /D) ergs cm-3 s-1
(vturb equivalent to b or 1/1.665 FWHM)
NV 1240, affected by photo-excitation + heating, [NeV] 3426 bossted by heating.
Ratios of resonance to forbidden lines in He-like triplets can indicate temperature and density. High r/f ratios: collisionally excited gas (Ogle et al. 2000); Photo-excitation (Sako et al. 2000; Kinkhabwala et al. 2002)/
But photo-excitation depends strongly on vturb
Sim of OVII triplet, courtesy of R. Porter.
Cloudy models, (logU=0), showing dependence of r/f ratio on vturb and column density.
Most readily answered using high-res UV spectra of Type 1 Seyferts.
STIS spectra of NGC 5548, showing multiple kinematic components in HI, NV, and CIV. Note the difference in the profiles.
Slope of Nh to FWHM is ~ 1.5. For Kolmogorov cascade, slope is unity. Note: slope is flatter for the lower envelope. Combination of turbulence and superposition?
Two cases, logU=-1.5, logNh=20.5
FWHM = 1000 km/s at face; no decay. Profile difference dominated by differences in ionic columns and oscillator strengths.
FWHM = 1000 km/s at face; exponential decay. Local value of vturb has strong effect.