From protostellar cores to disk galaxies - Zurich - 09/2007 S.Walch, A.Burkert, T.Naab Munich...
-
Upload
jennifer-ottaway -
Category
Documents
-
view
218 -
download
1
Transcript of From protostellar cores to disk galaxies - Zurich - 09/2007 S.Walch, A.Burkert, T.Naab Munich...
![Page 1: From protostellar cores to disk galaxies - Zurich - 09/2007 S.Walch, A.Burkert, T.Naab Munich University Observatory S.Walch, A.Burkert, T.Naab Munich.](https://reader035.fdocuments.net/reader035/viewer/2022062417/5517a33955034645368b5b9d/html5/thumbnails/1.jpg)
From protostellar cores to disk galaxies - Zurich - 09/2007
S.Walch, A.Burkert, T.NaabS.Walch, A.Burkert, T.Naab
Munich University Munich University ObservatoryObservatory
S.Walch, A.Burkert, T.NaabS.Walch, A.Burkert, T.Naab
Munich University Munich University ObservatoryObservatory
Formation & evolution Formation & evolution of protostellar disksof protostellar disksaround low-mass starsaround low-mass stars
Formation & evolution Formation & evolution of protostellar disksof protostellar disksaround low-mass starsaround low-mass stars
![Page 2: From protostellar cores to disk galaxies - Zurich - 09/2007 S.Walch, A.Burkert, T.Naab Munich University Observatory S.Walch, A.Burkert, T.Naab Munich.](https://reader035.fdocuments.net/reader035/viewer/2022062417/5517a33955034645368b5b9d/html5/thumbnails/2.jpg)
From protostellar cores to disk galaxies - Zurich - 09/2007
Density: Bonnor-Ebert SphereCentral density: max =10-18 g/cm³
Temperature: T = 20K
Cut-off radius: BE= 6.9 0.1pc
Total mass of the sphere: MBE 5.5Msun
EOS: Adiabatic ( =1.4 for H2)+ Molecular line cooling: Neufeld et al., (1995): Mostly H2, CO, H2O, HCl, O2
Initial Conditions
= Etherm/Epot
0.1
![Page 3: From protostellar cores to disk galaxies - Zurich - 09/2007 S.Walch, A.Burkert, T.Naab Munich University Observatory S.Walch, A.Burkert, T.Naab Munich.](https://reader035.fdocuments.net/reader035/viewer/2022062417/5517a33955034645368b5b9d/html5/thumbnails/3.jpg)
From protostellar cores to disk galaxies - Zurich - 09/2007
Velocity & Angular Momentum:Thermal line-widthsVelocity gradient maps (e.g. Caselli
2002)
Initial Conditions
![Page 4: From protostellar cores to disk galaxies - Zurich - 09/2007 S.Walch, A.Burkert, T.Naab Munich University Observatory S.Walch, A.Burkert, T.Naab Munich.](https://reader035.fdocuments.net/reader035/viewer/2022062417/5517a33955034645368b5b9d/html5/thumbnails/4.jpg)
From protostellar cores to disk galaxies - Zurich - 09/2007
Velocity & Angular Momentum: Caused by:
Overall core rotation?
From galactic differential rotation; clump-clump collisions?Sub-/Transonic Turbulence?(Burkert & Bodenheimer 2000)
Random Gaussian Velocity Fields; P(k) kn , n=-3..-4 Can turbulence account for net rotation?Reproduces Line-Width - Size relationship (Larson 1981):
() q (n=-3-2q), q=0.25..0.75 (e.g. Fuller & Myers 1992)
(Kolmogorov: q=0.33, n= - 11/3)Reproduces projected rotational properties of cores
Initial Conditions
= Erot/Epot
0.01
![Page 5: From protostellar cores to disk galaxies - Zurich - 09/2007 S.Walch, A.Burkert, T.Naab Munich University Observatory S.Walch, A.Burkert, T.Naab Munich.](https://reader035.fdocuments.net/reader035/viewer/2022062417/5517a33955034645368b5b9d/html5/thumbnails/5.jpg)
From protostellar cores to disk galaxies - Zurich - 09/2007
Numerical IssuesVINE-Code: VINE-Code: (Wetzstein et al.)
MPI-Parallel N-Body + SPH Code
Resolution:Resolution:430 000 Particles
-> Particle Mass: 1.28·10-5M
-> Min. resolvable Jeans Mass: 1.28·10-3M
-> Switch in EOS => Mjeans always resolved!
Minimum Smoothing Length:Minimum Smoothing Length: hmin = 2AU
VINE-Code: VINE-Code: (Wetzstein et al.)
MPI-Parallel N-Body + SPH Code
Resolution:Resolution:430 000 Particles
-> Particle Mass: 1.28·10-5M
-> Min. resolvable Jeans Mass: 1.28·10-3M
-> Switch in EOS => Mjeans always resolved!
