Quintessence Star Solutions with Conformal Symmetry in a Durgapal Spacetime

TL;DR

This work develops a physically viable, anisotropic compact star model incorporating a quintessence dark-energy field with equation of state parameter $w_Q$ in $(-1,-\tfrac{1}{3})$, within a conformal Killing symmetry framework based on the Durgapal-Fuloria metric. The authors derive exact interior solutions by solving the Einstein equations with a combined matter–quintessence energy-momentum tensor, closing the system with $p_r=\varpi\rho$ and enforcing CKV relations. They demonstrate smooth matching to a Schwarzschild exterior, verify stability via a generalized TOV equation and sound-speed criteria, and show that NEC/WEC/SEC are satisfied while DEC is violated, consistent with a quintessence star. Key results include regular central density, monotonic density and pressure profiles, a mass-radius relation within Buchdahl limits, finite surface redshift, and stable configurations against cracking, highlighting the viability of conformal-symmetric quintessence stars in DP spacetimes for studying dark-energy compact objects.

Abstract

The accelerated expansion of the Universe can be suitably attributed to the existence of the dark energy (DE). On the backdrop of this concept, this paper introduces a novel, anisotropic compact star model whose stability and structure are governed by the presence of quintessence field, defined by the parameter $ w_{Q} (-1<w_{Q}<-\frac{1}{3}) $ and which admits conformal symmetry. The construction of the model relied on the Durgapal-Fuloria (DP) metric formulation. The model successfully meets all the necessary physical constraints viz., TOV equation, energy conditions, compactness factor, surface redshift and casuality condition. The results are analyzed through analytical methods as well as through the graphical visualization for the various physical attributes.

Figures (20)

• Figure 1: Plot of $\rho^{eff}$ versus radial co-ordinate for $N = 0.00064309, N = 0.000662321, N= 0.00068761, N = 0.000708212$
• Figure 2: Plot of $p_{r}^{eff}$ versus radial co-ordinate for $N = 0.00064309, N = 0.000662321, N= 0.00068761, N = 0.000708212$
• Figure 3: Plot of $p_{t}^{eff}$ versus radial co-ordinate for $N = 0.00064309, N = 0.000662321, N= 0.00068761, N = 0.000708212$
• Figure 4: $\frac{d\rho^{eff}}{dr}$ against radial co-ordinate for different parameter values
• Figure 5: $\frac{d^{2}\rho^{eff}}{dr^{2}}$ against radial co-ordinate for different parameter values