scholarly journals Angular Momentum Transfer in Dark Matter Halos: Erasing the Cusp

2006 ◽  
Vol 649 (2) ◽  
pp. 591-598 ◽  
Author(s):  
C. Tonini ◽  
A. Lapi ◽  
P. Salucci
Keyword(s):  
Dark Matter ◽  
Angular Momentum ◽  
Momentum Transfer ◽  
Dark Matter Halos ◽  
Angular Momentum Transfer

scholarly journals Dark matter bars in spinning haloes

2019 ◽  
Vol 488 (4) ◽  
pp. 5788-5801 ◽  
Author(s):  
Angela Collier ◽  
Isaac Shlosman ◽  
Clayton Heller
Keyword(s):  
Dark Matter ◽  
Angular Momentum ◽  
Momentum Transfer ◽  
Direct Detection ◽  
Maximal Amplitude ◽  
Angular Momentum Transfer ◽  
Secular Evolution ◽  
Secondary Resonances ◽  
Spin Parameter ◽  
Resonance Transfer

ABSTRACT We study non-linear response of spinning dark matter (DM) haloes to dynamic and secular evolution of stellar bars in the embedded galactic discs, using high-resolution numerical simulations. For a sequence of haloes with the cosmological spin parameter λ = 0–0.09, and a representative angular momentum distribution, we analyse evolution of induced DM bars amplitude and quantify parameters of the response as well as trapping of DM orbits and angular momentum transfer by the main and secondary resonances. We find that (1) maximal amplitude of DM bars depends strongly on λ, while that of the stellar bars is indifferent to λ; (2) efficiency of resonance trapping of DM orbits by the bar increases with λ, and so is the mass and the volume of DM bars; (3) contribution of resonance transfer of angular momentum to the DM halo increases with λ, and for larger spin, the DM halo ‘talks’ to itself, by moving the angular momentum to larger radii – this process is maintained by resonances; and (4) prograde and retrograde DM orbits play different roles in angular momentum transfer. The ‘active’ part of the halo extends well beyond the bar region, up to few times the bar length in equatorial plane and away from this plane. (5) We model evolution of discless DM haloes and haloes with frozen discs, and found them to be perfectly stable to any Fourier modes. Finally, further studies adopting a range of mass and specific angular momentum distributions of the DM halo will generalize the dependence of DM response on the halo spin and important implications for direct detection of DM and that of the associated stellar tracers, such as streamers.

scholarly journals Baryons and Dark Matter halo distributions in ΛCDM Cosmology

2009 ◽  
Vol 5 (S262) ◽  
pp. 404-405
Author(s):  
Susana Pedrosa ◽  
Patricia Tissera ◽  
Cecilia Scannapieco
Keyword(s):  
Dark Matter ◽  
Angular Momentum ◽  
Momentum Transfer ◽  
Dark Matter Halo ◽  
Angular Momentum Transfer ◽  
History Of ◽  
Baryonic Mass ◽  
History Of Formation

AbstractWe analyse the dark matter (DM) distribution in a ≈1012M⊙ halo extracted from a simulation consistent with the concordance cosmology, where the physics regulating the transformation of gas into stars was allowed to change producing galaxies with different morphologies. Although the DM profiles get more concentrated as baryons are collected at the centre of the haloes compared to a pure dynamical run, the total baryonic mass alone is not enough to fully predict the reaction of the DM profile. Our findings suggest that the response of the DM halo is driven by the history of assembly of baryons into a galaxy. The accretion of satellites could be associated with an expansion of the dark matter profiles, triggered by angular momentum transfer from the incoming satellites. However, we also found that these mechanism have different efficiencies which are set by the history of formation of the structure.

scholarly journals The dark matter density problem in massive disk galaxies

2004 ◽  
Vol 220 ◽  
pp. 265-270 ◽  
Author(s):  
Benjamin J. Weiner
Keyword(s):  
Dark Matter ◽  
Angular Momentum ◽  
Momentum Transfer ◽  
Matter Density ◽  
Disk Galaxies ◽  
Dark Matter Halos ◽  
Barred Galaxies ◽  
Dark Matter Density ◽  
Disk Mass ◽  
Density Problem

We discuss measurements of disk mass from non-circular streaming motions of gas in the barred galaxies NGC 3095 and NGC 4123. in these galaxies with strong shocks and non-circular motions, the inner regions must be disk-dominated to reproduce the shocks. This requires dark matter halos of low central density and low concentration, compared to LCDM halo predictions. in addition, the baryonic collapse to a disk should have compressed the halo and increased the dark matter density, which sharpens the disagreement. One possible resolution is a substantial amount of angular momentum transfer from disk to halo, but this is not particularly attractive nor elegant.

scholarly journals Spin-lattice dynamics model with angular momentum transfer for canonical and microcanonical ensembles

2021 ◽  
Vol 103 (2) ◽  
Author(s):  
Mara Strungaru ◽  
Matthew O. A. Ellis ◽  
Sergiu Ruta ◽  
Oksana Chubykalo-Fesenko ◽  
Richard F. L. Evans ◽  
...  
Keyword(s):  
Angular Momentum ◽  
Momentum Transfer ◽  
Lattice Dynamics ◽  
Dynamics Model ◽  
Angular Momentum Transfer ◽  
Spin Lattice

scholarly journals Rotation of Galaxy Dark Matter Halos

2006 ◽  
Vol 2 (S235) ◽  
pp. 104-104
Author(s):  
Stéphane Herbert-Fort ◽  
Dennis Zaritsky ◽  
Yeun Jin Kim ◽  
Jeremy Bailin ◽  
James E. Taylor
Keyword(s):  
Dark Matter ◽  
Angular Momentum ◽  
Numerical Simulations ◽  
Galaxy Formation ◽  
Spiral Galaxy ◽  
Observational Studies ◽  
Spiral Galaxies ◽  
Satellite System ◽  
Dark Matter Halos ◽  
The Mean

AbstractThe degree to which outer dark matter halos of spiral galaxies rotate with the disk is sensitive to their accretion history and may be probed with associated satellite galaxies. We use the Steward Observatory Bok telescope to measure the sense of rotation of nearby isolated spirals and combine these data with those of their associated satellites (drawn from SDSS) to directly test predictions from numerical simulations. We aim to constrain models of galaxy formation by measuring the projected component of the halo angular momentum that is aligned with that of spiral galaxy disks, Jz. We find the mean bulk rotation of the ensemble satellite system to be co-rotating with the disk with a velocity of 22 ± 13 km/s, in general agreement with previous observational studies and suggesting that galaxy disks could be formed by halo baryons collapsing by a factor of ≈10. We also find a prograde satellite fraction of 51% and Jz, of the satellite system to be positively correlated with the disk, albeit at low significance (2655 ± 2232 kpc km/s).

scholarly journals Angular momentum transfer and partition in the deep-inelastic reaction 664 MeV 84Kr + natAg

1981 ◽  
Vol 371 (3) ◽  
pp. 510-532 ◽  
Author(s):  
L.G. Sobotka ◽  
C.C. Hsu ◽  
G.J. Wozniak ◽  
D.J. Morrissey ◽  
L.G. Moretto
Keyword(s):  
Angular Momentum ◽  
Momentum Transfer ◽  
Angular Momentum Transfer ◽  
Inelastic Reaction ◽  
Deep Inelastic Reaction
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