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Dwarf spheroidal galaxies (dSphs) are the most compact dark-matter-dominated objects observed so far. The Pauli exclusion principle limits the number of fermionic dark matter particles that can compose a dSph halo. This results in a well-known lower bound on their particle mass. So far, such bounds were obtained from the analysis of individual dSphs. We model dark matter halo density profiles...
The origin of dark matter (DM) is one of the most intriguing questions in modern physics.
One of the most promising DM models is the so-called `warm' dark matter (WDM) with particle mass in the range of keVs.
The signature of warm dark matter could be fewer small size dark matter halos and small mass galaxies in the early Universe (compared to the standard "cold dark matter" (CDM)...
Classification of galaxy types is one of the cornerstones for extragalactic astrophysics and observational cosmology. The most precise method of galaxy classification used by astronomers so far is the manual classification. Its major drawback, however, is the extensive usage of manpower, either from highly skilled professionals, or, in some cases (such as in Galaxy Zoo project) amateur...
We study an impact of asymmetric dark matter on properties of the neutron stars and their ability to reach the two solar masses limit, which allows us to present a new upper constraint on the mass of dark matter particle. Our analysis is based on the observational fact of existence of three pulsars reaching this limit and on the theoretically predicted reduction of the neutron star maximal...
The ultralight dark matter (ULDM) model proposes as DM particles candidates bosons with typical mass $10^{-22}$ eV, such that its de Broglie wavelength is of galactic scale ($\sim$kpc). The ULDM was among the models, that were proposed to resolve CDM tensions on the small scales, such as core-cusp and missing satellite problem. However last times it faces some difficulties between observed...
Three-dimensional electrically charged black hole with nonlinear electromagnetic field in anti-de Sitter spacetime is studied. Both static [1] and slowly rotating cases are considered. Solutions of field equations are obtained and thermodynamic behavior in extended phase space thermodynamics is examined.
[1] M. B. Tataryn, M. M. Stetsko, Int. J. Mod. Phys. D 28 (2019) 1950160.
For obtaining polarization effects in the Kerr space-time we have used algebraically special approach for Maxwell equations [1].
As a consequence, in Kinnersley tetrad Maxwell field is described only by one extremal component $\varphi_2$, and the Maxwell equations have closed-form solution [2]:
$\varphi_2= C \frac{e^{i\omega (t-\tilde{r}) + i m \phi }}{\sin\theta(r- i a \cos\theta)}...
