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DM density profiles in non-extensive theory
Eelco van Kampen
Institute for Astro- and Particle Physics Innsbruck University
In collaboration with Manfred Leubner and Thomas Kronberger
Classical gravity is an extremely rich theory
The wonderful world of r –1 :
ji
pairs ji
ji
i i
i
r
mmG
m
pH
2
2
A theory with many equations and approximations
from Saslaw (1987)
Classical Gravity (including GR)
• simple but highly non-linear• no equilibrium state (although timescales can be long)• long-range, so hard to isolate systems (galaxies & galaxy clusters !)• gravitational systems tend to form substructure
Gravitational systems are therefore intrinsically hard to model, so approximations are always made
If classical gravity is already hard to ‘use’, adding hydrodynamics (gas, stars !) makes things only harder
Given this, do we really need alternative theories ? Have we properly solved the highly non-linear classical equations yet ? Bottom line:
Astrophysical systems are messy and simply hard to model even
with ‘just’
ji
pairs ji
ji
i i
i
r
mmG
m
pH
2
2
Empirical fitting relations for DM density profiles
(3 )
1~( / ) (1 / )DM
s sr r r r
2 2
1~(1 / )(1 / )DM
s sr r r r
Burkert (1995), Salucci (2000)
Navarro, Frenk & White (1996,1997)
Moore et al. (1999)
Zhao (1996)
Kravtsov et al. (1998)
2
1~( / )(1 / )DM
s sr r r r
and others …
From exponential dependenceto power-law distributions
This does not account properly for long-range interactions
introduce correlations via non-extensive statistics
iiBB ppkS lnStandard Boltzmann-Gibbs statisticsbased on extensive entropy measure
pi…probability of the ith microstate, S extremized for equiprobability
Assumtions: particles independent from e.o. no correlations
isotropy of velocity directions extensivity
Consequence: entropy of subsystems additive Maxwell PDF
microscopic interactions short ranged, Euclidean space time
Non-extensive statistical physics
Subsystems A, B: EXTENSIVE ENTROPY
non-extensive statistics Renyi (1955), Tsallis (1985)
(PSEUDOADDITIVE) NON-EXTENSIVE ENTROPY
Dual nature: + tendency to less organized state, entropy increase - tendency to higher organized state, entropy
decrease
generalized entropy :
with 1/κ long–range interactions / mixing quantifies degree of non-extensivity /couplings
accounts for non-locality / correlations
)1( /11 ipS
)1/(1 q
1( ) ( ) ( ) ( ) ( )q q q q qS A B S A S B S A S B
Equilibrium of a many-body systemwith no correlations
spherical symmetric, self-gravitating, collisionless
f(r,v) = f(E) from Poisson’s equation: 2 314 ( )
2G f v d v
Introduce relative potential Ψ = - Φ + Φ0 (vanishes at boundary)
Er = -v2/2 + Ψ and ΔΨ = - 4π G ρ
f(Er) from extremizing BGS entropy, conservation of mass and energy
exponential energy distribution extensive, independent
202 3/ 2 2
/ 2( ) exp( )
(2 )r
vf E
Equilibrium of a many-body systemwith correlations
long-range gravitational interactions non-extensive systems
extremize non-extensive entropy,conservation of mass and energy corresponding distribution
02 3/ 2 3/ 2
( )
(2 ) ( 3 / 2)B
( κ < 0 energy cutoff v2/2 ≤ κ σ2 – Ψ )
3/ 2
0 2
11
2
2
1 / 2( ) 1r
vf E B
02 3/ 2 3/ 2
( 5 / 2)
(2 ) ( 1)B
02 3/ 2 3/ 2
( )
(2 ) ( 3 / 2)B
integration over v
limit κ = ∞ :∞ : 20 exp( / )
bifurcation κ > 0 :
κ < 0 :
Non-extensive density profiles
1/(3/ 2 )
22 2
0
1 41
d d Gr
r dr dr
1/ 3/ 2222
2 20
4 3/ 22 1 11 03/ 2
Gd d d
dr r dr dr
3/ 2
0 2
11
Combine
ρ(r) is the radial density distribution of spherically symmetric hot plasma (κ > 0) or dark matter halo ( κ < 0)
For κ = = ∞∞ we retrieve the conventional isothermal sphere we retrieve the conventional isothermal sphere
4 G
(Leubner 2005)
with
or
Non-extensive family of density profiles
Non-extensive family of density profiles ρ± (r) , κ = 3 … 10 = 3 … 10
Convergence to the BGS solution for κ = = ∞∞
Simulation vs. theory vs. empirical fit
Kronberger, Leubner & van Kampen (2006)
Theory vs. simulation vs. observation
X-ray data for A1413
(Pointecouteau et al. 2005)
Integrated mass profile
Kronberger, Leubner & van Kampen (2006)
Final thoughts
Classical gravity is an already rich theory full of possibilities to explainastrophysical observations, which have not been all explored yet
Hydrodynamics should be added before comparing to observations using gasand stars, adding a whole range of possibilities for explanations
A theory like non-extensive statistics should be favoured over empiricalfitting relations for density (and other) profiles
Non-extensive entropy generalization generates a bifurcationof the isothermal sphere solution into two power-law profiles,controlled by a single parameter accountin for non-local correlationswith
Κ > 0 for thermodynamic systemsΚ < 0 for self-gravitating systems