In this work we present a close correlation between third Kepler law and Titius-Bode empirical rule. Concretely, we demonstrate that third Kepler law, or, corresponding equilibrium condition between centrifugal and Newtonian gravitational force, impl
ies that planet orbital momentum becomes effectively a function of the planet distance as unique variable and vice versa. Then, approximation of the planet distance by its first order Taylor expansion over planet orbital momentum holds an exponential form corresponding to Titius-Bode rule. In this way it is not necessary postulate exponential form of the planet distance (as it has been done by Scardigli) but only discrete values of its argument. Physically, it simply means that, in the linear approximation, quantized planets orbital momentums do a geometrical progression.
In this work we do an interpolation of Scardigli theory of a quantum-like description of the planetary system that reproduces remarkable Titius-Bode-Richardson rule. More precisely, instead of simple, approximate, Bohr-like theory, or, accurate, Schr
$ddot{o}$dinger-like theory, considered by Scardigli, we suggest originally a semi-accurate, de Broglie-like description of the planetary system. Especially, we shall propose a de Broglie-like waves in the planetary systems. More precisely, in distinction from Scardigly (which postulated absence of the interference phenomena at planet orbits) we shall prove that, roughly speaking, planets orbits equal a sum of natural numbers of two types, large and small, of the de-Broglie-like waves. It is similar to well-known situation in atomic physics by interpretation of Bohr momentum quantization postulate by de Broglie relation.
Generalizing results of our previous work (where classical kinetic energy has been used) in this work (where ultra-relativistic kinetic energy is used) we suggest an original variant of the determination of minimal length (corresponding to Plank leng
th) by formation of a microscopic (tiny) black hole. Like to some previous authors we use Heisenberg coordinate-momentum uncertainty relation, on the one hand. But, instead of metric fluctuation (obtained by second derivative in Einstein equations) that generalizes uncertainty relation by an additional term, used by previous authors, we use Hawking temperature of the black hole and standard Heisenberg coordinate-momentum uncertainty relation.
In this work we suggest a simple model of the cosmological constant as the coefficient of the quantum tunneling of vacuum fluctuations (with wave length larger than Planck length) at tiny, boundary spherical shell of the universe (with thickness equi
valent to Planck length and radius equivalent to scale factor). Roughly speaking, given fluctuations can, by quantum tunneling (i.e. scattering with a potential barrier with highness equivalent to Planck energy and width proportional to, approximately, three hundred Planck length) leave universe and arrive in its exterior, i.e. multi-universe (in sense of Linde chaotic inflation theory universe can be considered as a causally-luminally connected space domain while its exterior can be considered as a space domain without causal-luminal connections with universe). It is in full agreement with usual quantum mechanics and quantum field theory as well as WMAP observational data (especially fine tuning condition).
In this work we present a generalized Laplace method for a formal, simple, quasi-classical, determination of the outer and inner horizon radius of Kerr-Newman black hole. We consider classical gravitational interaction between a thin, with homogeneou
sly distributed mass and electric charge, spherical (black) shell and a probe particle. Also, we use relativistic equivalence principle. Finally we suppose that probe particle propagates radially to shell with speed of light while tangentially it rotates in common with shell, so that total energy of a probe particle equals zero.
In this work we present a simple, approximate method for analysis of the basic dynamical and thermodynamical characteristics of Kerr-Newman black hole. Instead of the complete dynamics of the black hole self-interaction we consider only such stable (
stationary) dynamical situations determined by condition that black hole (outer) horizon circumference holds the integer number of the reduced Compton wave lengths corresponding to mass spectrum of a small quantum system (representing quant of the black hole self-interaction). Then, we show that Kerr-Newman black hole entropy represents simply the quotient of the sum of static part and rotation part of mass of black hole on the one hand and ground mass of small quantum system on the other hand. Also we show that Kerr-Newman black hole temperature represents the negative value of the classical potential energy of gravitational interaction between a part of black hole with reduced mass and small quantum system in the ground mass quantum state. Finally, we suggest a bosonic great canonical distribution of the statistical ensemble of given small quantum systems in the thermodynamical equilibrium with (macroscopic) black hole as thermal reservoir. We suggest that, practically, only ground mass quantum state is significantly degenerate while all other, excited mass quantum states are non-degenerate. Kerr-Newman black hole entropy is practically equivalent to the ground mass quantum state degeneration. Given statistical distribution admits a rough (qualitative) but simple modeling of Hawking radiation of the black hole too.
