Ionization equilibrium and spectrum formation in QSOs' absorption regions

The behaviour of the primary and secondary components in a sample of double-lined Algol-type eclipsing binaries in the logg-logT _e diagram is analyzed. Our results indicate that the hotter components behave like normal Main-Sequence stars while the effect of irradiation may partly explain the overluminosity of the cool components.Paper presented at the 11th European Regional Astronomical Meetings of the IAU on New Windows to the Universe, held 3–8 July, 1989, Tenerife, Canary Islands, Spain.     

Entropy measure of stepwise component in GPS time series

A new method for estimating the stepwise component in the time series is suggested. The method is based on the application of a pseudo-derivative. The advantage of this method lies in the simplicity of its practical implementation compared to the more common methods for identifying the peculiarities in the time series against the noise. The need for automatic detection of the jumps in the noised signal and for introducing a quantitative measure of a stepwise behavior of the signal arises in the problems of the GPS time series analysis. The interest in the jumps in the mean level of the GPS signal is associated with the fact that they may reflect the typical earthquakes or the so-called silent earthquakes. In this paper, we offer the criteria for quantifying the degree of the stepwise behavior of the noised time series. These criteria are based on calculating the entropy for the auxiliary series of averaged stepwise approximations, which are constructed with the use of pseudo-derivatives.     

Pycnonuclear burning of 34Ne in accreting neutron stars

We study the pycnonuclear burning of ³⁴Ne in the inner crust of an accreting neutron star. We show that the associated energy production rate can be calculated analytically for any arbitrary temporal variability of the mass accretion rate. We argue that the theoretical time-scale for ³⁴Ne burning is currently very uncertain and ranges from a fraction of a millisecond to a few years. The fastest allowable burning may change the composition of the accreted crust while the slowest burning leads to a time-independent nuclear energy generation rate for a variable accretion. The results are important for constructing self-consistent models of the accreted crust and deep crustal heating in neutron stars which enter soft X-ray transients.     

On the explosive prevention of collisions of asteroidal and cometary bodies with the earth at their late detection

We consider the questions of an explosive impact on asteroids and comets that approach the Earth in the case of a late forecast of the dangerous situation. Based on models for the destruction of the material of a celestial body in the shock wave produced by a strong self-buried explosion, we estimate the radius of the destroyed region, the ejected mass, and the recoil momentum. We determine the charges needed to completely destroy bodies of various sizes and compositions or to divert bodies from the Earth by the required distance. When comets are dangerous bodies, we compare the efficiencies of the explosive and sublimation methods of changing their orbits. We discuss how to increase the efficiency of the explosive impact on a dangerous body through the use of a high relative velocity of the encounter between this body and a charge-carrying rocket.     

A VES-IP survey near the geophysical station of Moscow State University, in the Kaluga region

Due to the progress in instrumentation and methods in the most recent decade apparent resistance curves have been supplemented by accurate apparent chargeability curves at some frequencies up to an electrode spacing of 500 m. The comparison of the induced polarization frequency characteristics makes it possible to arrive at additional conclusions on the nature of anomalies. The results of vertical electrical and induced polarization sounding survey (VES-IP) that were carried out under the geophysical field studies of the Moscow State University are described.     

Afterburst thermal relaxation in neutron star crusts

We study thermal relaxation in a neutron star after internal heating events (outbursts) in the crust. We consider thin and thick spherically symmetric heaters, superfluid and non-superfluid crusts, stars with open and forbidden direct Urca processes in their cores. In particular, we analyze long-term thermal relaxation after deep crustal heating produced by nuclear transformations in fully or partly accreted crusts of transiently accreting neutron stars. This long-term relaxation has a typical relaxation time and an overall finite duration time for the crust to thermally equilibrate with the core. Neutron superfluidity in the inner crust greatly affects the relaxation if the heater is located in the inner crust. It shortens and unifies the time of emergence of thermal wave from the heater to the surface. This is important for the interpretation of observed outbursts of magnetars and transiently accreting neutron stars in quasi-persistent low-mass X-ray binaries.     

The 3D profile inversion of the MTS–MVS data by the example of the Shiveluch volcanic zone in the Kamchatka Peninsula

The joint use of the magnetovariational (MV) and magnetotelluric (MT) data and the a priori information about the areal distribution of the deep electrical conductivity within the studied area and the integral conductance of the sedimentary cover enabled us to conduct a three-dimensional (3D) inversion of these data and construct the 3D model of the northeastern part of Kamchatka. The results show that within the Shiveluch volcano, north and south of it, there are northwesterly striking conductive faults penetrating up to the mantle which ascends from a depth of 41 to 35 km. The electrical conductivity of these crustal structures which accommodate high seismic and volcanic activity is probably accounted for by fluid saturation.     

Heating and cooling of magnetars with accreted envelopes

We study the thermal structure and evolution of magnetars as cooling neutron stars with a phenomenological heat source in an internal layer. We focus on the effect of magnetized (   B ≳ 10¹⁴  G) non-accreted and accreted outermost envelopes composed of different elements, from iron to hydrogen or helium. We discuss a combined effect of thermal conduction and neutrino emission in the outer neutron star crust and calculate the cooling of magnetars with a dipole magnetic field for various locations of the heat layer, heat rates and magnetic field strengths. Combined effects of strong magnetic fields and light-element composition simplify the interpretation of magnetars in our model: these effects allow one to interpret observations assuming less extreme (therefore, more realistic) heating. Massive magnetars, with fast neutrino cooling in their cores, can have higher thermal surface luminosity.     

Effect of the disproportionation reaction of ferrous iron in impact-evaporation processes

Evidence for the disproportionation of iron was found in model experiments imitating impact melting, evaporation, and condensation. The experiments were carried out using a laser system at a characteristic temperature of ～3000–4000 K and a pulse duration of ～10^?3 s in a He atmosphere (P = 1 atm). Augite and mixtures of peridotite with MnO₂ and WO₃ were used as starting target materials. Experimental products (condensed vapor phase) were analyzed by X-ray photoelectron spectroscopy. The results of condensate analysis provided compelling evidence for the presence of iron in three oxidation states (Fe⁰, Fe²⁺, and Fe³⁺). In an experiment with augite, the proportions of iron species of different valences were similar to the stoichiometry of the disproportionation reaction. Similar evidence for this reaction was first found in a condensate from the samples of the fine fraction of the Luna 16 regolith. In the layers of the lunar condensate, the proportions of the valence states of iron were on average Fe⁰:Fe²⁺:Fe³⁺ = 1.2: 1.9: 0.7.     

Tidal flows in binary systems

The expressions of the tidal velocity in not very close binaries (double stars, the Sun and a planet, a planet and a satellite) are derived and applied in particular to white dwarfs and the giant planets of the solar system. The magnitude of the velocity on the surface of Jupiter is estimated to be about 0.5 cm s^?1. In white dwarfs the velocities of the order of tens m s^?1 may be encountered, and they can influence their evolution. The symmetry of the tidal flows is noted to be suitable for the magnetic field generation.