ram pressure stripping of disk galaxies
DESCRIPTION
Ram Pressure Stripping of Disk Galaxies. Elke Schumacher , Institute of Theoretical Physics und Astrophysics Uni Kiel Gerhard Hensler, Institute for Astronomy Uni Vienna Environments of Galaxies, Crete, August 2004. . Roediger. Analytical Estimate:. Analytical Estimate:. - PowerPoint PPT PresentationTRANSCRIPT
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Ram Pressure Stripping of Disk Galaxies
Elke Schumacher, Institute of Theoretical Physics und Astrophysics Uni KielGerhard Hensler, Institute for Astronomy Uni Vienna
Environments of Galaxies, Crete, August 2004
Roediger
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Analytical Estimate:
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Analytical Estimate:
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d/dz gas
(r) = fgrav
= p
ram =
ICMv
ICM
2
Analytical Estimate:
![Page 5: Ram Pressure Stripping of Disk Galaxies](https://reader034.vdocuments.net/reader034/viewer/2022051316/56815a91550346895dc805a4/html5/thumbnails/5.jpg)
d/dz gas
(r) = fgrav
= p
ram =
ICMv
ICM
2
Analytical Estimate:
![Page 6: Ram Pressure Stripping of Disk Galaxies](https://reader034.vdocuments.net/reader034/viewer/2022051316/56815a91550346895dc805a4/html5/thumbnails/6.jpg)
d/dz gas
(r) = fgrav
= p
ram =
ICMv
ICM <
> 2
Analytical Estimate:
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d/dz gas
(r) = fgrav
= p
ram =
ICMv
ICM <
>
independent of Mach number?
independent ofvertical structure(thickness) ?
2
Analytical Estimate:
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Scanning the wind parameter space:
cluster centres
to
outskirts
ICM sound speed ( TICM
=4107K)
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The model galaxy: stellar disk mass 8 1010 Msun
bulge 2 1010 Msun
gas disk mass 8 109 Msun
DM mass (R<50kpc) 3.8 1011 Msun
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The model galaxy gas disk:
10-3 cm-3=10-27 g cm-3
density:
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The model galaxy gas disk:
same (r)
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Results - time evolution:
10-3 cm-3=10-27 g cm-3
density:
nICM
vICM
=1000 cm -3 km2 / s22
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Results - mass and radius of remaining disk:
measured:
a) mass inside disk region
b) bound mass
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Results - mass and radius of remaining disk:
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Results - mass and radius of remaining disk:
nICM
vICM
=1000 cm -3 km2 / s22
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Results - mass and radius of remaining disk:
nICM
vICM
=1000 cm -3 km2 / s22
1Msun / yr
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Results - mass and radius of remaining disk:
nICM
vICM
=10 000 cm -3 km2 / s22
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Results - mass and radius of remaining disk:
nICM
vICM
=100 cm -3 km2 / s22
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nICM
vICM
=10 cm -3 km2 / s2
Results - time evolution:2
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Results - influence of vertical structure:
nICM
vICM
=1000 cm -3 km2 / s22
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nICM
vICM
=1000 cm -3 km2 / s22
Results - influence of Mach number:
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Comparison analytical-numerical:
nICM
vICM
=1000 cm -3 km2 / s22
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Comparison analytical numerical
d/dz gas
(r) = fgrav
=
pram
= ICM
vICM
<>
2
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Comparison analytical numerical
d/dz gas
(r) = fgrav
=
pram
= ICM
vICM
<>
2
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Comparison analytical numerical
d/dz gas
(r) = fgrav
=
pram
= ICM
vICM
= 0.25
<>
2
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How much gas does fall back?
•10 to 15% of original gas disk mass
ISM that has left the disk:
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Conclusions:•Stripping radius can be predicted approximately by simple analytical estimate
•mainly dependent on ram pressure, slightly on Mach number
•independent of vertical structure of gas disk
•Cluster centres: heavy truncation and mass loss
- displacement of all but inner part in few 10Myr
- displaced gas unbound in few 100Myr
•Cluster outskirts: nearly no mass loss, yet truncation
- displacement of edge in few 100Myr
- displaced gas not gas unbound, but falls back
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Future Work
•basis for further investigations:
- inhomogeneous ISM
- inclination (other than face-on)
- time-dependent wind cluster crossing
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Timescales:
10x
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Results - mass and radius of remaining disk:
nICM
vICM
=10 cm -3 km2 / s22
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Results - location of bound gas:
nICM
vICM
=1000 cm -3 km2 / s22