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  • Webster's Revised Unabridged Dictionary
    • n Cuspis A point; a sharp end.
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Century Dictionary and Cyclopedia
    • n cuspis In zoology and anatomy, a cusp; a point, tip, or mucro.
    • ***


Webster's Revised Unabridged Dictionary


In science:

The inner parts of elliptical galaxies and many spiral bulges are well described by power-law (“cuspy ”) stellar density pro files of the form r ∼ r−g with g ≈ 2 .
The Final Parsec Problem
An example would be the possibility of avoiding the cuspy dark matter halo profiles expected in the context of CDM models.
The Role of Baryons in Unified Dark Matter Models
Many of the difficulties that CDM faces on small scales derive from the result that the centres of pure CDM halos are very cuspy.
Dark Matter in Galaxies: Conference Summary
Dwarf spheroidal galaxies show the highest degree of DM domination (Wilkinson), and the conclusion of Kleyna et al. (2003) that the UMi dwarf has a nearly harmonic core is certainly a headache for CDM, but Draco does have a cuspy potential (Kleyna et al. 2002).
Dark Matter in Galaxies: Conference Summary
It seems that in many, perhaps all LSB galaxies, the potentials are less cuspy than pure-CDM theory predicts.
Dark Matter in Galaxies: Conference Summary
If very high densities of dark matter are present in the galactic center, such as would be expected for very cuspy halo profiles or density spikes, sizable neutrino fluxes could be produced.
Searching For Dark Matter with Neutrino Telescopes
Cosmological numerical simulations invariably produce cuspy dark halos, but the precise value of the inner slope α of the radial density profile ρ ∼ rα is debated.
Dark Matter in Galaxies: Observational overview
Ferrer argued that χ annihilation into photons in the GC is an unpromising venture since the DM distribution is not cuspy. A better place to look would be Sagittarius or Draco which have a high M /L. W.
Summary of the XXXIX Rencontres de Moriond
The DM halo is then found to be ellipsoidal, less cuspy than the NFW (Navarro-Frenk-White) model and the Moore model.
Summary of the XXXIX Rencontres de Moriond
They also found that a central cuspy NFW fitting profile implies a velocity dispersion which is too large by a factor of ∼ 2 to be consistent with the measured velocity dispersion.
Long-term stability of collisionless equilibrium configurations; algorithms
We note that this process used a projected density map with pixel scale ≈ 2 arcsec, fine enough to retain any cuspy features in the mass distribution.
Physical component analysis of galaxy cluster weak gravitational lensing data
With no additional information it is impossible to infer uniquely the presence of convergence greater than unity: in contrast, when constructing the mass distribution from naturally cuspy components the convergence can be effectively interpolated upwards in a seamless and physically-reasonable way.
Physical component analysis of galaxy cluster weak gravitational lensing data
This agrees with the maps of Figure 4, where the cuspy cluster centre is not reproduced with the smooth maximum-entropy map.
Physical component analysis of galaxy cluster weak gravitational lensing data
One area now receiving attention is the manner in which angular momentum coupling between dark matter and baryons affects bar/disk formation and the cuspiness of bulges.
Galaxy Formation
Feedback may also play a role in determining the cuspiness of the dark matter halos, which does not appear consistent with profiles predicted from N-body simulations (Silk 2004).
Galaxy Formation