1. Star and Planet Formation
1. gravitational
collapse of
molecular clouds
Vela-C molecular cloud region as observed at optical (upper panel) and far-infrared wavelengths
(with Herschel, lower panel).
This slide-show takes about 15min ...

2. Star formation in a computer box
Computer simulation by
Prof. Ian Bonnell
(St Andrews University):
hydrodynamics → SPH method
turbulence and shock waves
gravitation
star formation → sink particles

3. 2. disc evolution

4. phases of disc evolution
- triggered star formation - spherical collapse - angular momentum conservation → formation of rotating protoplanetary disc
- jets and outflows - disc flattens and spreads - planet formation - disc looses gas
- a new planetary system is born

5. 10 Myrs of disc evolution in 20sec

6. But you know what ... Honestly, we don't know most of the details
what triggers star formation?
how do discs evolve? what drives their jets and outflows?
what is the shape of the protoplanetary discs? their densities? their gas and dust temperatures?
how to form the cores of planets?
how quickly is the gas in the disc lost?
why are planets so diverse? what are the chemical preconditions for planet formation?
→ That's why we need to keep on researching!

7. Planet formation: the core-accretion model

8. micrometer sizes, and aggregates: van der Waals forces - it works!

9. mm-particles: the bouncing barrier
- mm-particles don't stick (try this yourself at the beach!)
water / organic ices as “glue”?
charged particles?
what else could it be?

10. Big particles: shattering Houston, we have a problem ...

11. Or, maybe, planets form due to gravitational instabilities?
3D hydro-simulations with self-gravity and simplified cooling
(by Prof. Ken Rice, Royal Observatory
in Edinburgh)

12. FP7 SPACE “DiscAnalysis” (large EU-funded project at St Andrews University)

13. combine UV to mm wavelengths
What parts of the disc emit at which wavelengths ?
wavelength
spectral flux
distance from star
relative height in disc

14. combine continnum and lines
CO sub-mm line map & velocity profile
wavelength
spectral flux
Doppler wavelength shift

16. DG Tau: water emission from disc!
DG Tau: a young T Tauri star with X-ray jet emission
Yet, the water emission lines are double-peaked, so they comes from the disc rather than the outflow! (L. Podio et al., Herschel/HIFI, A&A in prep.)
spectral flux
Doppler wavelength shift

17. FP7 DIANA questions
what is the disc structure, both radially and vertically?
how warm is the gas?
what is the chemical composition of the planet forming gas?
what are the properties (size, opacities, ...) of the dust particles?
Does the gas structure differ from the dust structure? do dust grains settle?
role of viscous heating?

18. protoplanetary discs: thick or thin?

19. Transitional discs: T Cha

20. Debis discs: Formalhaut

21. Star and Planet Formation
Thank you for your attention!