In our previous work we suggested a very simple, approximate formalism for description of some basic (especially thermodynamical) characteristics of a non-charged, rotating, very thin black ring. Here, in our new work, generalizing our previous resul
ts, we suggest a very simple, approximate description of some basic (especially thermodynamical) characteristics of a weakly charged, rotating, very thin black ring. (Our formalism is not theoretically dubious, since, at it is not hard to see, it can represent an extreme simplification of a more accurate, e.g. Copeland-Lahiri, string formalism for the black hole description.) Even if suggested formalism is, generally speaking, phenomenological and rough, obtained final results, unexpectedly, are non-trivial. Concretely, given formalism reproduces exactly Bekenstein-Hawking entropy, Bekenstein quantization of the entropy or horizon area and Hawking temperature of a weakly charged, rotating, very thin black ring originally obtained earlier using more accurate analysis by Emparan, Aestefanesei, Radu etc. (Conceptually it is similar to situation in Bohrs atomic model where energy levels are determined practically exactly even if electron motion is described roughly.) Our formalism is physically based on the assumption that circumference of the horizon tube holds the natural (integer) number of corresponding reduced Comptons wave length. (It is conceptually similar to Bohrs quantization postulate in Bohrs atomic model interpreted by de Broglie relation.) Also, we use, mathematically, practically only simple algebraic equations.
In this work, starting by simple, approximate (quasi-classical) methods presented in our previous works, we reproduce effectively and generalize final results of Herdeiro and Rebelo on the basic thermodynamical characteristics (entropy and temperatur
e) of two interacting Kerr black holes (in touching limit) obtained recently by accurate analysis. Like as it has been done in our previous works, we simply suppose that circumference of the horizon of total black hole (that includes two or, generally, a crystal lattice of many interacting Kerr black holes in touching limit, without angular momentum) holds integer number of reduced Compton wave lengths corresponding to mass spectrum of a small quantum system captured at horizon. (Obviously it is conceptually analogous to Bohr quantization postulate interpreted by de Broglie relation in Old, Bohr-Sommerfeld, quantum theory.) It, by simple mathematical methods, first neighbour approximation of the black holes interaction and first thermodynamical law, implies mentioned basic thermodinamical characteristic of the total black hole as well as any its part, i.e. single black hole. Especially, it is shown that, in limit of increasing number of the black holes, entropy and horizon surface of the total black hole stand observables of the discrete spectrum while entropy and horizon surface of the single black hole tends toward observables of the continuous spectrum.
In this work, starting by simple, approximate (quasi-classical) methods presented in our previous works, we suggest a simple determination of the (logarithmic) corrections of (Schwarzschild) black hole entropy without knowing the details of quantum g
ravity(Fursaev). Namely, in our previous works we demonstrated that all well-known important thermodynamical characteristics of the black hole (Bekenstein-Hawking entropy, Bekenstein entropy/surface quantization and Hawking temperature) can be effectively reproduced starting by simple supposition that black hole horizon circumference holds integer number of reduced Compton wave lengths corresponding to mass (energy) spectrum of a small quantum system. (Obviously it is conceptually analogous to Bohr quantization postulate interpreted by de Broglie relation in Old, Bohr-Sommerfeld, quantum theory.) Especially, black hole entropy can be presented as the quotient of the black hole mass and the minimal mass of small quantum system in ground mass (energy) state. Now, we suppose that black hole mass correction is simply equivalent to negative classical potential energy of the gravitational interaction between black hole and small quantum system in ground mass (energy) state. As it is not hard to see absolute value of the classical potential energy of gravitational interaction is identical to black hole temperature. All this, according to first thermodynamical law, implies that first order entropy correction holds form of the logarithm of the surface with coefficient -0.5. Our result, obtained practically quasi-classically, without knowing the details of quantum gravity, is equivalent to result obtained by loop quantum gravity and other quantum gravity methods for macroscopic black holes.
In this work we suggest a very simple, approximate formalism for description of some basic (especially thermodynamical) characteristics of a rotating, very thin black ring. (In fact, our formalism is not theoretically dubious, since, at it is not har
d to see, it can correspond to an extreme simplification of a more accurate, Copeland-Lahiri string formalism for the black hole description.) Even if suggested formalism is, generally speaking, phenomenological and rough, obtained final results, unexpectedly, are non-trivial. Concretely, given formalism reproduces exactly Bekenstein-Hawking entropy, Bekenstein quantization of the entropy or horizon area and Hawking temperature of a rotating, very thin black ring obtained earlier using more accurate analysis by Reall, Emparan, Elvang, Virmani etc. (Conceptually it is similar to situation in Bohrs atomic model where energy levels are determined practically exactly even if electron motion is described roughly.) Our formalism, according to suggestions in our previous works, is physically based on the assumption that circumference of the horizon tube holds the natural (integer) number of corresponding reduced Comptons wave length. (It is conceptually similar to Bohrs quantization postulate in Bohrs atomic model interpreted by de Broglie relation.) Also, we use, mathematically, practically only simple algebraic equations (by determination of Hawking temperature we use additionally only simple differentiation of Smarr relation).
