The Mach's Principle and Large-scale Modification of Newtonian Gravitation as Alternative Approach to Cold Dark Matter and Dark Energy

We take a heterodox approach to the ΛFRW Cosmology starting from the modification of Newtonian gravity by explicitly incorporating Mach's Principle through an additional term a great scale in the gravitation. The results show that at the after of the matter-radiation decoupling, the distribution of matter at scales greater than 10Mpc contributes with an inverse Yukawa-like field, which verifies the observations: resulting null in the inner solar system, weakly attractive in ranges of interstellar comoving distances, very attractive in comoving distance ranges comparable to the clusters of galaxies, and repulsive in cosmic scales. This additional term explains dark energy, removes the incompatibility between the density of matter and the flatness of the universe; and also allows the theoretical deduction of the Hubble-Lemaitre Law. Additionally, Birkhoff Theorem, Virial Theorem, the missing mass of Zwicky, the BAO, gravitational redshift are discussed. It is concluded that the dark energy and the missing mass can be approached with the usual physics if a classical, large-scale modification of the Inverse Square Law.

On the Equivalence of Physical Theories

This chapter argues against formal accounts of theoretical equivalence in physics. It defends the importance of a theory’s picture of the world and its explanations of the phenomena, drawing on examples from classical physics, Newtonian gravitation, classical electromagnetism, special relativity, and quantum mechanics. The discussion draws a distinction between metaphysical equivalence and informational equivalence and argues that these are equally important to the equivalence of physical theories. The chapter concludes that there are fewer cases of wholly equivalent theories in physics than usually thought. However, this is not a problem, for it is still possible to talk about the various respects in which physical theories are, or are not, equivalent to one another.

Нeat transfer processes in the gas placed into a newtonian gravitation field

In this paper, using the theoretical and numerical investigation of molecular motion, we study heat transfer processes in the gas placed in a Newtonian gravitational field. The influence of gravity on the heat conductivity of the gas is analyzed. The gravity considered is more than 100 000 times higher than that of the Earth. The main differences of the gas heat conductivity under such high gravity from the one detected under normal gravity are demonstrated and explained. It is shown how the thermal equilibrium for the heat conductivity of the gas depends on gravity and the type of gas. The difference between natural gravity and the centrifugal force is discussed. It is shown how the gas density influences the thermal equilibrium for the heat conductivity under a strong centrifugal force. The convective heat transfer in the gas placed into a gravitational or centrifugal field is analyzed. It is shown that the thermal equilibrium of the convective heat transfer under intensive gravity is not the same as under normal gravity. The horizontal convection mechanism is discussed. A technical way of the realization of gravity thermal effects in the gas is represented. All necessary parameters of the experimental setup are given.

Nonlinear Fokker–Planck Equation Approach to Systems of Interacting Particles: Thermostatistical Features Related to the Range of the Interactions

Nonlinear Fokker–Planck equations (NLFPEs) constitute useful effective descriptions of some interacting many-body systems. Important instances of these nonlinear evolution equations are closely related to the thermostatistics based on the S q power-law entropic functionals. Most applications of the connection between the NLFPE and the S q entropies have focused on systems interacting through short-range forces. In the present contribution we re-visit the NLFPE approach to interacting systems in order to clarify the role played by the range of the interactions, and to explore the possibility of developing similar treatments for systems with long-range interactions, such as those corresponding to Newtonian gravitation. In particular, we consider a system of particles interacting via forces following the inverse square law and performing overdamped motion, that is described by a density obeying an integro-differential evolution equation that admits exact time-dependent solutions of the q-Gaussian form. These q-Gaussian solutions, which constitute a signature of S q -thermostatistics, evolve in a similar but not identical way to the solutions of an appropriate nonlinear, power-law Fokker–Planck equation.

Yarkovsky Effect on the Orbital Dynamics of 1566 Icarus Asteroid

The orbital dynamic of small objects is an n-body problem that can not be solve by analitically, it is needed to use numerical integration to find the solution instead. This work is about orbital dynamic of asteroid 1566 Icarus under Classical Newtonian gravitation and if thermal effect (Yarkovsky effect) is included. Yarkovsky Effect is a thermal radiation force resulted from time span of small rotating objects to receive heat from the Sun and then re-radiates it. The Yarkovsky Effect is working optimum for objects with diameter from 10 cm up to 10 km, and now is implemented to Asteroid 1566 Icarus with diameter 1.3 km which are member of Apollo and Earth crosser object. This Asteroid is called Earth crosser due to its orbit is crossing Earth’s orbit. With semi major axis a  1.078 au and eccentricity e  0.827, asteroid 1566 Icarus has perihelion distance q = 0.18674 au or less than semi major axis of Mercury. Due to that reason, Yarkovsky effect was considered to be applied on the orbital dynamics of asteroid 1566 Icarus. Due to sensitivity in input-data of numerical integration for n-body, one hundred simulation preliminary data were made as input in numerical integration process, therefore, 100 clones of Asteroid 1566 Icarus are gathered. Cloning process was conducted by using random number from Asteroid 1566 Icarus orbital elements at epoch 2456800.5 (23 May 2014) to standard deviation . The integration then later conducted within 105 years time span from the epoch. The result shown that the orbital dynamics of asteroid 1566 Icarus with Yarkovsky effect is still within the range of 100 clones of asteroid 1566 Icarus. Thereby, within 105 years, Yarkovsky effect does not change the orbital dynamic of asteroid 1566 Icarus globally, except for two phenomenon between close encounter with planet.