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Small scale dissipative
structures of the diffuse ISM
I– CO diagnostics
P. Hily-Blant . . . . . . . IRAM, Grenoble, France
E. Falgarone. . . . . . . . LERMA/ENS, Paris, France
J. Pety . . . . . . . . . . . . IRAM, Grenoble, France
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Diffuse molecular gas
• low extinction : AV ≤ 1mag
• radiation field : interstellar mean field
• magnetized : B ≈ 1 − 30µG
• tracer : mostly 12CO(1 − 0), generally assumed optically thick
• turbulent : linewidths ≈ 10cs
• structured
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• IRIS dataMiville-Deschenes & Lagache
ApJS 2005
• crosses : YSO from IRAS faint sources
catalog log10(I12/I25) < −0.4 I60 < I100
• circles : Lynds objects• diffuse gas : I < 7MJy/sr
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Aims and method
−→ structured at which scales ?−→ seeds of star forming structures ?
• observe large quiescent regions : cover large scales high angular resolutions high sensitivity
• statistical analysis of the velocity field high spectral resolutions large number of spectra
• correlation density and velocity fieldsgood tracers of velocity field and mass :13CO, 12CO
• a good telescope : IRAM-30m (knowm beam pat-tern)
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Morphology : integrated intensity
8000 spectra, δx = 10′′ = 0.0075 pc, δv = 0.05km s−1
IRAM-30m
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13CO(1 − 0) : dense 12CO(1 − 0) : tenuous
Filaments : ∅ ≈ 0.03 pc ≈ 6000 AU
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12CO(1−0) line wings
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Physical conditions : LVG
• 13CO filaments : 12CO and 13CO(1−0), (2−1) N(13CO)/∆v = 2 × 1015cm−2 (km s−1)−1
nH2 ≈ 1 − 2 × 103cm−3, Tkin = 8 − 9 K
• thin-12CO filaments : 12CO(1 − 0), (2 − 1) τ(1−0) ≤ 0.6 N(12CO)/∆v = 3 × 1015cm−2 (km s−1)−1
nH2 ≈ 8 − 1 × 102cm−3, Tkin = 20 − 400 K
100
1000
1000
10
Tkin [K]
100
thin−12CO filaments
13CO filaments
n [cm−3]
?
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Magnetic fields
Morphology : spatial coherence
thin-12CO filaments
Polarization angle ofBlos :
P.A. = 110 ± 18
13CO filaments
Orientation of filaments is not random : role of ~B ?
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What generates non-random structure
in molecular clouds ?
Possibly turbulence and its fundamental property ofintermittency :
• at a given small scale l, rare and large local excur-sions of the velocity create timescales much shor-ter than the corresponding turnover timeτl ∼ l/vl ∼ l2/3
• these large excursions are rare but significantlymore numerous than in a Gaussian distribution
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Tracers of intermittency
• Incompressible turbulence non-Gaussian distributions of velocity incre-
ments, shear, vorticity,...
the smaller the lag, the larger the devia-
tion from Gaussian
coherent intense vortices, seen in the laboratory
• Compressible turbulence Existence of shocks : same statistical properties
as small scale vortices (Pety & Falgarone 2000)
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Pety & Falgarone 2000
Shocks versus intense vortices
Simulations of supersonic turbulence
(Porter, Pouquet Woodward, 1992)5123, decaying, rms Mach ∼ 1
• full cube (left)• shocks (center)• vortices (right)
⊲ both have non Gaussian statistics⊲ fv = 3 × 10−2 but fS ∼ 1
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Is gas vorticity accessible to observations ?
Subset of largest line Centroid Velocity increments (CVIs)Subset of largest 〈Ωsky〉los
Lis et al 1996
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Velocity shear statistics
Hily-Blant et al 2006
Lag : 18 pixelsLag : 3 pixels
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The regions of largest velocity shear
Hily-Blant et al 2006
Extrema of CVI
• are not correlated with 12CO or 13CO integrated emission :
pure velocity structures
• are associated with the thin-12CO filaments
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The regions of largest velocity shear
– Small scales –
IRAM-PdB
0.015 pc
0.4 pc
IRAM-30m
Hily-Blant et al 2006
Extrema of CVI
• contain structures at sizes down to 1000 AU
• large velocity shears at 1000 AU scale :
≈ 1km s−1/1000AU = 200km s−1 pc−1
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The regions of largest velocity shear : large scales
0.015 pc
IRAM PdB
IRAM 30m
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Conclusions
⊲ Diffuse molecular gas is structured in space andvelocity
⊲ Optically thin 12CO is not distributed uniformly,but organized into filaments
⊲ These filaments are not randomly distributed, butfollow the orientation of magnetic fields
⊲ The molecular gas velocity field is intermittent
⊲ Dissipative structures of turbulence may have beenmapped for the first time : warm and tenuous12CO filaments
‡ Cold and dense 13CO filaments may proceed fromdissipation that take place into 12CO filaments
‡ These dissipative structures would provide the gaswith a heating source, independant of photodisso-ciation
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Model vs observations
MHD numerical simulations :
Padoan et al 1998
⊲ dynamical role of magnetic
fields
⊲ multifluid approach
Position-velocity cuts
Vlsr
Position
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Morphology : channel maps13CO(1 − 0) 12CO(1 − 0)
Far 12CO(1 − 0) wings : T12/T13 ≥ 35
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Dynamics into filamentary clouds
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