Dark Matter and Galactic Structuresicranet.org/am/talks/talk_krut.pdf · 29.06.2016Dark Matter 1/38 and Galactic Structures Adriatic Meeting June 20th – June 30, 2016 Pescara (Italy)

1/38 29.06.2016

Dark Matter and Galactic Structures

Adriatic Meeting June 20th – June 30, 2016

Pescara (Italy)

A. Krut, C. R. Argüelles, G. Gomez, J. A. Rueda and R. Ruffini

Supported by the Erasmus Mundus Joint Doctorate Program by Grants Number 2014-0707 from the agency EACEA of the European Commission

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Outline

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Introduction

DM model

Milky Way

Conclusion Galaxy Morphology Different types of stallar formations

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Introduction

DM model

Milky Way

Conclusion Milky Way Besides the bulge and disk

halo

massive and compact core

bulge

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Introduction

DM model

Milky Way

Conclusion Lambda-CDM The Large Structures of the Universe

0%

5%

10%

15%

20%

25%

30%

ordinarymatter

darkmatter

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Introduction

DM model

Milky Way

Conclusion So, where can we find DM? Dark Matter distribution on galactic scales

dwarf galaxies

spirals

big ellipticals

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Introduction

DM model

Milky Way

Conclusion Dark Matter Candidates Particle candidates beyond SM

CD

M

WD

M

HD

M

!

particle mass

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Introduction

DM model

Milky Way

Conclusion Model assumptions From first principles

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Introduction

DM model

Milky Way

Conclusion Fermionic DM with Cutoff Self-gravitating system of massive fermions in spherical symmetry

phase space DF

Ruffini R., Stella L., 1983, A&A, 119, 35

rel. energy

temperature parameter

rel. chemical potential

rel. escape energy

degeneracy parameter

cutoff parameter

phase space density

chemical potential (relativistic)

escape energy (relativistic)

energy

temperature parameter

degeneracy parameter

cutoff parameter

Ruffini R., Stella L., 1983, A&A, 119, 35

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Introduction

DM model

Milky Way

Conclusion Perfect fluid in equilibrium

mass density

pressure

mass

metric potential

Stat

isti

cs

GR

spherically symmetric

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Introduction

DM model

Milky Way

Conclusion Thermodynamic equilibrium EOS

Tolman & Ehrenfest (1930)

Klein (1949)

conservation of energy

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Introduction

DM model

Milky Way

Conclusion Initial conditions Parameter of the model

4 parameters scaling factors

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Introduction

DM model

Milky Way

Conclusion

Fermi-Dirac distribution

No evaporation

Turn off evaporation Let‘s start slowly

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Introduction

DM model

Milky Way

Conclusion RAR family halo-core solutions

Ruffini R., Argüelles C. R., Rueda J. A., 2015, MNRAS, 451, 622

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Introduction

DM model

Milky Way

Conclusion Turn on evaporation from halo-core solutions to fully degenerate cores

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Introduction

DM model

Milky Way

Conclusion (most) general profile regimes in density profile

core plateau halo fall

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Introduction

DM model

Milky Way

Conclusion (most) general profile regimes in density profile - core

1 2

1

2

uniform core

core shell


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Introduction

DM model

Milky Way

Conclusion (most) general profile regimes in density profile - fall

1 2

3

4

1

2

3

4

uniform core

core shell

steep fall

evaporation pull


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Introduction

DM model

Milky Way

Conclusion (most) general profile regimes in density profile – plateau and halo

1 2

3

4

5 6

1

2

3

4

5

6

uniform core

core shell

steep fall

evaporation pull

plateau

free halo with cutoff


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Introduction

DM model

Milky Way

Conclusion (most) general profile less regimes in rotation curve

degenerate core

core shell

(internal)

Keplerian

halo core (external)

Keplerian


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Introduction

DM model

Milky Way

Conclusion Core, Plateau and free Halo defined by extrema in the rotation curve

core

plateau

free halo

first maxima

lowest minima

maxima after plateau

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Introduction

DM model

Milky Way

Conclusion Various regimes For varying central degeneracy (temperature and cutoff parameter are fixed)

A B C D E F

A

B

C

D

E

F

diluted regime diluted core with halo

semi-degenerate transition core becomes more degenerate

degenerate regime (with halo) surface radius is decreasing

critical regime surface effects appear

degenerate regime (no halo) halo evaporated

fully degenerate core

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Introduction

DM model

Milky Way

Conclusion Various regimes For varying central degeneracy (temperature and cutoff parameter are fixed)

A B C D E F

A

B

C

D

E

F


semi-degenerate transition core becomes more degenerate





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Introduction

DM model

Milky Way

Conclusion Focus regimes with halo For varying central degeneracy (temperature and cutoff parameter are fixed)

A B C D E F

A

B

C

D

E

F


semi-degenerate transition a degenerate core forms





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Introduction

DM model

Milky Way

Conclusion Vary evaporation

D C B A

A

B

C

D

weak evaporation finite mass distribution

critical evaporation surface effects appear

strong evaporation evaporation of the halo

disruptive evaporation fully degenerate core

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Introduction

DM model

Milky Way

Conclusion Vary central temperature

A B C

A

B

C

low temperatures temperature invariance

moderate temperature thermal effects appear

high temperature blow up by thermal pressure

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Introduction

DM model

Milky Way

Conclusion BiKe model in MW Two Keplerian behaviour in rotation curve

core Keplerian inner Bulge

main Bulge

disk halo Intergalactic

medium

Bi-Keplerian

family

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Introduction

DM model

Milky Way

Conclusion BiKe model Change of parameters

core Keplerian inner Bulge

main Bulge

disk halo Intergalactic

medium

1

2

Bi-Keplerian

family

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Introduction

DM model

Milky Way

Conclusion BiKe family in Milky Way different degenerate cores for same halo

speed of light

S-stellar cluster

Exp. Sphere model

!

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Introduction

DM model

Milky Way

Conclusion BiKe family in Milky Way

critical density of Galactic Nucleus

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Introduction

DM model

Milky Way

Conclusion BiKe family analysis Extrema in parameter space

local maxima

local minima

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Introduction

DM model

Milky Way

Conclusion BiKe family analysis Bifurkation in parameter space

local maxima

local minima

bifurcation

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Introduction

DM model

Milky Way

Conclusion Alternative Core density profile

critical density of Galactic core

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Introduction

DM model

Milky Way

Conclusion Alternative Core rotation curve

speed of light

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Introduction

DM model

Milky Way

Conclusion Compactness Two Schwarzschild radii

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Introduction

DM model

Milky Way

Conclusion Compactness Two Schwarzschild radii

core compactness coverges to approx. 2 Schwarzschild radii

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Introduction

DM model

Milky Way

Conclusion Summary

halo

degenerate core

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Introduction

DM model

Milky Way

Conclusion

Thank you

Dark Matter and Galactic Structuresicranet.org/am/talks/talk_krut.pdf · 29.06.2016Dark Matter 1/38 and Galactic Structures Adriatic Meeting June 20th – June 30, 2016 Pescara (Italy)

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