This paper considers latest highlights in simultaneous and follow-up optical observations of high energy astrophysical phenomena by MASTER Global Robotic Net. Such extreme Universe sources includes gamma-ray bursts, gravitational wave events, detected by LIGO/Virgo, fast radio bursts, high energy neutrino sources and others. Some of the neutrinos detected by ground-based facilities owe their births to supermassive black holes – blazars, which are in a special anxious state with high statistical reliability. We discovered the effect of a rapid decrease in the brightness of the blazar PKS 0735+17 at the time of the multiple detection of the high-energy neutrino event IceCube-211208A. This decrease in brightness within several hours was detected with a high confidence (SNR 10) in comparison with a multi-day brightening state of the blazar, which was accompanied not only by a maximum increase in the average brightness, but also by an increase in the amplitude of its brightness fluctuations. Additionally, we analyzed all cases of successful observation of blazars around neutrino events and obtained statistically reliable indications of the relationship between neutrino events and optical activity of blazars in the doubled error box at the 4.2 σ level.

Recent observational data on the type Ia supernova rates are in excellent agreement with the earlier results of the population synthesis of binary stars and confirm that the overwhelming majority of type Ia supernovas (∼99%) in elliptical galaxies form via mergers of binary white dwarfs with a total mass exceeding the Chandrasekhar limit.

Hard X-ray INT observations of SS 433 carried out during 2003-2005 years with an analysis of precessional and orbital variability is presented. The width of X-ray eclipse in the 25-50 keV range at the precessional phase ψ=0.1 (accretion disk is open to observer) is higher than that in the Ginga 18.4-27.6 keV range. This fact suggests existance the presence of hot extended corona around the supercritical accretion disk. Spectrum of hard X-rays in the range 10-200 keV does not change with the precessional phase which also suggests that hard X-ray flux is generated in the hot extended corona around the accretion disk. The parameters of this hot corona are: kT=23-25 keV, τ= 1.8-2.8. Mass ratio estimated from the analysis of the ingress part of the eclipse light curve is in the range q=m_x/m_v=0.3-0.5.

Results of simultaneous INTEGRAL and optical observations of the galactic microquasar SS433 in May 2003 and INTEGRAL / RXTE observations in March 2004 are presented. Persistent precessional variability with a maximum to minimum uneclipsed hard X- ray flux ratio of similar to 4 is discovered. The 18 - 60 keV X- ray eclipse is found to be in phase with optical and near infrared eclipses. The orbital eclipse observed by INTEGRAL in May 2003 is at least two times deeper and apparently wider than in the soft X- ray band. The broadband 2 - 100 keV X- ray spectrum simultaneously detected by RXTE/ INTEGRAL in March 2004 can be explained by bremsstrahlung emission from optically thin thermal plasma with kT similar to 30 keV. Optical spectroscopy with the 6- m SAO BTA telescope confirmed the optical companion to be an A5 - A7 supergiant. For the first time, spectorscopic indications of a strong heating effect in the optical star atmosphere are found. The measurements of absorption lines which are presumably formed on the non- illuminated side of the supergiant yield its radial velocity semi- amplitude K-v = 132 9 kms(-1). The analysis of the observed hard X- ray light curve and the eclipse duration, combined with the spectroscopically determined optical star radial velocity corrected for the strong heating effect, allows us to model SS433 as a massive X- ray binary. Assuming that the hard X- ray source in SS433 is eclipsed by the donor star that exactly fills its Roche lobe, the masses of the optical and compact components in SS433 are suggested to be M-v approximate to 30 M-circle dot and M-x approximate to 9 M-circle dot, respectively. This provides further evidence that SS433 is a massive binary system with supercritical accretion onto a black hole.

Results of simultaneous INTEGRAL and optical observations of galactic microquasar SS433 in May 2003 are presented. The analysis of the X-ray and optical eclipse duration and hard X-ray spectra obtained by INTEGRAL together with optical spectroscopy obtained on the 6-m telescope allows us to construct a model of SS433 as a massive X-ray binary. Xray eclipse in hard X-rays has a depth of ∼ 80% and extended wings. The optical spectroscopy allows us to identify the optical companion as a A5-A7 supergiant and to measure its radial velocity semiamplitude Kv = 132 km/s. A strong heating effect in the optical star atmosphere is discovered spectroscopically. The observed broadband X-ray spectrum 2-100 keV can be described by emission from optically thin thermal plasma with kT ∼ 15 − 20keV

Results of simultaneous {\it INTEGRAL} and optical observations of galactic microquasar SS433 in May 2003 are presented. The analysis of the X-ray and optical eclipse duration and hard X-ray spectra obtained by {\it INTEGRAL} together with optical spectroscopy obtained on the 6-m telescope allows us to construct a model of SS433 as a massive X-ray binary. X-ray eclipse in hard X-rays has a depth of $\sim 80%$ and extended wings. The optical spectroscopy allows us to identify the optical companion as a A5-A7 supergiant and to measure its radial velocity semi-amplitude $K_v=132$ km/s. A strong heating effect in the optical star atmosphere is discovered spectroscopically. The observed broadband X-ray spectrum 2-100 keV can be described by emission from optically thin thermal plasma with $kT\sim 15-20 keV$

The binary relativistic stars merge rate in the Universe is determined mostly by the evolutionary scenario of the binary stars. Some of the unknown parameters of this scenario can be estimateted by the comparison of population synthesis predictions with the actually observed galactic population. We performed the Scenario Machine simulations with a revised scenario model and obtained that the lower estimate of the binary black hole merger rate should be similar to 7 times higher than was given before.

