Finding the Missing Link between Two Extrema of Wind Speed Patterns:Use of Quintessence Contaminated Pseudo Newtonian Potential

Abstract

In the literature, two distinct patterns of wind are followed. For adiabatic accretion onto Kerr metric, the wind curve turns almost constant valued, i.e., parallel to the radial distance axis as we go far from the central gravitating object. On the other hand, the accretion model of dark energy candidate shows a wind curve which is parallel to the velocity axis, i.e., the wind speed reaches the value of light’s speed at a finite radial distance. So far we fail to find any intermediate wind speed profile style. These works are done with a methodology where the highly nonlinearness grown due to general relativity is avoided by introducing a pseudo Newtonian potential which is a function of the radial distance from the black hole and the spin parameter of the black hole only. In this present work, we are motivated to find some system where the wind speed may stay in the intermediate region of the said extremities. A black hole sitting in a quintessence tub shows repulsive nature as an accretor. Viscosity, on the other hand, does act like a heating up/ frictional element which opposes a smooth inward flow. We check the joint effects on a quintessence black hole as well as viscosity on accretion disc. The variations of density profiles are studied along with the corresponding shear viscosity to entropy density ratio. Results are tallied with the conventional predictions about the values of such quantities.