Environmental Engineering Reference
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Table 3. Values of parameters related to two-component, collisionless, virialized
systems at the end of computer runs performed in a recent investigation (Nipoti et al.,
2006). The principal axes of inertia related to the stellar subsystem, are denoted as
A
,
B
,
C
, respectively. Cases (i)-(iv) and (vii) are largely aspherical.
ID
Name
C/A
B/A
Γ
∗
Γ
h
Β
R
i
hpl1r2m002
0.34
0.35
0.12
1.45
10.70
2
ii
plpl05r2m002
0.30
0.34
1.37
0.57
01.78
2
iii
plpl05r5m002
0.47
0.72
1.48
0.58
01.59
5
iv
g0hq05r2m002
0.42
0.85
1.98
0.65
02.48
2
v
hpl4r2m005
0.99
0.99
0.00
0.18
00.56
2
vi
hpl8r2m005
0.99
1.00
0.00
0.34
00.32
2
vii
npl4r2m005
0.33
0.33
0.00
1.37
05.14
2
viii
npl4r4m005
0.97
0.98
0.02
1.98
02.78
4
xi
g15pl4r2m005
0.97
0.99
0.00
1.38
00.86
2
Table 4. Input and output parameters related to 5 computer runs performed in the
current investigation, starting from a spherical-symmetric
Γ
∗
density profile
(
N
= 102
,
400)
within a fixed gravitational potential induced by a
spherical-symmetric
Γ
h
density profile. The fractional scaling radii,
Β
sim
and
Β
MVPE
,
are related to the best fitting (at the end of the computer run) GG model and MVPE
configuration with equal
R
, respectively. The stellar subsystem at the end of Sim3
computer run cannot be reproduced by
Γ
density profiles.
Input parameters
Output parameters
ID
Γ
h
Γ
∗
Β
R
Γ
∗
Β
sim
R
Β
MVPE
Sim1
1.00
1.00
2.00
25
0.01
4.17
25
13.25
Sim2
1.00
0.00
1.00
25
1.16
0.85
25
6.12
Sim3
0.00
1.00
2.00
25
-
-
25
-
Sim4
0.00
0.00
0.50
25
0.49
0.62
25
7.00
Sim5
0.50
0.00
0.50
25
1.00
0.46
25
6.20
according to Eqs. (11) and (12), where no absolute extremum point is present. In a reduced
representation, called
energy-conservation paradigm
, extremum points take place above a
threshold in the DM halo to stellar mass ratio,
R
, and MVPE configurations are defined
with that specific fractional scaling radius,
Β
=
R
h
/
R
∗
, which univocally represents the
maximum of the VPE.
With the aim of investigating the role of MVPE configurations in large-scale objects,
ETGs and their hosting DM halos have been modeled as two-component systems described
by density profiles of astrophysical interest.
Using the FP of ETGs, it has been shown
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