Canterbury 01.09.2014 The problem of star formation is not how to make stars. The problem of star...
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Transcript of Canterbury 01.09.2014 The problem of star formation is not how to make stars. The problem of star...
Canterbury 04/11/23
The problem of star formation is not how to make stars.
The problem of star formation is how not to make stars.
Canterbury 04/11/23
The Physics of
Star Formation
Dr Dirk Froebrich
University of Kent
Canterbury 04/11/23
- How do we know stars are forming?
- Where do stars form?
- Properties of young stars
- Temperature & Turbulence vs. Gravity
- Collapse, Discs and Jets
Content
Canterbury 04/11/23
- How do we know stars are forming?
- Where do stars form?
- Properties of young stars
- Temperature & Turbulence vs. Gravity
- Collapse, Discs and Jets
Content
Canterbury 04/11/23
Inside Stars...
Massive stars are bright and short lived (few Million years)
Canterbury 04/11/23
The Sky
Gal. CenterGal. Plane Gal. Plane
Gal. North Pole
Gal. South Pole
Canterbury 04/11/23
Massive O-Stars
Canterbury 04/11/23
Massive OB-Stars
Canterbury 04/11/23
OB-Stars + Dust
Canterbury 04/11/23
OB-Stars + Dust
Gal. CenterGal. Plane Gal. Plane
Gal. North Pole
Gal. South Pole
Canterbury 04/11/23
The Circinus Cloud
Canterbury 04/11/23
B68
Canterbury 04/11/23
- How do we know stars are forming?
- short lived massive stars exist
- they must have formed in the last few Myrs
- the Universe is 13.7Gyrs old
Content
Canterbury 04/11/23
- Where do stars form?
- in or near Giant Molecular Cloudsmostly molecular hydrogen + 1% dust+ traces of CO, H2O, NH3, ...
- these clouds are massive (104-106MSUN)
- these clouds are cold (10-30K)
Content
Canterbury 04/11/23
- How do we know stars are forming?
- Where do stars form?
- Properties of young stars
- Temperature & Turbulence vs. Gravity
- Collapse, Discs and Jets
Content
Canterbury 04/11/23
Region S106:150 young starsforming in Cygnus
Subaru Observatory
Canterbury 04/11/23
Region NGC346:young stars forming in the LMC
Hubble SpaceTelescope
Canterbury 04/11/23
Tarantula Nebula:young stars forming in the LMC
Hubble SpaceTelescope
Canterbury 04/11/23
SubaruTelescope
Orion Nebula
Canterbury 04/11/23
- Properties of young stars
- they are ‘social‘ – most form in clusters,some in isolation
- single/binary/tripple/multiple – 147/64/9/1
- many low mass and few high mass stars,universal mass distribution
Content
Canterbury 04/11/23
- How do we know stars are forming?
- Where do stars form?
- Properties of young stars
- Temperature & Turbulence vs. Gravity
- Collapse, Discs and Jets
Content
Canterbury 04/11/23
OriB
OriA
Ori
Betelgeuse
ONC
NGC2024
NGC2071
MON R2
The Problem:
10s of light years
Canterbury 04/11/23
The Problem:
OriB
OriA
Ori
Betelgeuse
ONC
NGC2024
NGC2071
MON R2
10s of light years Solar Diameter
Size: 1016m 109m7 orders of magnitude (x 10.000.000)
Density: changes by 21 orders of magnitude
(x 1.000.000.000.000.000.000.000)
Canterbury 04/11/23
The Problem:
OriB
OriA
Ori
Betelgeuse
ONC
NGC2024
NGC2071
MON R2
10s of light years Solar Diameter
Gravity
But why has not everything collapsed?
Thermal Pressure of gas clouds
critical (Jeans) mass for collapseabout 1MSUN for a cloud of 1ly radius
Canterbury 04/11/23
The Problem:
OriB
OriA
Ori
Betelgeuse
ONC
NGC2024
NGC2071
MON R2
10s of light years Solar Diameter
Gravity
Gravity vs. Thermal pressure
Almost all clouds are above Jeans limit should collapse But we do not observe this!
Solution: Turbulence
Canterbury 04/11/23
The Problem:
OriB
OriA
Ori
Betelgeuse
ONC
NGC2024
NGC2071
MON R2
10s of light years Solar Diameter
Gravity
Turbulence:random bulk motion of materialat supersonic velocities
v>sound speed (200m/s)
creation of shocksincreasing density
Canterbury 04/11/23
The Problem:
OriB
OriA
Ori
Betelgeuse
ONC
NGC2024
NGC2071
MON R2
10s of light years Solar Diameter
Gravity
Gravity vs. Thermal pressure + Turbulence
Star Formation is the interplay of Gravity and supersonic turbulence in Molecular Clouds
Gravoturbulent Fragmentation
Canterbury 04/11/23
- How do we know stars are forming?
- Where do stars form?
- Properties of young stars
- Temperature & Turbulence vs. Gravity
- Collapse, Discs and Jets
Content
Canterbury 04/11/23
Stage 1 Stage 2 Stage 3
Now, how does it work?
Canterbury 04/11/23
Now, how does it work?
Canterbury 04/11/23
Canterbury 04/11/23
Orion Nebula: Discs seen in silhouette
Canterbury 04/11/23
Canterbury 04/11/23
HH 46/47
Canterbury 04/11/23
HH 212
Canterbury 04/11/23
HH 46/47
HST 1994 - 1997
Canterbury 04/11/23
HH 46/47
HST 1994 - 1997
Canterbury 04/11/23
HH 34
HST 1994 - 1997
Canterbury 04/11/23
HH 34
HST 1994 - 1997
Canterbury 04/11/23
The Problem:
OriB
OriA
Ori
Betelgeuse
ONC
NGC2024
NGC2071
MON R2
10s of light years Solar Diameter
Gravity
Gravity vs. Thermal Pressure + Turbulence + angular Momentum + magn. Fields
Spin accretion disc formation ejection of jets (accelerated and collimated by magnetic fields)
feedback from outflows and radiation turblence
Canterbury 04/11/23
Planet Formation
Canterbury 04/11/23
Canterbury 04/11/23
The end