Observations of SS433 by INTEGRAL carried out in March-May 2003 are presented. SS433 is evidently detected on the INTEGRAL images of the corresponding sky region in the energy bands 25-50 and 50-100 keV. The precessional variability of the hard X-ray flux is clearly seen. The X-ray eclipse caused by the binary orbital motion is also detected. A possible origin of the hard continuum is briefly discussed.

We compute the GRB rates in different types of galaxies by performing a population synthesis using the "Scenario Machine" code in the framework of merging binary relativistic stars model. Our model predicts that similar to 1/3 of GRB should occur in elliptical galaxies, and this fraction should increase with the redshift. This fraction is comparable with the observed fraction of GRB without (detectable) X-ray afterglows.

We present the results of the population synthesis of the population ofthe supernovae progenitors. Both single and double degenerate progenitorsof SN Ia are considered. We compute the cosmic rate histories for SN I,SN II and both classes of SN Ia, and present them in the form of redshiftand magnitude distributions. These results can be compared with observationaldata, allowing to estimate the star formation rate history and thecosmological parameters including ω baryons which cannot beestimated from analysing the Hubble diagrams of supernovae.We find that single degenerate (SD) SN Ia are younger than double degenerate (DD) ones, and so the SN Ia in elliptical galaxies should be mostly DD.We propose to use the redshift dependence of relative supernovae rates indifferent types of galaxies, or of different supernovae types forinterpretation of observations. These relative rates should be lessinfluenced by the selection effects than the absolute ones.

The prospects of detecting extragalactic supernovae (SNs) down to visual magnitudes 23-25 give us hope for observing them in the most distant parts of the universe. Using a Monte Carlo method of stellar population synthesis (the Scenario Machine), we compute, under standard assumptions of stellar evolution, the rates of SNs of various types in a model galaxy and evaluate the SN rates in the universe. The expected cumulative distribution log N - m (number of events - stellar magnitude) is calculated for various SN types and different star formation histories in the universe. The results are also presented in terms of evolution of supernova units with redshifts. Recent observational data on the high-redshift SN Ia rate are in good agreement with our predictions for the relative density of baryons contained in stars at the present time (Omega* = 0.0057).

The possible low-frequency radio emission from the progenitors of gamma ray bursts can experience a delay from tens of seconds to hours on the way to the observer due to the dispersion in galactic and extragalactic plasma, and thus reach the observer as a radio afterglow of the burst. This opens a unique possibility (peculiar “time machine”) of seeing what happened at that place before the catastrophe.

We examine and develop the model of gamma ray bursts origin proposed by Shaviv and Dar (astro-ph/9606032), according to which the strong gamma ray emission is produced by the interaction of the baryonic relativistic jet (outflow) with the soft photon field in a dense stellar region. It is shown by the simulations of the burst profiles that these profiles are very sensitive to the jet geometry, and the 'clarity' of the GRB profile is (in this model) somehow connected with the gamma rays beaming. Also some event-rate based restrictions are derived and discussed.

A view of the sky seen in gravitational waves (GW) in a wide frequency range (∼ 10−9–103 Hz) is considered. Stochastic gravitational wave background (GWB) produced by binary systems, both galactic and extragalactic in origin, studied in more detail. Critical frequencies above which the galactic and extragalactic GWB becomes transparent for a GW detector with 1° angular resolution are about 2 × 10−3 Hz and ∼ 10 Hz, respectively. A realistic “map” of the GW sky is constructed based on realistic matter distribution within a distance of ∼ 50 Mpc according to Tully's Catalogue of Nearby Galaxies. Rates of coalescence of binary neutron stars (NS) and of supernova explosions for these galaxies are about 3 and 40 per year, respectively. The calculated rate of binary NS merging, about 10−4 per year per 1011 M[odot], yields ∼ 103 events for a LIGO limiting sensitivity hc ≃ 10−21.9 at the frequency 100 Hz.

We present a WWW-version of the {\it Scenario Machine} - a computer code designed to calculate the evolution of close binary stellar systems. The Internet users can directly access to the code and calculate binary evolutionary tracks with parameters at the user's will. The program is running on the {\it Pentium} server of the Division of the Relativistic Astrophysics of the Sternberg Astronimical Institute (this http URL ). The results are presented both in the form of tables and graphic diagrams. The work is always in progress. More possibilities for Internet users are intended to become available in the near future.

We present a WWW-version of the Scenario Machine-a computer code designed to calculate the evolution of close binary stellar systems. The In-ternet users can directly access to the code and calculate binary evolutionary tracks with parameters at the user's will. The program is running on the Pentium server of the Division of the Relativistic Astrophysics of the Stern-berg Astronimical Institute (http://xray.sai.msu.su/). The results are presented both in the form of tables and graphic diagrams. The work is always in progress. More possibilities for Internet users are intended to become available in the near future.

Binary neutron stars mergers that are expected to be the most powerful source of energy in the Universe definitely exist in nature, as is proven by the observed behavior of the Hulse-Taylor binary radio pulsar. Though most of energy in such events is radiated in gravitational waves, there probably exist several mechanisms giving also electromagnetic radiation. We propose a new one, involving a revival of the radio pulsar several orbital cycles before the merger.