On the Nature of Star Forming Regions as a function of Galactic - - PowerPoint PPT Presentation

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On the Nature of Star Forming Regions as a function of Galactic - - PowerPoint PPT Presentation

May 03, 2023 339 likes •547 views

On the Nature of Star Forming Regions as a function of Galactic Dynamics Florent Renaud CEA-Saclay, Paris with F. Bournaud, E. Emsellem, B. Elmegreen, R. Teyssier, J. Alves, D. Chapon, F. Combes, A. Dekel, J. Gabor, P. Hennebelle, K. Kraljic

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Florent Renaud

On the Nature of Star Forming Regions as a function of Galactic Dynamics

CEA-Saclay, Paris

with F. Bournaud, E. Emsellem, B. Elmegreen, R. Teyssier, J. Alves,

  • D. Chapon, F. Combes, A. Dekel, J. Gabor, P. Hennebelle, K. Kraljic
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widely inspired by Daddi+ (2010b) (see also Genzel+ 2010) Kennicutt+(1998) Kennicutt+(2007) Bigiel+(2008) Tacconi+(2010) ; Daddi+(2010a) Kennicutt+(1998) Bouché+(2007) ; Bothwell+(2009) Bolatto+(2011) SMC high-z disks local spirals low-z starbursting mergers high-z starbursting mergers

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SMC high-z disks local spirals low-z starbursting mergers high-z starbursting mergers Renaud, Kraljic & Bournaud (2012)

Dependence on à turbulence (Mach number) à metallicity (cooling)

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redshift galaxy-galaxy interaction(s) (intrinsic) galaxy evolution galaxy structure

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Resolving star forming cores, in the galactic context

M31

cores: 0.01 pc galaxy: 100 kpc 7 orders of magnitude in space AND time How: self-consistent simulation of a galaxy, at subparsec resolution

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h t t p : / / i r f u . c e a . f r / P i s p / f l o r e n t . r e n a u d / m w . p h p 200 billion pixels

(183,251,238,912 to be exact!) ¡

maps

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resolution: 0.05 pc

Renaud et al. (arXiv:1307.5639)

stars gas 60M particles (DM + stars) RAMSES

Teyssier et al. (2002) Dubois & Teyssier (2008) Teyssier et al. (2013) Renaud et al. (2013)

star formation + feedback (HII + radiation pressure + SNe)

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740 Myr 748 Myr 755 Myr R θ Fragmenting spiral ¡ Formation of beads on a string within 10-15 Myr ¡

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NGC 628 Foyle et al. (2013) M83 Gusev & Efremov (2013) see also Elmegreen & Elmegreen (1983)

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σ? = σgas ≈ 10 km/s

when stars form: ¡

v2

rotation ≈ v2 circular − σ2 (relaxation...) ¡ (dissipation...) ¡ 10 Myr later: ¡

σ? ≈ 15 km/s σgas ≈ 9 km/s

Binney & Tremaine (1987, p326)

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Decoupling star-gas ¡ SN progenitors lag behind the cloud ¡ Asymmetric, offset feedback ¡ Inefficient at destroying clouds ¡

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Surface density Velocity (horizontal) M 51 spurs in formation 5 Myr older spurs Kelvin-Helmholz instabilities On the leading side of spirals Exist in 3D models (without MHD)

Chakrabarti et al. (2003) Wada & Koda (2004) Kim & Ostriker (2006) Shetty & Ostriker (2006) Dobbs & Bonnell (2006)

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Schinnerer et al. (2013)

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young

  • ld
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small pitch angle large pitch angle strong velocity gradient: KH instabilities weak velocity gradient: no KH instabilities

Renaud et al. (2013b) see Wada & Koda (2004) for an analytical approach

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Shear Cloud-cloud collisions Tidal features SF enhancement in complexes ¡

Tasker & Tan (2009) Fukui et al. (2013)

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1 kpc

Emsellem, Renaud et al. (in prep.)

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Beads on a string = clustered star formation Assymetric drift =

  • ffset, less efficient feedback

Spurs from KH instabilities = SF on leading side of spirals Galactic dynamics matter to star formation! Several environments for SF found in the same disk Disk dynamics (shear, pitch angle etc) set the conditions for star formation Down to what scale?