We will address the existence of a new symmetry for an imperfect
fluid by introducing local four-velocity gauge-like transformations for the case when there is vorticity^1. A similar tetrad formulation as to the Einstein-Maxwell spacetimes formalism presented in previous manuscripts^2,3 will be developed in this manuscript for the imperfect fluids. The four-velocity curl and the metric...
The formalism of the Kinetic Theory of Relativistic Gases provides a geometrical framework to obtain the distribution function of the matter components. Such distribution function possesses the symmetries of the space-time in which it is embedded. In this talk we present the distribution function for a matter component in a Friedmann-Robertson-Walker (FRW) universe. Once the more general...
When simulating relativistic gas flows, complex flows are often formed in zones that are much smaller than the entire calculation domain. The processes that take place outside such zones may greatly affect not only the behavior but also the formation of the complex flows. The use of adaptive mesh refinement technique is a universal method of domain discretization in computing such multi-scale...
Spherical collapse in general relativity has been studied with different methods, especially by using a priori given equations of state that describe the collapsing matter as a perfect fluid. We propose an alternative perspective, in which the initial density of the perfect fluid is given as a polynomial function of the radial coordinate that is regular everywhere inside the fluid. We then...
According to theoretical estimates, our Galaxy contains about 100 million black holes, a large majority of which should be isolated. Yet, not a single isolated black hole had ever been unambiguously detected. After a brief review of the subject, the powerful technique of astrometric microlensing to detect isolated stellar mass black holes will be described. We used this novel technique of...
This study explored the behavior of the $f(T, \mathcal{T})$ cosmological model with the use of various data set combinations. We also compared the results for this model between the Pantheon+ (without SH0ES) and the Pantheon+\&SH0ES (with SH0ES) data sets. Additionally, we incorporated data from BAO along with $H_0$ priors. We observed that integrating SH0ES data points leads to a higher...
Considering our 4G model of final unification, we have noticed a simple relation for Planck length in terms of nuclear physical constants. It’s published version can be expressed as, $\sqrt{\frac{G_N \hbar}{c^3}}\cong \left ( \frac{m_p^2}{\left ( m_n-m_p \right )m_e} \right )\left ( \frac{2 \pi R_0^2}{3ct_n} \right )\cong \left ( \frac{m_p^2}{\left ( m_n-m_p \right )m_e} \right ) \left (...
Black holes are among the most extraordinary and intriguing objects in the Universe. Within the framework of General Relativity, one of the most well-established modern physical theories, the study of these objects can be carried out using the simplest solution, known as the Schwarzschild metric. This solution describes a static and spherically symmetric black hole, enabling the analysis of...
With our corrected cosmic red shift formula and Hubble-Hawking model of cosmology [1], we have developed a direct relation for fitting the accelerating model of luminosity distances (LD) [2-6] having $H_0\cong 2.92\times 10^{-19}\left(2.725\right)^2\cong 66.9 \textrm{ km/sec/Mpc}$. If $z_{new}\cong \frac{E_{emitted}-E_{Observed}}{E_{emitted}}\cong \frac{\lambda_{Observed}-\lambda_{emitted}}...
With our corrected cosmic red shift formula and Hubble-Hawking model of cosmology, we have developed direct relations for fitting the adot and Hubble parameter. Hubble-Hawking model of current Hubble parameter can be expressed as, $\left ( H_{0} \right )_{HH} \cong 2.92 \times 10^{-19} \left ( 2.725 \right )^2\cong 66.9 \textrm{ km/sec/Mpc}$. If $z_{new}\cong...
The intrinsic spin of fermions can generate torsion in spacetime. This gives rise to an effective four-fermion interaction that fermions experience within a fermionic distribution. This interaction is expected to become significant when densities become large, such as in early-universe cosmology or in compact astrophysical objects like neutron stars. In this contribution, I will discuss the...
