I. Novikov

Black Hole Physics: Basic Concepts and New Developments

Preface. I. Basic Concepts. 1. Introduction: Brief History of Black Hole Physics. 2. Spherically Symmetric Black Holes. 3. Rotating Black Holes. 4. Black Hole Perturbations (with N. Andersson). 5. General Properties of Black Holes. 6. Stationary Black Holes. 7. Physical Effects in the Gravitational Field of a Black Hole. 8. Black Hole Electrodynamics. 9. Astrophysics of Black Holes. II. Further Developments. 10. Quantum Particle Creation by Black Holes. 11. Quantum Physics of Black Holes. 12. Thermodynamics of Black Holes. 13. Black Holes in Unified Theories. 14. The Interior of a Black Hole. 15. Ultimate Fate of Black and White Holes. 16. Black Holes, Wormholes, and Time Machines. Conclusions. Appendices: A: Mathematical Formulas. B: Spherically Symmetric Spacetimes. C: Rindler Frame in Minkowski Spacetime. D: Kerr-Newman Geometry. E: Newman-Penrose Formalism. F: Wave Fields in a Curved Spacetime. G: Wave Fields in the Kerr Metric. H: Quantum Fields in Kerr Spacetime. I: Quantum Oscillator. Bibliography. Index.

Gauss - Legendre sky pixelization (GLESP) for CMB maps

A new scheme of sky pixelization is developed for CMB maps. The scheme is based on the Gauss–Legendre polynomials zeros and allows one to create strict orthogonal expansion of the map. A corresponding code has been implemented and comparison with other methods has been done.

Astrophysics of Black Holes

The black hole phenomenon is undoubtedly one of the most striking and intriguing of those predicted by theorists. However, a paramount question is: “Do black holes exist in the Universe, or are they only an abstract concept of the human mind?” In principle, a black hole could be built artificially. However, this meets such grandiose technical difficulties that it looks impossible, at least in the immediate future. In fact, the artificial construction of a black hole looks even more problematic than an artificial creation of a star. Thus, we have to conclude that the physics of black holes, as well as the physics of stars, is the physics of celestial bodies. Stars definitely exist, but what may one say about the existence of astrophysical black holes?

The appearance of highly relativistic, spherically symmetric stellar winds

A nonluminous, steady state, spherically symmetric, relativistic wind, with the opacity dominated by electron scattering appears against a bright background as a dark circle with the radius rd. A luminous wind would appear as a bright spot with a radius rl = rd/2 pi gamma exp 3, where gamma is the Lorentz factor of the wind. The bright wind photosphere is convex for v equal to or less than 2c/3, and appears concave for higher outflow velocities. 5 refs.

Generalizations of the Kerr and Kerr-Newman metrics possessing an arbitrary set of mass-multipole moments

The authors present in a concise analytical form two asymptotically flat metrics describing the superposition of the Kerr solution with an arbitrary static vacuum Weyl field which differ in their angular momentum distributions. They are then used for the construction of two asymptotically flat generalizations of the Kerr-Newman spacetime possessing the full set of mass-multipole moments able to describe the exterior gravitational field of a charged rotating arbitrary axisymmetric mass.

Astrophysics of Wormholes

We consider the hypothesis that some active galactic nuclei and other compact astrophysical objects may be current or former entrances to wormholes (WHs). A broad mass spectrum for astrophysical WHs is possible. We consider various new models of the static WHs including WHs maintained mainly by an electromagnetic field. We also discuss observational effects of a single entrance to WH and a model for a binary astrophysical system formed by the entrances of WHs with magnetic fields and consider its possible manifestation.

A New Model of a Tidally Disrupted Star

A new semianalytical model of a star evolving in a tidal —eld is proposed. The model is a gener- alization of the so-called affine stellar model. In our model the star is composed of elliptical shells with diUerent parameters and diUerent orientations depending on time and on the radial Lagrangian coordi- nate of the shell. The evolution equations of this model are derived from the virial relations under certain assumptions, and the integrals of motion are identi—ed. It is shown that the evolution equations can be deduced from a variational principle. The evolution equations are solved numerically and com- pared quantitatively with the results of three-dimensional numerical computations of the tidal interaction of a star with a supermassive black hole. The comparison shows very good agreement between the main ii integral ˇˇ characteristics describing the tidal interaction event in our model and in the three- dimensional computations. Our model is eUectively a one-dimensional Lagrangian model from the point of view of numerical computations, and therefore it can be evolved numerically 102¨103 times faster than the three-dimensional approach allows. This makes our model well suited for intensive calculations covering the whole parameter space of the problem. Subject headings: black hole physicscelestial mechanics, stellar dynamicshydrodynamics

The Gauss-Legendre Sky Pixelization for the CMB polarization (GLESP-pol). Errors due to pixelization of the CMB sky

We present the development of the method for numerical analysis of polarization in the Gauss–Legendre sky pixelization (GLESP) scheme for CMB maps. This incorporation of the polarization transforms in the pixelization scheme GLESP completes the creation of our new method for numerical analysis of CMB maps. A comparison of GLESP and HEALPix calculations is done.

Strong effects during close encounters of a star with a massive black hole

Using a three-dimensional Eulerian hydrodynamical code we consider close encounters of a star with a massive black hole that are accompanied by stripping of matter from the star, or disruption of it. An estimate is made of the critical pericentric distance at which the deposited energy is equal to the binding energy of the stellar model. Stripping of the outer layers and strong squeezing of the star by tidal forces are discussed

PASSAGE OF RADIATION THROUGH WORMHOLES

We investigate numerically the process of the passage of a radiation pulse through a wormhole and the subsequent evolution of the wormhole that is caused by the gravitational action of this pulse. The initial static wormhole is modeled by a spherically symmetrical solution with zero mass. The radiation pulses are modeled by spherically symmetrical shells of self-gravitating massless scalar fields. We demonstrate that the compact signal propagates through the wormhole and investigate the dynamics of the fields in this process for both cases: collapse of the wormhole into the black hole and for the expanding wormhole.