Structure Of Satellite Systems Research Articles

Choosing the Structure of Satellite Systems for Meteorology and Forest Fire Detection on the Basis of a Vector Model of Surveying the Earth

A vector model of surveying the Earth has been used to show that the satellite systems that are considered should have an “equidistant” structure formed by equal shifts of orbital nodes by longitude and by the phase of satellites. The structure options have been compared using a computer program developed from the vector model of surveying the Earth that calculates all survey interruptions with their frequencies for the subsequent version of the satellite system in a split second. Analyzing all possible options, we have elaborated recommendations for choosing the structure of systems consisting of four meteorological satellites of METEOR-M-type and five or six satellites with wide-range infrared radiometers tested for the first time on the KANOPUS-V-IK satellite. An additional finding is that, in the variants at hand, the frequency of the maximum survey interruption, which is widely used as a criterion for the efficiency of the Earth observation systems, turned out to be less than 0.01. In view of this, we have concluded that the use of this criterion is impractical.

ON THE PERSISTENCE OF TWO SMALL-SCALE PROBLEMS IN ΛCDM

We investigate the degree to which the inclusion of baryonic physics can overcome two long-standing problems of the standard cosmological model on galaxy scales: (i) the problem of satellite planes around Local Group galaxies, and (ii) the "too big to fail" problem. By comparing dissipational and dissipationless simulations, we find no indication that the addition of baryonic physics results in more flattened satellite distributions around Milky-Way-like systems. Recent claims to the contrary are shown to derive in part from a non-standard metric for the degree of flattening, which ignores the satellites' radial positions. If the full 3D positions of the satellite galaxies are considered, none of the simulations we analyse reproduce the observed flattening nor the observed degree of kinematic coherence of the Milky Way satellite system. Our results are consistent with the expectation that baryonic physics should have little or no influence on the structure of satellite systems on scales of hundreds of kiloparsecs. Claims that the "too big to fail" problem can be resolved by the addition of baryonic physics are also shown to be problematic.