Minimum Smoothing Length:Minimum Smoothing Length: hmin = 2AU
Boundary Conditions: Periodic in Hydro Isolated in Gravity
![Page 6: From protostellar cores to disk galaxies - Zurich - 09/2007 S.Walch, A.Burkert, T.Naab Munich University Observatory S.Walch, A.Burkert, T.Naab Munich.](https://reader035.fdocuments.net/reader035/viewer/2022062417/5517a33955034645368b5b9d/html5/thumbnails/6.jpg)
From protostellar cores to disk galaxies - Zurich - 09/2007
Rigid rotation vs. turbulence
Turbulent core: j=2.7•1021 cm2s-1
Rigidly rotating core: =6•10-14 s-1 => j=1021 cm2s-1
![Page 7: From protostellar cores to disk galaxies - Zurich - 09/2007 S.Walch, A.Burkert, T.Naab Munich University Observatory S.Walch, A.Burkert, T.Naab Munich.](https://reader035.fdocuments.net/reader035/viewer/2022062417/5517a33955034645368b5b9d/html5/thumbnails/7.jpg)
From protostellar cores to disk galaxies - Zurich - 09/2007
Rigid rotation vs. turbulence
Zur Anzeige wird der QuickTime™ Dekompressor „YUV420 codec“
benötigt.
Zur Anzeige wird der QuickTime™ Dekompressor „YUV420 codec“
benötigt.
![Page 8: From protostellar cores to disk galaxies - Zurich - 09/2007 S.Walch, A.Burkert, T.Naab Munich University Observatory S.Walch, A.Burkert, T.Naab Munich.](https://reader035.fdocuments.net/reader035/viewer/2022062417/5517a33955034645368b5b9d/html5/thumbnails/8.jpg)
From protostellar cores to disk galaxies - Zurich - 09/2007
Rigid rotation vs. turbulence
![Page 9: From protostellar cores to disk galaxies - Zurich - 09/2007 S.Walch, A.Burkert, T.Naab Munich University Observatory S.Walch, A.Burkert, T.Naab Munich.](https://reader035.fdocuments.net/reader035/viewer/2022062417/5517a33955034645368b5b9d/html5/thumbnails/9.jpg)
From protostellar cores to disk galaxies - Zurich - 09/2007
Global core structure
z
0.1 pc across
![Page 10: From protostellar cores to disk galaxies - Zurich - 09/2007 S.Walch, A.Burkert, T.Naab Munich University Observatory S.Walch, A.Burkert, T.Naab Munich.](https://reader035.fdocuments.net/reader035/viewer/2022062417/5517a33955034645368b5b9d/html5/thumbnails/10.jpg)
From protostellar cores to disk galaxies - Zurich - 09/2007
Global core structure
104 AU across
z
![Page 11: From protostellar cores to disk galaxies - Zurich - 09/2007 S.Walch, A.Burkert, T.Naab Munich University Observatory S.Walch, A.Burkert, T.Naab Munich.](https://reader035.fdocuments.net/reader035/viewer/2022062417/5517a33955034645368b5b9d/html5/thumbnails/11.jpg)
From protostellar cores to disk galaxies - Zurich - 09/2007
Global core structure
2000 AU across
z
![Page 12: From protostellar cores to disk galaxies - Zurich - 09/2007 S.Walch, A.Burkert, T.Naab Munich University Observatory S.Walch, A.Burkert, T.Naab Munich.](https://reader035.fdocuments.net/reader035/viewer/2022062417/5517a33955034645368b5b9d/html5/thumbnails/12.jpg)
From protostellar cores to disk galaxies - Zurich - 09/2007
Origin of spiral arms?
![Page 13: From protostellar cores to disk galaxies - Zurich - 09/2007 S.Walch, A.Burkert, T.Naab Munich University Observatory S.Walch, A.Burkert, T.Naab Munich.](https://reader035.fdocuments.net/reader035/viewer/2022062417/5517a33955034645368b5b9d/html5/thumbnails/13.jpg)
From protostellar cores to disk galaxies - Zurich - 09/2007
SBR: Nice big disks, which grow constantly in size & mass
Filamentary & elongated (prolate) global core structure
Disk sizes are in agreement with later observations Average Accretion Rates in “Class 0“ stage:
Solid Body: 6.4 ·10-5 Msun/yr Hb17: 2.3 ·10-5 Msun/yr
With turbulence, irregular infall, accretion is dynamically very complicated: Disks are warped and tilted
No Fragmentation: Global gravitational torques cause spiral structure
Wide binaries may form due to turbulence in the core - even in Bonnor-Ebert sphere!
Conclusions
![Page 14: From protostellar cores to disk galaxies - Zurich - 09/2007 S.Walch, A.Burkert, T.Naab Munich University Observatory S.Walch, A.Burkert, T.Naab Munich.](https://reader035.fdocuments.net/reader035/viewer/2022062417/5517a33955034645368b5b9d/html5/thumbnails/14.jpg)
From protostellar cores to disk galaxies - Zurich - 09/2007
Predict observablesPredict observables (ALMA, SCUBA, Spitzer)Bridge gap !
When can we first observe young protostars? Parameter study:Parameter study: Fragmentation & Characteristic disk parameters
-> Brown Dwarf formation? In core / in disk?-> Gas giant planet formation? Do disks become massive enough? Toomre unstable?
Outlook