Astrophysical Gas Dynamics - Australian National University · Astrophysical Gas Dynamics -...
Transcript of Astrophysical Gas Dynamics - Australian National University · Astrophysical Gas Dynamics -...
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Christoph Federrath
Astrophysical Gas Dynamics
ASTR4012 / ASTR8002
ANU – 2nd semester 2018
Course and Tutorials: Mondays and Wednesdays 9-11
Webpage:
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Image credit: M. S. Povich
Topics:- Motivation (most of astrophysics is gas dynamics: stars, accretion discs, galaxies)- Hydrodynamical Equations (derivation, Eulerian, Lagrangian, conservation laws)- Waves and Shocks- Turbulence- Magnetohydrodynamics- Accretion and Winds
- Computational Fluid dynamics (numerical solution of hydro equations, advection)- -> get computer account at RSAA; application form on course web page
Astrophysical Gas Dynamics
Resources:Lecture notes by Ogilvie, Sormani, Bai, Zaroubi, ZingaleSijaki: https://www.ast.cam.ac.uk/students/undergrad/part_ii/lectures/fluids
Fluid Mechanics Films:http://web.mit.edu/hml/ncfmf.html
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- Need at least one student rep (by end of week 2) -> Rosie Iervasi- Student rep communicates with students and course convener- Student rep name and email address published on Wattle website- Please nominate yourself or someone else, if you are interested
Astrophysical Gas Dynamics
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Image credit: M. S. Povich
Astrophysical Gas Dynamics
- assessment based on 4 assignments in total- 4th assignment counts double as final exam- one assignment per about every 2-3 weeks- assignments published on webpage- submission via email ([email protected]) or directly to me- feedback within two weeks after submission
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The Gas Dynamics inStar Formation and Turbulence
Image Credit: ESA and the HFI Consortium, IRAS 2010
Christoph FederrathANU – 01 August 2018
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Density PDF → Star Formation Rate
Why is star formation so inefficient?
Turbulence → Density PDF
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Carina Nebula, NASA, ESA, N. Smith (University of California, Berkeley), and The Hubble Heritage Team (STScI/AURA), and NOAO/AURA/NSF
Turbulence Stars Feedback
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Clouds è Cores è Disk + Star + Jet / Outflow
The Star Formation Paradigm
Beuther 2008
Star Formation
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Jets and Outflows
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Outflow mass:
Outflow velocity:
Outflow angular momentum:
Federrath et al. 2014, ApJ 790, 128
Sink Particles as Star Formation Subgrid Model
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Jet/Outflow Feedback
Federrath et al. 2014, ApJ 790, 128Movies available: https://www.mso.anu.edu.au/~chfeder/pubs/outflow_model/outflow_model.html
Federrath – SFDE 2017
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NGC1333Image credit: Gutermuth & Porras
Star Formation – Outflow/Jet Feedback
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The role of outflow/jet feedback for star cluster formation
SGS off SGS onFederrath et al. 2014, ApJ 790, 128
Movies available: https://www.mso.anu.edu.au/~chfeder/pubs/outflow_model/outflow_model.html
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Efficiency~ 30-40%?
Alves et al. (2007); Andre et al (2010)
RESULTS:
- Outflow/Jet feedback reduces the SFR by factor ~ 2
- Outflow/Jet feedback reduces average star mass by factor ~ 3
1/3
The role of outflow/jet feedback for star cluster formation
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Why is Star Formation is so Inefficient?
Turb+Mag+Jets
Turb
Turb+Mag
Gravityonly
Movies available: http://www.mso.anu.edu.au/~chfeder/pubs/ineff_sf/ineff_sf.html
Federrath – SFDE 2017
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Federrath 2015, MNRAS 450, 4035
Star Formation is Inefficient
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Conclusions
� Jet/outflow feedback in star cluster formation:
� Supersonic, magnetized turbulence is key for star formation
- Star formation rate reduced by ~2x- Average star mass reduced by ~3x → Initial Mass Function!
- SFR from density PDF depends onvirial parameter, forcing parameter, Mach number, plasma beta
- Very good agreement between theory, simulations and observations
� Star Formation is inefficient → Only combination of Turb+Mag+Feedback gives realistic SFRs
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Astrophysical Gas Dynamics
ASTR4012 / ASTR8002
NEXT: Hydrodynamical Equations
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Astrophysical Fluid Dynamics
(Bai lecture notes)
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Derivation of Hydrodynamical Equations
- Introduction of fluid variables
- Conservation of mass, momentum, energy
- Equation of state to close the system
- Validity of the fluid approach
→ White board
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