a different dark matter potential for modeling cluster atmospheres andisheh mahdavi university of...
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![Page 1: A Different Dark Matter Potential for Modeling Cluster Atmospheres Andisheh Mahdavi University of Hawai’i](https://reader036.vdocument.in/reader036/viewer/2022062423/56649d575503460f94a36703/html5/thumbnails/1.jpg)
A Different Dark Matter Potential for Modeling Cluster Atmospheres
Andisheh Mahdavi
University of Hawai’i
1/0( )n n nGM r r
![Page 2: A Different Dark Matter Potential for Modeling Cluster Atmospheres Andisheh Mahdavi University of Hawai’i](https://reader036.vdocument.in/reader036/viewer/2022062423/56649d575503460f94a36703/html5/thumbnails/2.jpg)
Why are the shapes of cluster potentials so important?
• N-body simulations predict self-similar dark matter halos
• Shapes of potentials can constrain dark matter physics
• Clusters of galaxies probe dark matter potentials at the very largest scales.
![Page 3: A Different Dark Matter Potential for Modeling Cluster Atmospheres Andisheh Mahdavi University of Hawai’i](https://reader036.vdocument.in/reader036/viewer/2022062423/56649d575503460f94a36703/html5/thumbnails/3.jpg)
Mass profiles in common use
3
2 20( )
rM
r r
2 20ln( )r r
2 20
2 2 20
(3 / )
( )
r r
r r
“-model” profile
00
ln(1 / )r
M r rr r
0ln(1 / )r r
r
20
1
( )r r r
NFW profile
Not analytic
Not analytic
30
1
( )n nr r r
Generalized cusp
![Page 4: A Different Dark Matter Potential for Modeling Cluster Atmospheres Andisheh Mahdavi University of Hawai’i](https://reader036.vdocument.in/reader036/viewer/2022062423/56649d575503460f94a36703/html5/thumbnails/4.jpg)
An invertible potential with variable slope
1
001/
0 0
Consider = - ( )
nn n
n n n n n
GM rM M
r r r r
•Has finite mass M0
•Invertible:
•Useful for calculating distribution functions
•Facilitates stellar dynamics modeling
•n=1 corresponds to Hernquist’s model; n=2 gives the Plummer sphere.
![Page 5: A Different Dark Matter Potential for Modeling Cluster Atmospheres Andisheh Mahdavi University of Hawai’i](https://reader036.vdocument.in/reader036/viewer/2022062423/56649d575503460f94a36703/html5/thumbnails/5.jpg)
An invertible potential with variable slope
2 1/20Density =
nn n nr r r
•Inner slope is 2-n; outer slope is 3+n
•n~1/2 is close to the highest resolution N-body simulations
•Generalizes classical mass profiles, but allows a free shape parameter
![Page 6: A Different Dark Matter Potential for Modeling Cluster Atmospheres Andisheh Mahdavi University of Hawai’i](https://reader036.vdocument.in/reader036/viewer/2022062423/56649d575503460f94a36703/html5/thumbnails/6.jpg)
![Page 7: A Different Dark Matter Potential for Modeling Cluster Atmospheres Andisheh Mahdavi University of Hawai’i](https://reader036.vdocument.in/reader036/viewer/2022062423/56649d575503460f94a36703/html5/thumbnails/7.jpg)
Hydrodynamics with the potential
Hydrostatic equilibrium: gP
0/
2 200
Luminosity ( ) diverges.
True of any potential with convergent mass.
pm kT
g
g
e
T r dr
Isothermal solutions:
![Page 8: A Different Dark Matter Potential for Modeling Cluster Atmospheres Andisheh Mahdavi University of Hawai’i](https://reader036.vdocument.in/reader036/viewer/2022062423/56649d575503460f94a36703/html5/thumbnails/8.jpg)
Hydrodynamics with the potential
Hydrostatic equilibrium: gP
3 /
0
0 0
0 0
3 1
nn nr rg
GM m
r kT
Isothermal solutions: unphysical
Equipartition solutions: kT
![Page 9: A Different Dark Matter Potential for Modeling Cluster Atmospheres Andisheh Mahdavi University of Hawai’i](https://reader036.vdocument.in/reader036/viewer/2022062423/56649d575503460f94a36703/html5/thumbnails/9.jpg)
Hydrodynamics with the potential
Hydrostatic equilibrium: gP
1/( 1)
0
The equipartition solution is a
polytrope with 1 1/ 3
nn ng r r
gP Equipartition solutions: kT Isothermal solutions: unphysical
Polytropic solutions:
![Page 10: A Different Dark Matter Potential for Modeling Cluster Atmospheres Andisheh Mahdavi University of Hawai’i](https://reader036.vdocument.in/reader036/viewer/2022062423/56649d575503460f94a36703/html5/thumbnails/10.jpg)
Application
• Are clusters regular outside the very central regions?
• Many are poorly fit by the standard -model profile
• Cooling flows may not always be the cause for the surface brightness peak.
![Page 11: A Different Dark Matter Potential for Modeling Cluster Atmospheres Andisheh Mahdavi University of Hawai’i](https://reader036.vdocument.in/reader036/viewer/2022062423/56649d575503460f94a36703/html5/thumbnails/11.jpg)
Abell 2550
![Page 12: A Different Dark Matter Potential for Modeling Cluster Atmospheres Andisheh Mahdavi University of Hawai’i](https://reader036.vdocument.in/reader036/viewer/2022062423/56649d575503460f94a36703/html5/thumbnails/12.jpg)
![Page 13: A Different Dark Matter Potential for Modeling Cluster Atmospheres Andisheh Mahdavi University of Hawai’i](https://reader036.vdocument.in/reader036/viewer/2022062423/56649d575503460f94a36703/html5/thumbnails/13.jpg)
![Page 14: A Different Dark Matter Potential for Modeling Cluster Atmospheres Andisheh Mahdavi University of Hawai’i](https://reader036.vdocument.in/reader036/viewer/2022062423/56649d575503460f94a36703/html5/thumbnails/14.jpg)
Conclusion•A new surface brightness formulation is proposed, with an extra free parameter that can be tied to a physical potential
•This profile can fit clusters with rising SB without the need for a divergent power law
•The inferred value of n for Abel 2550 is 0.4, close the what high resolution simulations predict for dark matter halos
•The potential is an invertible generalization of commonly used ones, and so is useful outside X-ray astronomy:
1/0( )n n nGM r r