1. Star and Planet Formation Sommer term 2007 Henrik Beuther & Sebastian Wolf 16.4 Introduction (H.B. & S.W.) 23.4 Physical processes, heating and cooling, radiation transfer (H.B.) 30.4 Gravitational collapse & early protostellar evolution I (H.B.) 07.5 Gravitational collapse & early protostellar evolution II (H.B.) 14.5 Protostellar and pre-main sequence evolution (H.B.) 21.5 Outflows and jets (H.B.) 28.5 Pfingsten (no lecture) 04.6 Clusters, the initial mass function (IMF), massive star formation (H.B.) 11.6 Protoplanetary disks: Observations + models I (S.W.) 18.6 Gas in disks, molecules, chemistry, keplerian motions (H.B.) 25.6 Protoplanetary disks: Observations + models II (S.W.) 02.7 Accretion, transport processes, local structure and stability (S.W.) 09.7 Planet formation scenarios (S.W.) 16.7 Extrasolar planets: Searching for other worlds (S.W.) 23.7 Summary and open questions (H.B. & S.W.) More Information and the current lecture files: http://www.mpia.de/homes/beuther/lecture_ss07.htmlhttp://www.mpia.de/homes/beuther/lecture_ss07.html and http://www.mpia.de/homes/swolf/vorlesung/sommer2007.htmlhttp://www.mpia.de/homes/swolf/vorlesung/sommer2007.html Emails: beuther@mpia.de, swolf@mpia.de

2. Summary last week - The “first core” contracts until temperatures are able to dissociate H 2 to H. - H-region spreads outward, T and P not high enough to maintain equilibrium, further collapse until H gets collisionally ionized. The dynamically stable protostar has formed. - Accretion luminosity. Definition of low-mass protostar can be “mass-gaining object where the luminosity is dominated by accretion”. - Structure of the protostellar envelope and effects of rotation. - Stellar structure equations: follow numerically the protostellar and then later the pre-main sequence evolution. - Convection and deuterium burning. - End of protostellar/beginning or pre-main sequence evolution --> birthline. - Pre-main sequence evolution in the Hertzsprung-Russel (HR) diagram. - Connection of HR diagram with protostellar and pre-main sequence class scheme.

3. Star Formation Paradigm

4. Discovery of outflows I Herbig 1950, 1951; Haro 1952, 1953 Initially thought to be embedded protostars but soon spectra were recognized as caused by shock waves --> jets and outflows

5. Discovery of outflows II - In the mid to late 70th, first CO non-Gaussian line wing emission detected (Kwan & Scovile 1976). - Bipolar structures, extremely energetic, often associated with HH objects Bachiller et al. 1990 Snell et al. 1980

6. HH30, a disk-outflow system

7. Outflow multiplicities in Orion Stanke et al. 2002

8. The prototypical molecular outflow HH211

9. Jet entrainment in HH211 From Hirano et al. 2006, Palau et al. 2006, Chandler & Richer 2001, Gueth et al. 1999, Shang et al. 2006 - Warmer gas closer to source - Jet like SiO emission has always larger velocities than CO at the same projected distance from the driving protostar

10. IRAS 20126+4104 Lebron et al. 2006

11. Mass vs.velocity, energy vs. velocity Lebron et al. 2006 - Mass-velocity relation exhibits broken power-law, steeper further out - Energy at high velocities of the same magnitude than at low velocities

12. Outflow/jet precession Stanke 2003 Fendt & Zinnecker 1998

13. Jet rotation in DG Tau Bacciotti et al. 2002 blue red Testi et al. 2002 Corotation of disk and jet

14. General outflow properties - Jet velocities 100-500 km/s Outflow velocities 10-50 km/s - Estimated dynamical ages between 10 3 and 10 5 years - Size between 0.1 and 1 pc - Force provided by stellar radiation too low (middle panel) --> non-radiative processes necessary! Mass vs. L Force vs. L Outflow rate vs. L Wu et al. 2004, 2005

15. Wu et al. 2004 Collimation degrees Collimation degrees (length/width) vary between 1 and 10 HH211, Gueth et al. 1999

16. Collimation and pv-structure Lee et al. 2001 HH212: consistent with jet-driving VLA0548: consistent with wind-driving - pv-structure of jet- and wind-driven models very different - Often Hubble-law observed --> increasing velocity with increasing distance from the protostar

17. Outflow entrainment models I Basically 4 outflow entrainment models are discussed in the literature: Turbulent jet entrainment model - Working surfaces at the jet boundary layer caused by Kelvin-Helmholtz instabilities form viscous mixing layer entraining molecular gas. --> The mixing layer grows with time and whole outflow gets turbulent. - Broken power-law of mass-velocity relation is reproduced, but velocity decreases with distance from source --> opposite to observations Jet-bow shock model - As jet impact on ambient gas, bow shocks are formed at head of jet. High pressure gas is ejected sideways, creating a broader bow shock entraining the ambient gas. Episodic ejection produces chains of knots and shocks. - Numerical modeling reproduce many observables, e.g. Hubble-law. Raga et al. 1993 Gueth et al. 1999

18. Jet simulations I Rosen & Smith 2004 3-dimensional hydrodynamic simulations, including H, C and O chemistry and cooling of the gas, this is a pulsed jet.

