Secondary infall model of galactic halo formation and the spectrum of cold dark matter particles on Earth

Sikivie, P.; Tkachev, I.; Wang, Yun

doi:10.1103/physrevd.56.1863

Cited by 163 publications

(192 citation statements)

References 24 publications

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“…Moreover, dimensional analysis suggests that the rms angular momentum of particles in the inner region scales with radius as j / GrM r ð Þ ½ 1 = 2 . This scale-free assumption allows a self-similarity that changes only gradually from outer to inner regions, as noted by Sikivie et al (1997), Nusser (2001), Le Delliou & Henriksen (2003), and Ascasibar et al (2004). Here we argue that this rms angular momentum is generated by torques due to the evolving barlike perturbation.…”

Section: The Radial Orbit Instabilitymentioning

confidence: 96%

“…Naive selfsimilarity can be extended to incorporate nonradial motions. Sikivie et al (1997), Nusser (2001), Le Delliou & Henriksen (2003), and Ascasibar et al (2004) include angular momentum in the infall model while preserving (only adiabatically changing) approximate self-similarity and spherical symmetry. These conditions require that the distribution of particle orbits be isotropic in the plane tangent to the radial direction and that the specific rms angular momentum at turnaround be proportional to M ta r ta ð Þ 1/2 .…”

Section: Introductionmentioning

confidence: 99%

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On Universal Halos and the Radial Orbit Instability

MacMillan

Widrow

Henriksen

2006

ApJ

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The radial orbit instability drives the density profile of a collapsing nearly spherical density perturbation toward the universal form found in cosmological simulations. This conclusion, first noted by Huss and coworkers, is explored in detail through a series of numerical experiments involving isolated halos. Simulations are run with and without the nonradial forces responsible for the instability. In the absence of the instability, the density profile is a pure power law, the differential energy distribution is close to a Boltzmann distribution, and the orbits are radially biased. The instability transforms the density profile to the NFW form, induces an energy cutoff at high binding energy, and isotropizes the orbits near the center of the system. New insights into the underlying physics of the radial orbit instability are presented. Subject headingg s: cosmology: theory -dark matter -large-scale structure of universe

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Section: The Radial Orbit Instabilitymentioning

confidence: 96%

Section: Introductionmentioning

confidence: 99%

On Universal Halos and the Radial Orbit Instability

MacMillan

Widrow

Henriksen

2006

ApJ

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A solution to the problems of cusps and rotation curves in dark matter halos in the cosmological standard model

Doroshkevich¹,

Lukash²,

Mikheeva³

2012

Uspekhi Fizicheskikh Nauk

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“…In CDM theories of large scale structure formation, ǫ is expected to be in the range 0.2 to 0.35 [15,16]. In that range, the galactic rotation curves predicted by the self-similar infall model are flat [17].…”

Section: Introductionmentioning

confidence: 99%

“…where j max is a parameter, with a specific value for each halo, which is proportional to the amount of angular momentum that the dark matter particles have [15,16], h is the present Hubble constant in units of 100 km/(s Mpc), and v rot is the rotation velocity of the galaxy.…”

Section: Introductionmentioning

confidence: 99%

Gravitational lensing and structural stability of dark matter caustic rings

Onemli

2006

Phys. Rev. D

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Gravitational lensing by the dual cusp (A −3 ) catastrophes of the cold dark matter (CDM) caustic rings at cosmological distances may provide the tantalizing opportunity to detect CDM indirectly, and discriminate between axions and weakly interacting massive particles (WIMPs). The infall of CDM onto isolated galaxies such as our own produces discrete number of flows and caustics in the halo CDM distribution. Caustics are places where the CDM particles are naturally focussed. In the CDM cosmology, caustics in the distribution of dark matter are plentiful once density perturbations enter the nonlinear regime. Our focus is upon the caustic rings which are closed tubes whose cross-section is an elliptic umbilic (D −4 ) catastrophe with three dual cusps. We call this cross-section a "tricusp." Caustic rings are located near where the particles with the most angular momentum in a given inflow reach their distance of closest approach to the galactic center before going back out. We reparameterize the CDM flow near a caustic ring, and obtain the ring equations in space, as single valued functions of an angular variable parameterizing the tricusp. A caustic ring has a specific density profile, a specific geometry and, therefore, precisely calculable gravitational lensing signatures that vary on the caustic surface, depending on the location of the line of sight. We calculate the image magnification of point-like sources as a function of the angular parameter of the tricusp for the line of sights that are parallel to the galactic plane of the caustic ring and near tangent to the surface. The magnification monotonically increases 1 as the line of sight approaches to the cusps where it diverges in the limit of zero velocity dispersion. If the velocity dispersion is small but nonzero, the divergence is cut off, because the caustic surface gets smeared over some distance in space and the cusps are smoothed out. The lensing effects are no longer infinite at the cusps, but merely large. To estimate the magnification numerically, for the rings at cosmological distances and for the ring closest to us (the fifth caustic ring of the Milky Way), we choose sample points near the cusps. We find that the lensing effects are largest at the outer cusp which lies in (or, near) the galactic plane.Around the outer cusp, the surface is curved toward the side with two extra flows. We call such a surface concave. In the limit of zero velocity dispersion, at a sample point near the outer cusp, we find 37% magnification for the CDM caustic rings at cosmological distances. This is about 250 times stronger than the lensing effect we predicted for the concave folds (considering the A 2 catastrophes enveloping the galaxy), and 37 times stronger than the largest lensing effect we predicted for the CDM caustics (considering the convex folds of the rings) before. In the presence of finite velocity dispersion, the lower and upper bounds of the effective velocity dispersions of the axion and WIMP flows in galactic halos may be used to constrai...

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Secondary infall model of galactic halo formation and the spectrum of cold dark matter particles on Earth

Cited by 163 publications

References 24 publications

On Universal Halos and the Radial Orbit Instability

On Universal Halos and the Radial Orbit Instability

A solution to the problems of cusps and rotation curves in dark matter halos in the cosmological standard model

Gravitational lensing and structural stability of dark matter caustic rings

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