a reply to palla & stahler 2000: an origin of accelerating ... · of accelerating star...
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A Reply to Palla & Stahler 2000: An Origin of Accelerating Star Formation
Shu-ichiro Inutsuka (Nagoya University)
Star Formation in Space and Time (June 5–9, 2017)
June 7, 2017 Instituto degli Innocenti, Firenze, Italy
Main Collaborators:Tsuyoshi Inoue, Doris Arzoumanian, Masato Kobayashi, Masanobu Kunitomo (Nagoya Univ)Kazunari Iwasaki, Kengo Tomida (Osaka Univ)Takashi Hosokawa (Kyoto Univ)Philippe André (CEA, Saclay)
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Star Formation in Space and Time (June 5–9, 2017)
June 7, 2017 Instituto degli Innocenti, Firenze, Italy
THE ASTROPHYSICAL JOURNAL, 540: 255-270, 2000 September 1©2000. The American Astronomical Society. All rights reserved. Printed in U.S.A.
ACCELERATING STAR FORMATION IN CLUSTERS AND ASSOCIATIONSFRANCESCO PALLA AND STEVEN W. STAHLER
Received 1999 November 29; accepted 2000 April 7
Age t (Myr)
Num
ber
Section 4. DISCUSSION
“The present study therefore reinforces our view that both the production and collapse of dense cores occur in response to global evolution of the parent cloud.” “What is the nature of this evolution?”
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Formation of Molecular Clouds
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Radiative Equilibrium for a given density
Warm Medium
Cold Neutral Medium
Solid: NH=1019cm-2, Dashed: 1020cm-2
e.g., Wolfire et al. 1995, Koyama & SI 2000
ρ ×102
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Shock Propagation into WNM
Hot Medium
Color: Density
12
5432
Koyama & Inutsuka (2002) ApJ 564, L97
Ambient ISM
WNM
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Summary of TI-Driven TurbulenceKoyama & SI (2002): 2D/3D Calculation of Propagation of Shock Wave into WNM via Thermal Instability fragmentation of cold layer into cold clumps with long-sustained supersonic velocity dispersion (~ km/s)
1D: Shock ⇒ Eth ⇒ Erad
2D&3D: Shock ⇒ Eth ⇒ Erad + Ekin
δv ~ a few km/s < CS,WNM =10km/s104K due to Lyα line: Universality!
TCNM ~102K C+158µm (~92K)Hennebelle & Audit (2007):
Turbulence Spectrum ~ Kolmogorov
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20 p
c
10,0002Hennebelle & Audit 07
Heitsch+ 20062D, 40962
Vazquez-Semadeni et al. 2011
Magnetic Field?
c.f. Kritsuk & Norman 1999
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Cloud Formationin Magnetized Medium
Can compression of magnetizedWNM create molecular clouds?
Ref. Inoue & SI (2008) ApJ 687, 303Inoue & SI (2009) ApJ 704, 161Inoue & SI (2012) ApJ 759, 35
SI, Inoue, Iwasaki, Hosokawa 2015 A&A 580, A49
Two-Fluid Resistive MHD + Cooling/Heating + Thermal Conduction + Chemistry (H2, CO,…)
Ambipolardiffusion included
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Colliding WNM with B0=3µG
v=10km/s(a) 15deg
<δB2>init = B02
(a) 40 deg
<δB2>init = 4B02
2-Fluid MHD Simulation (AD included)Inoue & SI (2008) ApJ 687, 303
10km/s 10km/s
10km/s10km/s
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Compression of Magnetized WNMCan direct compression of magnetized WNM
create molecular clouds? Not at once!Inoue & SI (2008) ApJ 687, 303Inoue & SI (2009) ApJ 704, 161
Essentially same result byHeitsch+2009; Körtgen & Banerjee 2015; Valdivia+2016; (Iwasaki+2017 in prep)
We need multiple episodes of compression.Timescale of Molecular Cloud Formation ~ a few 107yrNext Question: What happens for further compressions?
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Black Lines: Magnetic Field Lines
Further Compress. of Mole. Clouds
Self-Gravity Included, SI, Inoue, Iwasaki, & Hosokawa 2015
Further Compression of Molecular Cloud
Magnetized Massive Filaments& Striations
c.f. obs. by Soler, Pillai, Arzoumanian, Fissel, etc.
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Highlight of Herschel Result (André+2010)
Self-Gravity Essential in Filaments
2Cs2/G
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SI & Miyama 1997
Mass Function of Cores in a FilamentInutsuka 2001, ApJ 559, L149
Line-Mass Fluctuation of FilamentsInitial Power Spectrum
P(k) ∝ k –1.5
Mass FunctiondN/dM∝M −2.5
Observation of Both Perturbation Spectrum and Mass Function
Clear and Direct Test!SI & Miyama 1997
P (k) ∝ k -1.5
t/tff = 0 (dotted) , 2, 4, 6, 8, 10 (solid)
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“A possible link between the power spectrum of interstellar filaments and the origin of the
prestellar core mass function”Roy, André, Arzoumanian et al. (2015) A&A 584, A111
δ ...Gaussian
P (k)∝ k n
n= −1.6±0.3
Supporting Inutsuka 2001; Li, Hennebelle & Chabrier 2017
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Filament ParadigmCompletely Successful?!