19. Jet simulations II: small precession Rosen & Smith 2004

20. Jet simulations III, large precession Rosen & Smith 2004

21. Outflow entrainment models II Wide-angle wind model - A wide-angle wind blows into ambient gas forming a thin swept-up shell. Different degrees of collimation can be explained by different density structures of the ambient gas. - Attractive models for older and low collimated outflows. Circulation model - Molecular gas is not entrained by underlying jet or wind, but it is rather infalling gas that was deflected from the central protostar in a region of high MHD pressure. - This model was proposed to explain also massive outflows because it was originally considered difficult to entrain that large amounts of gas. Maybe not necessary today anymore … Fiege & Henriksen 1996 Shu et al. 1991

22. Outflow entrainment models III Arce et al. 2002

23. Jet launching - Large consensus that outflows are likely driven by magneto- centrifugal winds from open magnetic field lines anchored on rotating circumstellar accretion disks. - Two main competing theories: disk winds X-winds - Are they launched from a very small area of the disk close to the truncation radius (X-wind), or over larger areas of the disk (disk wind)?

24. Jet-launching: Disk winds I Collapse: 6.81 x 10 4 yr 5 months later 1AU~ 1.5x10 13 cm - Infalling core pinches magnetic field. - If poloidal magnetic field component has angle larger 30˚ from vertical, centrifugal forces can launch matter- loaded wind along field lines from disk surface. - Wind transports away from 60 to 100% of disk angular momentum. Banerjee & Pudritz 2006 Recent review: Pudritz et al. 2006

25. Jet-launching: Disk winds II Banerjee & Pudritz 2006 1AU~ 1.5x10 13 cm Toroidal magnetic field t=1.3x10 5 yr t=9.66x10 5 yr - On larger scales, a strong toroidal magnetic field builds up during collapse. - At large radii (outside Alfven radius r A, the radius where kin. energy equals magn. energy) B  /B p much larger than 1 --> collimation via Lorentz-force F L ~j z B 

26. X-winds Shu et al. 2000 - The wind is launched magneto-centrifugally from the inner co-rotation radius of the accretion disk (~0.03AU)

27. Jet-launching points and angular momenta Woitas et al. 2005 r 0,in corresponds approximately to corotation radius ~ 0.03 AU - From toroidal and poloidal velocities, one infers footpoints r 0, where gas comes from --> outer r 0 for the blue and red wing are about 0.4 and 1.6 AU (lower limits) --> consistent with disk winds - About 2/3 of the disk angular momentum may be carried away by jet. Spectro-Astrometry

28. Impact on surrounding cloud - Entrain large amounts of cloud mass with high energies. - Potentially partly responsible to maintain turbulence in cloud. - Can finally disrupt the cores to stop any further accretion. - Can erode the clouds and alter their velocity structure. - May trigger collapse in neighboring cores. - Via shock interactions heat the cloud. - Alter the chemical properties.

29. Outflow chemistry Bachiller et al. 2001

30. Summary - Outflows and jets are ubiquitous and necessary phenomena in star formation. - Transport angular momentum away from protostar. - The are likely formed by magneto-centrifugal disk-winds. - Collimation is caused by Lorentz forces. - Gas entrainment can be due to various processes: turbulent entrainment, bow-shocks, wide-angle winds, circulation … - They inject significant amounts of energy in the ISM, may be important to maintain turbulence. - Disrupt at some stage their maternal clouds. - Often point back to the forming star

31. Star and Planet Formation Sommer term 2007 Henrik Beuther & Sebastian Wolf 16.4 Introduction (H.B. & S.W.) 23.4 Physical processes, heating and cooling, radiation transfer (H.B.) 30.4 Gravitational collapse & early protostellar evolution I (H.B.) 07.5 Gravitational collapse & early protostellar evolution II (H.B.) 14.5 Protostellar and pre-main sequence evolution (H.B.) 21.5 Outflows and jets (H.B.) 28.5 Pfingsten (no lecture) 04.6 Clusters, the initial mass function (IMF), massive star formation (H.B.) 11.6 Protoplanetary disks: Observations + models I (S.W.) 18.6 Gas in disks, molecules, chemistry, keplerian motions (H.B.) 25.6 Protoplanetary disks: Observations + models II (S.W.) 02.7 Accretion, transport processes, local structure and stability (S.W.) 09.7 Planet formation scenarios (S.W.) 16.7 Extrasolar planets: Searching for other worlds (S.W.) 23.7 Summary and open questions (H.B. & S.W.) More Information and the current lecture files: http://www.mpia.de/homes/beuther/lecture_ss07.htmlhttp://www.mpia.de/homes/beuther/lecture_ss07.html and http://www.mpia.de/homes/swolf/vorlesung/sommer2007.htmlhttp://www.mpia.de/homes/swolf/vorlesung/sommer2007.html Emails: beuther@mpia.de, swolf@mpia.de