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--- tests:collision:gc1_archive [2014/10/22 15:42] – v.henault-brunet
+++ tests:collision:gc1_archive [2022/10/24 12:26] (current) – external edit 127.0.0.1
@@ Line 1: / Line 1: @@
-====== Archived from GC1 workshop ======
+====== GC I ======
-==== Challenge 1: Equal mass clusters in a tidal field =====
+===== Challenge 1: Equal mass clusters in a tidal field =====
 ^ ^ ^  All Stars ^^^^ 1000 stars^^^^
@@ Line 82: / Line 82: @@
 |  | Parametric Jeans          |   |           |    |           |
 |  | Discrete Jeans            |   |           |    |           |
+===== Challenge 3: Clusters in tidal fields with stellar evolution =====
+(Simulations ran and kindly made available by Holger Baumgardt)\\
+Here we consider 2 clusters which are slightly more realistic:
+  - IC: King (1966) W_0 = 5 model, N = 131072, Kroupa (2001) mass function between 0.1-15 Msun (no black-holes).
+  - No primordial binaries, no central black hole, circular orbit in logarithmic halo with V = 220 km/s.
+  - Z = 0.001
+  - Stellar evolution and mass-loss according to Hurley et al. (2000, 2002)
+  - Two Galactocentric radii: 8.5 kpc and 15 kpc.
+Below are 2 snapshots at an age of roughly 10 Myr, 100 Myr, 1Gyr and 12 Gyr. The columns are the same as in Challenge 2.
+  - {{:data:W05_N131K_RG8.5_FEH-0.0_T10.gz}} UPDATED! Thursday August 22
+  - {{:data:W05_N131K_RG8.5_FEH-0.0_T100.gz}} UPDATED! Thursday August 22
+  - {{:data:W05_N131K_RG8.5_FEH-0.0_T1000.gz}} UPDATED! Thursday August 22
+  - {{:W05_N131K_RG8.5_FEH-0.0_T12000.gz}}
+  - {{:data:W05-N131K_RG15_FEH-0.0.T10.gz}} NEW! Tuesday August 20
+  - {{:data:W05-N131K_RG15_FEH-0.0.T100.gz}} NEW! Tuesday August 20
+  - {{:data:W05-N131K_RG15_FEH-0.0.T1000.gz}} NEW! Tuesday August 20
+  - {{:W05_N131K_RG15_FEH-0.0_T12000.gz}}
+Questions are the same as in Challenge 2, and in addition:
+  - Is the presence of the tidal field affecting the velocity anisotropy in the outer parts?
+  - Can the mass segregation be reproduced by multi-mass King models?
+ Example of the velocity dispersion difference of different mass components:
+{{:data:sig2ratio.png?250}}
+Different models to fit:
+  - $f_\nu$
+  - Multi-mass King
+  - Discrete "Jeans like" modelling
+  - DF fitting (Mark W?)
+==== Results: ====
+Using all stars:
+^ ^ ^ ^  All Stars ^^^^ 1000 stars^^^^
+^ Cluster ^ Snapshot ^ Method             ^$M$^$r_{\rm c}$^$r_{\rm h}$^$r_{\rm J}$ ^ $M$^$r_{\rm c}$^$r_{\rm h}$^$r_{\rm J}$^
+|1 | 1 | Isotropic King   |  |         | |           |
+|  | 1 | Multimass Michie King      |         | |   |           |
+|  | 1 | $f_\nu$              |  |           | |           |
+|  | 1 | Discrete modelling        |   |           |           |           |
+|1 | 2 | Isotropic King   |  |         | |           |
+|  | 2 | Multimass Michie King      |         | |   |           |
+|  | 2 | $f_\nu$              |  |           | |           |
+|  | 2 | Discrete modelling        |   |           |           |           |
+|1 | 3 | Isotropic King   |  |         | |           |
+|  | 3 | Multimass Michie King      |         | |   |           |
+|  | 3 | $f_\nu$              |  |           | |           |
+|  | 3 | Discrete modelling        |   |           |           |           |
+|1 | 4 | Isotropic King   |  |         | |           |
+|  | 4 | Multimass Michie King | $2.118$ |  | $11.353$ |  |
+|  | 4 | $f_\nu$              |  |           | |           |
+|  | 4 | Discrete modelling        |   |           |           |           |
+|2 | 1 | Isotropic King   |  |         | |           |
+|  | 1 | Multimass Michie King      |         | |   |           |
+|  | 1 | $f_\nu$              |  |           | |           |
+|  | 1 | Discrete modelling        |   |           |           |           |
+|2 | 2 | Isotropic King   |  |         | |           |
+|  | 2 | Multimass Michie King      |         | |   |           |
+|  | 2 | $f_\nu$              |  |           | |           |
+|  | 2 | Discrete modelling        |   |           |           |           |
+|2 | 3 | Isotropic King   |  |         | |           |
+|  | 3 | Multimass Michie King      |         | |   |           |
+|  | 3 | $f_\nu$              |  |           | |           |
+|  | 3 | Discrete modelling        |   |           |           |           |
+|2 | 4 | Isotropic King   |  |         | |           |
+|  | 4 | Multimass Michie King      |         | |   |           |
+|  | 4 | $f_\nu$              |  |           | |           |
+|  | 4 | Discrete modelling        |   |           |           |           |
+Plots
+^ Cluster  ^ Plots ^
+|1 | 1 | Isotropic King vs $f_\nu$ | |
+|  | 1 | Multimass Michie King   | |
+|  | 1 | Discrete modelling        | |
+|1 | 2 | Isotropic King vs $f_\nu$ | |
+|  | 2 | Multimass Michie King   | |
+|  | 2 | Discrete modelling        | |
+|1 | 3 | Isotropic King vs $f_\nu$ | |
+|  | 3 | Multimass Michie King   | |
+|  | 3 | Discrete modelling        | |
+|1 | 4 | Isotropic King vs $f_\nu$ | |
+|  | 4 | Multimass Michie King   |{{:data:t3c1.png?250}} |
+|  | 4 | Discrete modelling        | |
+|2 | 1 | Isotropic King vs $f_\nu$ | |
+|  | 1 | Multimass Michie King   | |
+|  | 1 | Discrete modelling        | |
+|2 | 2 | Isotropic King vs $f_\nu$ | |
+|  | 2 | Multimass Michie King   | |
+|  | 2 | Discrete modelling        | |
+|2 | 3 | Isotropic King vs $f_\nu$ | |
+|  | 3 | Multimass Michie King   | |
+|  | 3 | Discrete modelling        | |
+|2 | 4 | Isotropic King vs $f_\nu$ | |
+|  | 4 | Multimass Michie King   | |
+|  | 4 | Discrete modelling        | |
+==== Results: ====
+Velocity dispersion for different mass species: the multi-mass King models assume that the product $m\sigma_K^2$= constant. The parameters $\sigma_K$ is not exactly the velocity dispersion.