Estimation of the Population of Stars in the Universe

Stars are light years away, and their brightness depends on multiple variables. Starting in the 20th century, artificial satellites were launched that added to the bright bodies of the observable sky. From 26.816 satellite observations and 9.037 stars visible to the naked eye, regression models were made between brightness and distances. The existence of a visual convergence plane that receives light photons arriving with a delay, c = 299.792.458 m·s^-1 was assumed. Under the principle of large-scale homogeneity and isotropy, the objective of the study was to develop models to estimate the population of stars in the universe. It is concluded that the correlation between the satellite brightness model and the surface light quantity model presented a high adjustment, so that the value of the a priori probability of emitting sources of photons (stars) per surface derives from the probability gradient theorem (TGP). The value 4.62E-9 starlight m^-2·s¹, is a universal constant obtained from the delay (speed) of light. The velocity of wave-bodies is associated with their probability of occurrence. The probability of physical phenomena is regulated by randomness which explains 50% and by causality which explains the remaining 50%. Light has a probability that arises from its speed, from that probability it is estimated that the population of stars in the universe is 4.5E24.