Field theory

Conferences

2017

11 - 13 October 2017
RTG Autumn Workshop
Where: Oldenburg

28 September - 01 October 2017 
21st German Conference of Women in Physics 
Where: Ilmenau

18 -19 May 2017 
12. Kosmologietag 
Where: Center for Interdisciplinary Research, ZiF at Bielefeld University

13. - 17. March 2017 
DPG Spring Meeting 
Where: Universty of Bremen, ZARM

6 - 7 March 2017 
GRK Workshop Hannover
Where: Hannover

Bremen-Oldenburg Relativity Seminar

                      Andreas Krut
            La Sapienza University, Rome, Italy

   "Novel constraints on fermionic dark matter from galactic observables"

             Thursday, 11 January 2018, 14:30, 12:00
             University of Bremen, ZARM, Room 1280

Abstract:


We have recently introduced a new model for the distribution of dark
matter (DM) in galaxies, the Ruffini-Argüelles-Rueda (RAR) model, based
on a self-gravitating system of massive fermions at finite temperatures.
The RAR model for fermion masses above keV successfully describes the DM
halos in galaxies and predicts the existence of a denser quantum core
towards the centre of each configuration. We demonstrate here that the
introduction of a cutoff in the fermion phase-space distribution,
necessary to account for the finite Galaxy size, defines a new solution
with a compact quantum core which represents an alternative to the
central black hole (BH) scenario for SgrA*. For a fermion mass in the
range mc² = 48 - 345 keV the DM halo distribution fulfils the most
recent data of the Milky Way rotation curves while harbours a dense
quantum core of 4E6 Msun within the S2 star pericentre. In particular,
for a fermion mass of mc² = 48 keV the model is able to explain the DM
halos from typical dwarf spheroidal to normal elliptical galaxies while
harbouring dark and massive compact objects from 1E3 Msun up to 1E8 Msun
at their respective centres. The model is shown to be in good agreement
with different observationally inferred universal relations, such as the
ones connecting DM halos with supermassive dark central objects.
Finally, the model provides a natural mechanism for the formation of
supermassive BHs as heavy as few 1E8 Msun. We argue that larger BH
masses (1E9 - 1E10 Msun) may be achieved by assuming subsequent
accretion processes onto the above heavy seeds, depending on accretion
efficiency and environment.