Том 63, № 2 (2019)

The algorithms often used for the interpretation of light curves, such as the frequently applied JKTEBOP algorithm, have limited accuracy, which causes rounding errors, and hence a non-physical contribution to the residuals (digital noise). The transit light curve of the binary HD 209458 is used as an example to demonstrate the need to take into account this digital noise. Improving the accuracy of lightcurve computations enables more reliable determination of whether the observed light curve is adequately described by a particular model, thanks to the elimination of the non-physical contribution to the residuals resulting from computational errors. A website where the algorithm developed can be obtained is given in the Conclusions.

The results of observations of the pulsar B0301+19 (J0304+1932) carried out on the Large Scanning Antenna of the Pushchino Radio Astronomy Observatory at 111 MHz during 2012–2017 are analyzed. The regular generation of powerful individual pulses at the longitudes of both components of the mean profile of the pulsar, classified as giant pulses, was observed. The most powerful of these pulses had a peak flux density of ≈935 Jy and a pulse energy of ≈6930 Jyms. The highest excess of the flux density relative to the value for the mean profile in a session was 93.7. The mean full width at half maximum of the most powerful giant pulse at was 2.8ms, with the width of the corresponding component in the mean profile being about 10 ms. The distributions of the peak flux densities and pulse energies of these anomalously strong pulses are complex, and cannot be reduced to a simple lognormal or power-law distribution over the entire range of values.

An analysis of data from three years of monitoring of interplanetary scintillations in 2015–2017 during a phase of decreasing solar activity is presented. The observations were carried out on the Large Scanning Antenna of the Lebedev Physical Institute at 111 MHz. During the period considered, the spatial distriution of the scintillation level was close to spherically symmetrical, on average, and did not undergo any strong time variations on scales of months or years. The monthly-mean scintillation level is not correlated with theWolf number.

Results of a study of the influence of solar-type host stars superflares on the gas dynamics of the extended envelopes of giant exoplanets are presented. During flare events, the radiation intensity of the host star in the extreme ultraviolet and soft X-ray can increase by several orders of magnitude for a short time, leading to strong local heating of the exoplanet atmosphere on the side facing the star, with the formation of shocks in the atmosphere. Computations of the gas-dynamical response of the atmosphere of the hot Jupiter HD 209458b to characteristic superflares of solar-like stars were carried out earlier in [1] using a one-dimensional aeronomical model correctly taking into account heating and chemical processes in the atmosphere. To investigate the outflow of atmospheric gas, the results obtained with this onedimensional model were used as simple boundary conditions for computations of the three-dimensional flow structure after a flare. The results of these three-dimensional gas-dynamical computations show that the mass ejection of the flare increases the size of the envelope over several hours, which could be detected with existing observing facilities. It is shown that the mass-loss rates for the most powerful superflare considered could be enhanced by an order of magnitude over several tens of hours after the flare.