Other Modes of Star Formation?
Cloud Collision (Fukui, Tan, Dobbs,...)Collect & Collapse (Elmegreen-Lada, Whitworth,
Palouš, Deharveng, Zavagno,…)
?
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Toward Global Pictureof Cloud Formation
tform = a few107yr
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Network of Expanding Shells
Long (>10Myr) Exposure Picture!Each bubble disappears quickly (<Myr).
Multiple Episodes of Compression Formation of Magnetized Molecular Clouds
SI+2015; cf. Elmegreen 2007
GMC Collision
Dense HI Shell
MolecularCloud
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Velocity Dispersion of Clouds
Shell Expansion Velocities ~ 101 km/s
Multiple Episodes of Compression Formation of Magnetized Molecular Clouds
Stark & Brand 1989
Cloud-to-Cloud Velocity Dispersion
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GMC Collision
Dense HI Shell
MolecularCloud
Network of Expanding Shells
Each Bubble Visible Only for Short Time (~1Myr)!δv of Clouds ~ Cloud-Cloud Col. Velocity ~ 10km/s
Multiple Episodes of Compression Formation of Magnetized Molecular Clouds
Fukui+2012
Peretto+2013Inoue & Fukui 2013
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Star Formation Efficiency in Dense GasHerschel Observation (e.g., Andre+2014, Könyves+2015)
Mcore / Mfilament < 15%Star Formation Efficiency in Dense Core: εcore
εcore ~ 33% (ex. Machida+)
Star Formation Efficiency in Dense Gas: εdense gas
εdense gas= Mcore / Mfilament × εcore ~ 5%Consumption Timescale of Dense Gas: tdense gas
tdense gas−1 = (106 yr)−1 × εdense gas = (20Myr)−1
tdense gas ~ 20Myr (eg. Lada+2010, Andre+2014)
~
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Schmidt-Kennicutt Law of SF
• Column Density: Σgas [M/pc2]• SF Rate: ΣSFR [M /kpc2 yr]• Timescale: Μ /(SFR) ~ 20MyrSee also Gao & Solomon 2004; Wu+2005; Bigiel et al. 2008,2010,2011, Shimajiri+2017
Σgas [M/pc2]
Star Formation Rate
Kennicutt 1998
Lada+2010,2012,2013
High Density Tracer
Timescale: Σgas / ΣSFR ~ Gyr
Σ SFR
[M
/kpc
2yr
]
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How Many Generations of Filaments?Star Formation Efficiency in Dense Gas: εdense gas
εdense gas= Mcore / Mfilament × εcore ~ 5%
Typical Mass of Star Forming Filaments: L ~ 3pc, MLine ~2Cs2/G
M = MLine × L ~ 60Msun
Total Mass of Stars Created in a Filament: 60Msun × εdense gas ~ 3Msun
Total Mass of YSOs: M*total# of Filaments to Form Stars = M*total/3Msun
Multiple Generations of Filaments Needed!
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Natural Acceleration of Star Formation
Molecular Cloud GrowthMass Increase in
Supercritical Filaments Accelerated SF
Also in Lupus, Chamaeleon, ρ Ophiuchi, Upper Scorpius,
IC 348, and NGC 2264See also Poster 52 by Kunitomo
Palla & Stahler 2000
Age t (Myr)
Num
ber
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My Last Exchange with Francesco PallaDear Francesco and Steven,
I would like to introduce our recent paper on a scenario of Galactic star formation. This is based on our time-consuming (~15yrs) work on the formation of molecular clouds and their destruction, and accepted forAstronomy & Astrophysics.I think we found a clue in understanding “Accelerating Star Formation” you found in the year I started this line of work. I hope you would have some interest. Thank you.
With my best regards, Shu-ichiro Inutsuka
Dear Shu-Ichiro,
good to hear form you and many thanks for your paper. I will read it with great pleasure!It also comes at the right time since in my course I’m now teaching the formation and evolution of molecular clouds. So, in addition to my personal interest, it will provide me with important material for the students.
All the best, Francesco
18 May 2015
19 May 2015
27 Jan 2016, RIP
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Summary• Fragmentation of Filaments Core Mass Function• Bubble-Dominated Formation of Molecular CloudsUnified Picture of Star Formationδvcloud-cloud ~ 101km/sAccelerated Star FormationSchmidt-Kennicutt LawStar Formation Efficiency: εSF ~ 10-2
Slope of Cloud Mass Func =1+𝑇𝑇form/𝑇𝑇dis ~1.7SI, Inoue, Iwasaki, & Hosokawa 2015, A&A 580, A49
Kobayashi, SI, Kobayashi, & Hasegawa 2017, ApJ 836, 175Poster 12