Fractional Stars

TL;DR

This paper explores star formation from fractional molecular clouds using fractional gravity, deriving key parameters like Jeans mass and star burning temperature, and discusses stability conditions through hydrostatic equilibrium analysis.

Contribution

It introduces a fractional gravity framework for star formation, deriving new expressions for Jeans mass and star temperature, expanding understanding of fractional celestial systems.

Findings

Jeans mass in fractional gravity is significantly smaller than traditional models.

Derived star burning temperature using Gamow theory.

Analyzed hydrostatic equilibrium and Lane-Emden equation for fractional stars.

Abstract

This study examines the possibility of starting the process of collapsing and forming stars from a fractional molecular cloud. Although the Verlinde's approach is employed to derive the corresponding gravitational potential, the results are easily generalizable to other gravitational potential proposals for fractional systems. It is due to the fact that the different methods, despite the difference in the details of results, all obtain power forms for the potential in terms of radius. An essential result of this analysis is the derivation of the corresponding Jeans mass limit, which is a crucial parameter in understanding the formation of stars. The study shows that the Jeans mass of a cloud in fractional gravity is much smaller than the traditional value. In addition, the study also determines the burning temperature of the resulting star using the Gamow theory. This calculation provides insight into the complex processes that govern the evolution of these celestial bodies. Finally, the study briefly discusses the investigation of hydrostatic equilibrium, a crucial condition that ensures the stability of these fractional stars. It also addresses the corresponding Lane--Emden equation, which is pivotal in understanding this equilibrium.