@article{GuendelmanSingletonYongram2012,
  author    = {G{\"u}ndelman, Eduardo and Singleton, Douglas and Yongram, N.},
  title     = {A two measure model of dark energy and dark matter},
  series = {Journal of cosmology and astroparticle physics},
  journal   = {Journal of cosmology and astroparticle physics},
  number    = {11},
  publisher = {IOP Publ. Ltd.},
  address   = {Bristol},
  issn      = {1475-7516},
  doi       = {10.1088/1475-7516/2012/11/044},
  pages     = {12},
  year      = {2012},
  abstract  = {In this work we construct a unified model of dark energy and dark matter. This is done with the following three elements: a gravitating scalar field, phi with a non-conventional kinetic term, as in the string theory tachyon; an arbitrary potential, V (phi); two measures - a metric measure (root-g) and a non-metric measure (Phi). The model has two interesting features: (i) For potentials which are unstable and would give rise to tachyonic scalar field, this model can stabilize the scalar field. (ii) The form of the dark energy and dark matter that results from this model is fairly insensitive to the exact form of the scalar field potential.},
  language  = {en}
}
@article{Baushev2016,
  author    = {Baushev, Anton N.},
  title     = {Can the dark matter annihilation signal be significantly boosted by substructures?},
  series = {Journal of cosmology and astroparticle physics},
  volume    = {30},
  journal   = {Journal of cosmology and astroparticle physics},
  publisher = {IOP Publ. Ltd.},
  address   = {Bristol},
  issn      = {1475-7516},
  doi       = {10.1088/1475-7516/2016/01/018},
  pages     = {12 -- 18},
  year      = {2016},
  abstract  = {A very general cosmological consideration suggests that, along with galactic dark matter halos, much smaller dark matter structures may exist. These structures are usually called `clumps', and their mass extends to 10\&\#8722;6 M \&\#8857; or even lower. The clumps should give the main contribution into the signal of dark matter annihilation, provided that they have survived until the present time. Recent observations favor a cored profile for low-mass astrophysical halos. We consider cored clumps and show that they are significantly less firm than the standard NFW ones. In contrast to the standard scenario, the cored clumps should have been completely destroyed inside ~ 20 kpc from the Milky Way center. The dwarf spheroidals should not contain any dark matter clumps. On the other hand, even under the most pessimistic assumption about the clump structure, the clumps should have survived in the Milky Way at a distance exceeding 50 kpc from the center, as well as in low-density cosmic structures. There they significantly boost the dark matter annihilation. We show that at least 70\% of the clumps endured the primordial structure formation should still exist untouched in the present-day Universe.},
  language  = {en}
}
@article{BaushevBarkov2018,
  author    = {Baushev, Anton N. and Barkov, M. V.},
  title     = {Why does Einasto profile index n similar to 6 occur so frequently?},
  series = {Journal of cosmology and astroparticle physics},
  journal   = {Journal of cosmology and astroparticle physics},
  number    = {3},
  publisher = {IOP Publ. Ltd.},
  address   = {Bristol},
  issn      = {1475-7516},
  doi       = {10.1088/1475-7516/2018/03/034},
  pages     = {15},
  year      = {2018},
  abstract  = {We consider the behavior of spherically symmetric Einasto halos composed of gravitating particles in the Fokker-Planck approximation. This approach allows us to consider the undesirable influence of close encounters in the N-body simulations more adequately than the generally accepted criteria. The Einasto profile with index n approximate to 6 is a stationary solution of the Fokker-Planck equation in the halo center. There are some reasons to believe that the solution is an attractor. Then the Fokker-Planck diffusion tends to transform a density profile to the equilibrium one with the Einasto index n approximate to 6. We suggest this effect as a possible reason why the Einasto index n approximate to 6 occurs so frequently in the interpretation of N-body simulation results. The results obtained cast doubt on generally accepted criteria of N-body simulation convergence.},
  language  = {en}
}