content_image/351072.jpg content_image/351073.jpg content_image/351074.jpg content_image/351075.jpg content_image/351076.jpg
Here M now refers to the mass of wormhole. Using (6) and (12) in (3), we get 

Putting (19) in (7), we obtain 

<img src='content_image/351072.jpg'>

<img src='content_image/351073.jpg'>

Alternatively, Eq. (20) can be obtained by inserting (6) and (12) in (4). In Fig. 1 and 2, we have plotted the magnitudes of the radial and the transverse pressures against the radial coordinate. These show that both the pressures have arbitrary large values near the throat while these vanish in the asymptotic limit of r . This shows that the matter distribution also satisfies the condition of asymptotic flatness, consistently with the wormhole geometry. The difference of radial and transverse pressures represents surface tension which plays very crucial role in compact stars [20]. Fig. 3 shows that the behavior of surface tension is analogous to the two pressures. 

Comparison of Eqs. (8) and (19) yields a relationship between pressure and energy density, given by 

On comparing Eq. (21) with p = ωρ , we get 

<img src='content_image/351074.jpg'>

<img src='content_image/351075.jpg'>

It shows that the wormhole under consideration satisfies a variable equation of state. The variable EoS arises naturally while solving the field equations for the wormhole. Interestingly a variable EoS unifies various forms of dark energy including phantom energy and Chaplygin gas, both of which support the wormhole spacetime [21]. The behavior of ω ( r ) is given in Fig. 4 and it shows that the EoS parameter ω has to be negative to model a wormhole. It naturally yields negative radial pressure and positive energy density. 

The case of isotropic pressure p = p$_{t}$ is obtained by fixing α = 1. We have 

<img src='content_image/351076.jpg'>

