Stars: From Collapse to Collapse
In 2016 the leading center of Russian ground-based observational astronomy, the Special Astrophysical Observatory of the Russian Academy of Sciences, celebrated its 50th anniversary. As part of the anniversary celebration, the Observatory organized a conference to discuss a broad range of topics related to the astrophysics of stars and star systems, which brought together the leading experts from Russia, the Russian Commonwealth, and our foreign colleagues. The main idea of the meeting is reflected in its name: the life of a star from its birth (molecular cloud collapse) to death (supernova core collapse). The result of the conference is the present volume containing the latest achievements of the Russian astronomical community in stellar astrophysics, obtained both with domestic instruments and as part of international cooperation. This volume presents recent results of the studies of star-forming regions and the interstellar medium, stellar atmospheres and magnetism, activity of stars, multiple stellar systems and exoplanets, and stars after the nuclear burning stage. Methods and instruments of present-day stellar astrophysics are also discussed.
The process of the plasma ejection formation from the accreting neutron star is investigated. Magnetocavitation model of this process is suggested. According to this model, the plasma ejection is produced because of the magnetospheric destruction associated with the processes of the neutron star quake, resonant interaction of magnetosphere with the accreted plasma and actions of the shock waves from the accretion disk of the neutron star. The suggested model imposes some restrictions on the ejection parametres, nevertheless, the estimations of the ejection parametres obtained in this research are in accordance with the observational data.
The interaction of the supersonic gas jet from a young star with the surrounding interstellar medium is studied. Based on the law of energy conservation, simple estimates for the jet and ambient medium parameters in the region of their interaction are obtained. These estimates agree with the observational data for such regions.