793 research outputs found
Details of the spatial structure and kinematics of the Castor and Ursa Major streams
A list of the Castor stream members is compiled based on the data from
various authors. The membership probabilities for some stars are revised based
on the individual apex, multiplicity, observational errors, and peculiarity.
The apex of the Castor moving group is determined using the apex diagram
method. The parameters of the Castor and Ursa Major streams are compared and
the positions of the two streams on the apex diagram are found to differ by
225deg, implying that the two groups move in almost opposite directions. Stars
of both moving groups are intermixed in space, the Castor stream occupies a
smaller volume than the UMa stream and is located inside it. Our results can be
useful for understanding the morphology of the Galactic disk in the Sun's
vicinity
Radial velocity dispersions of star groups in M 67
High-precision measurements of radial velocities of the M 67 cluster members
are used to calculate the radial-velocity dispersions in the stellar groups
found earlier in the cluster's corona. The previously detected feature in one
of the groups (Group 60) consisting of stars with almost identical space
velocities was confirmed. The possibility of more accurate future studies of
the parameters of star groups using the Gaia catalogues is discussed.Comment: 7 pages, 2 figure
Algorithmic statistics: forty years later
Algorithmic statistics has two different (and almost orthogonal) motivations.
From the philosophical point of view, it tries to formalize how the statistics
works and why some statistical models are better than others. After this notion
of a "good model" is introduced, a natural question arises: it is possible that
for some piece of data there is no good model? If yes, how often these bad
("non-stochastic") data appear "in real life"?
Another, more technical motivation comes from algorithmic information theory.
In this theory a notion of complexity of a finite object (=amount of
information in this object) is introduced; it assigns to every object some
number, called its algorithmic complexity (or Kolmogorov complexity).
Algorithmic statistic provides a more fine-grained classification: for each
finite object some curve is defined that characterizes its behavior. It turns
out that several different definitions give (approximately) the same curve.
In this survey we try to provide an exposition of the main results in the
field (including full proofs for the most important ones), as well as some
historical comments. We assume that the reader is familiar with the main
notions of algorithmic information (Kolmogorov complexity) theory.Comment: Missing proofs adde
Pair plasma relaxation time scales
By numerically solving the relativistic Boltzmann equations, we compute the
time scale for relaxation to thermal equilibrium for an optically thick
electron-positron plasma with baryon loading. We focus on the time scales of
electromagnetic interactions. The collisional integrals are obtained directly
from the corresponding QED matrix elements. Thermalization time scales are
computed for a wide range of values of both the total energy density (over 10
orders of magnitude) and of the baryonic loading parameter (over 6 orders of
magnitude). This also allows us to study such interesting limiting cases as the
almost purely electron-positron plasma or electron-proton plasma as well as
intermediate cases. These results appear to be important both for laboratory
experiments aimed at generating optically thick pair plasmas as well as for
astrophysical models in which electron-positron pair plasmas play a relevant
role.Comment: Phys. Rev. E, in pres
Electromagnetic field of a charge asymptotically approaching spherically symmetric black hole
We consider a test charged particle falling onto a Schwarzschild black hole
and evaluate its electromagnetic field. The Regge-Wheeler equation is solved
analytically by approximating the potential barrier with Dirac delta function
and rectangular barrier. We show that for asymptotically large time measured by
a distant observer the electromagnetic field approaches the spherically
symmetric electrostatic field exponentially fast. This implies that in the
region accessible to a distant observer the initial state of separated charge
and Schwarzschild black hole becomes asymptotically indistinguishable from the
Reisnner-Nordstr\"om solution. Implications of this result for models with
plasma accretion on black holes are discussed.7 aComment: 7 pages, 2 figure
Electromagnetic radiation and electromagnetic self-force of a point charge in the vicinity of Schwarzschild black hole
Point charge, radially moving in the vicinity of a black hole is considered.
Electromagnetic field in wave zone and in the small neighbourhood of the charge
is calculated. Numerical results of the calculation of the spectrum of
electromagnetic radiation of the point charge are presented. Covariant approach
for the calculation of electromagnetic self-force is used for the case of the
slowly moving charge. Numerical results for the self-force in the case of slow
motion of the particle are obtained and compared to the results in literature.Comment: 5 pages, 3 figure
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