Magnetized Molecular Cloud Formation and DynamicsMagnetized Molecular Cloud Formation and Dynamics...
Transcript of Magnetized Molecular Cloud Formation and DynamicsMagnetized Molecular Cloud Formation and Dynamics...
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Magnetized Molecular Cloud Formation and Dynamics
Mordecai-Mark Mac Low Juan C. Ibáñez-Mejía
Joshua E. Wall Stephen McMillan Ralf S. Klessen
ESA/Herschel/PACS, SPIRE/Gould Belt survey Key Programme/Palmeirim et al. 2013
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Ballesteros-Paredes+ 11
CO CS
Larson’s size-velocity relation has been argued to result from turbulent driving.
But, it only applies to a narrow range of column densities.
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Ballesteros-Paredes+ 11
1/2 ]
normalization of Larson’s linewidth-size relation depends on column density
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Modeling the turbulent ISM with FlashModel ingredients
20 k
pc
1 kpc
Gas self-gravity
Included at late times
Heating and coolingG0
T0 T1>T0
Ha
C+
C+
Ha
Ha
CO
CO
C+
C+
gstatic [pc / Myr2]
02.5
1.0
2.0
-2.5
-1.0
-2.0
random supernova & superbubbles
SN
SB
Magnetic fields
Ibáñez-Mejía + 16
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Modeling the turbulent ISM with FlashMorphology
Ibáñez-Mejía et al. 2016
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Modeling the turbulent ISM with FlashMorphology
Ibáñez-Mejía et al. 2016
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Ibáñez-Mejía + 16
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Ibáñez-Mejía + 16
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Zooming-in to collapsing cloudsModel
1016
1017
1018
1019
1020
1021
Col
umn
dens
ity [
cm-2]
Δx = 0.06 pc
Δx = 0.12 pc Δx = 0.06 pc
Ibáñez-Mejía et al. 2017, in press, ArXiv:1705.01779
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Evolution and collapse of a dense cloudResults
Ibáñez-Mejía et al. 2017, in press, ArXiv:1705.01779
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Evolution and collapse of a dense cloudResults
Ibáñez-Mejía et al. 2017, in press, ArXiv:1705.01779
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t = 0
Resolution study of energy: acceptable 25% variation
Ibáñez-Mejía et al. 2017, in press, ArXiv:1705.01779
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1 pc
10 pc
100 pc
Ibáñez-Mejía, thesis & in prep +18M3e3
dx = 0.06 pc
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Field angle varies Morphology
Dec
R. A.
20.7
21.6
22.5log10 (NH / cm -2)
b) c)
b) c)
Palmeirim et al. 2013, Narayanan et al., 2008, Ade et al. 2016. Planck XXXIII 2016Ibáñez-Mejía et al. 2018, in prep;
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Field angle varies Morphology
Dec
R. A.
20.7
21.6
22.5log10 (NH / cm -2)
b) c)
b) c)
Ibáñez-Mejía et al. 2018, in prep;
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blue data points from Crutcher +10
3
4 5
2
-1
10Ibáñez-Mejía, thesis, in prep +18
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Dense clouds collapse quickly while accreting.Results
Ibáñez-Mejía et al. 2017, in press, ArXiv:1705.01779
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Gravitational energy dominates cloud evolution.Results
Ibáñez-Mejía et al. 2017, in press, ArXiv:1705.01779
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Contraction dominates over accretion for KE.Results
Ibáñez-Mejía et al. 2017, in press, ArXiv:1705.01779
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Trans-Alfvénic envelope, super-Alfvénic coreResults
Cloud
Envelope
Ibáñez-Mejía et al. 2018, in prep
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Histogram of relative orientations (HRO) between magnetic field and density gradient shows moderate alignment in envelope, none in core with n > 103 cm-3.
Ibáñez-Mejía, thesis & in prep +18
Soler+16
Crutcher+transitiondensity
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Alfvénic Mach number inside and around a cloudResults
• Nearby SN feedback maintains the diffuse ISM super-Alfvénic.
• Cloud envelopes are mostly trans-Alfvénic to mildly super-Alfvénic.
• gravitational contraction drives fast, super-Alfvénic, motions inside the cloud
Cloud
Envelope
MA <1
MA ≈1
MA >1
Ibáñez-Mejía et al. 2018, in prep
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Astrophysical MUlti-Purpose Software Environment
Wall, M-MML, McMillan, Klessen, Portegies-Zwart, in prep
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Wall, M-MML, McMillan, Klessen, Portegies-Zwart, in prep
2400 AU resolution
104 M⊙
test cloud
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Wall, M-MML, McMillan, Klessen, Portegies-Zwart, in prep
2400 AU resolution
104 M⊙
test cloud
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Wall, M-MML, McMillan, Klessen, Portegies-Zwart, in prep
2400 AU resolution
104 M⊙
test cloud
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Wall, M-MML, McMillan, Klessen, Portegies-Zwart, in prep
2000 AU resolution
103 M⊙
test cloud
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Wall, M-MML, McMillan, Klessen, Portegies-Zwart, in prep
2000 AU resolution
103 M⊙
test cloud
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Wall, M-MML, McMillan, Klessen, Portegies-Zwart, in prep
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Wall, M-MML, McMillan, Klessen, Portegies-Zwart, in prep
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Conclusionsconclusions
• In the absence of star formation and internal feedback, gravitational contraction seems to be the main driver of non-thermal motions inside dense clouds.
• Nearby SN explosions both compress the clouds’ envelopes, increasing mass accretion rates, and erode the surface and fragment the cloud.
• Gas flows around clouds are predominantly trans-Alfvénic, so magnetic fields play an active role regulating mass accretion rates.
• Magnetic fields inside dense clouds seem unable to prevent collapse. Hierarchical gravitational contraction drives super-Alfvénic internal motions.
• HII region expansion carries the field with it, but angle of observation matters.
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