This paper proposes a mechanism to stabilize the size of the extra dimension in the Randall-Sundrum scenario. The potential for the modulus field that determines the size of the fifth dimension is generated by a bulk scalar field with quartic interactions localized on the two 3-branes. This potential allows the compactification scale to solve the hierarchy problem without fine-tuning parameters. The Standard Model has been successful in explaining experimental observations but has several issues, including the gauge hierarchy problem, which is the large disparity between the weak scale and the Planck scale. The Randall-Sundrum model proposes a higher-dimensional scenario without requiring large extra dimensions. It involves a single $ S^1/Z_2 $ orbifold extra dimension with 3-branes at the fixed points and a finely tuned cosmological constant. The resulting spacetime metric has a redshift factor that depends exponentially on the radius of the compactified dimension. The non-factorizable geometry of this model leads to a four-dimensional Planck mass that is of order the fundamental scale M. A field confined to the 3-brane at $ \phi = \pi $ has a physical mass that is exponentially smaller than its mass parameter. Kaluza-Klein gravitational modes have TeV-scale mass splittings and couplings. A bulk field with mass on the order of M has low-lying Kaluza-Klein excitations that reside near $ \phi = \pi $, giving them masses on the order of the weak scale. In the Randall-Sundrum scenario, $ r_c $ is associated with the vacuum expectation value of a massless scalar field. This modulus field has zero potential, so $ r_c $ is not determined by the model's dynamics. To stabilize $ r_c $, a potential is generated by a bulk scalar field with interaction terms localized on the two 3-branes. The minimum of this potential can be arranged to yield $ kr_c \sim 10 $ without fine-tuning. A scalar field $ \Phi $ with a bulk action and interaction terms on the branes leads to a $ \phi $-dependent vacuum expectation value. Solving the differential equation for $ \Phi $ yields an effective four-dimensional potential for $ r_c $. The potential has a minimum at $ kr_c \sim 10 $, which is achieved without extreme fine-tuning. The stress tensor for the scalar field is negligible compared to the stress tensor induced by the bulk cosmological constant. The potential for $ r_c $ is valid for large $ kr_c $, but for small $ kr_c $, the potential becomes singular. However, finite $ \lambda $ corrections remove the singularity. The scenario allows for a standard cosmology at temperatures below the weak scale, but differs from Friedmann cosmology at higher temperatures. The Randall-Sundrum model is an attractive solution to the hierarchy problem but has features less appealing than the Standard Model, such as no explanation for the smallness ofThis paper proposes a mechanism to stabilize the size of the extra dimension in the Randall-Sundrum scenario. The potential for the modulus field that determines the size of the fifth dimension is generated by a bulk scalar field with quartic interactions localized on the two 3-branes. This potential allows the compactification scale to solve the hierarchy problem without fine-tuning parameters. The Standard Model has been successful in explaining experimental observations but has several issues, including the gauge hierarchy problem, which is the large disparity between the weak scale and the Planck scale. The Randall-Sundrum model proposes a higher-dimensional scenario without requiring large extra dimensions. It involves a single $ S^1/Z_2 $ orbifold extra dimension with 3-branes at the fixed points and a finely tuned cosmological constant. The resulting spacetime metric has a redshift factor that depends exponentially on the radius of the compactified dimension. The non-factorizable geometry of this model leads to a four-dimensional Planck mass that is of order the fundamental scale M. A field confined to the 3-brane at $ \phi = \pi $ has a physical mass that is exponentially smaller than its mass parameter. Kaluza-Klein gravitational modes have TeV-scale mass splittings and couplings. A bulk field with mass on the order of M has low-lying Kaluza-Klein excitations that reside near $ \phi = \pi $, giving them masses on the order of the weak scale. In the Randall-Sundrum scenario, $ r_c $ is associated with the vacuum expectation value of a massless scalar field. This modulus field has zero potential, so $ r_c $ is not determined by the model's dynamics. To stabilize $ r_c $, a potential is generated by a bulk scalar field with interaction terms localized on the two 3-branes. The minimum of this potential can be arranged to yield $ kr_c \sim 10 $ without fine-tuning. A scalar field $ \Phi $ with a bulk action and interaction terms on the branes leads to a $ \phi $-dependent vacuum expectation value. Solving the differential equation for $ \Phi $ yields an effective four-dimensional potential for $ r_c $. The potential has a minimum at $ kr_c \sim 10 $, which is achieved without extreme fine-tuning. The stress tensor for the scalar field is negligible compared to the stress tensor induced by the bulk cosmological constant. The potential for $ r_c $ is valid for large $ kr_c $, but for small $ kr_c $, the potential becomes singular. However, finite $ \lambda $ corrections remove the singularity. The scenario allows for a standard cosmology at temperatures below the weak scale, but differs from Friedmann cosmology at higher temperatures. The Randall-Sundrum model is an attractive solution to the hierarchy problem but has features less appealing than the Standard Model, such as no explanation for the smallness of