Isotropic compact stellar model in Rastall's gravitational theory
Is Rastall's theory of gravity equivalent to Einstein's general relativity theory? This question has sparked a significant debate, prompting researchers to delve into the topic. To investigate further, we apply Rastall's theory's field equation to a spacetime characterized by sph...
| Main Author: | |
|---|---|
| Format: | Article |
| Language: | English |
| Published: |
Elsevier
2023-09-01
|
| Series: | Nuclear Physics B |
| Online Access: | http://www.sciencedirect.com/science/article/pii/S0550321323002341 |
| _version_ | 1797736877862682624 |
|---|---|
| author | G.G.L. Nashed |
| author_facet | G.G.L. Nashed |
| author_sort | G.G.L. Nashed |
| collection | DOAJ |
| description | Is Rastall's theory of gravity equivalent to Einstein's general relativity theory? This question has sparked a significant debate, prompting researchers to delve into the topic. To investigate further, we apply Rastall's theory's field equation to a spacetime characterized by spherical symmetry. This leads us to encounter a system of non-linear differential equations that is overdetermined. To address this, we make assumptions about the specific form of the metric potential's temporal component, denoted as gtt. Additionally, we impose constraints to eliminate the anisotropic condition, resulting in a vanishing effect. These steps allow us to determine the form of grr and ultimately achieve an isotropic spacetime. Furthermore, our investigation focuses on the potential of obtaining a set of parameters that align with the observed behavior of pulsars. To achieve this, we employ junction conditions to match the interior spacetime with the exterior Schwarzschild configuration, thereby constraining the model's relevant constants. Subsequently, we employ the pulsar SAXJ1748.9−2021, characterized by a measured mass of M=1.81±0.31,M⊙ and a radius of R=11.7±1.7 km, to numerically explore the physical properties of the model. Stability is assessed using the Tolman-Oppenheimer-Volkoff equation and the adiabatic index. Our findings suggest that Rastall's parameter, a key distinction of Rastall's theory from Einstein's general relativity, can play a crucial role in forming a realistic, compact object consistent with observational data. Furthermore, we verify the model's validity by comparing it with various observed masses and radii of different pulsars, ensuring a satisfactory fit between the model proposed in this study and the observed data. |
| first_indexed | 2024-03-12T13:20:30Z |
| format | Article |
| id | doaj.art-80861ae53e6849cf9749c1f15206622c |
| institution | Directory Open Access Journal |
| issn | 0550-3213 |
| language | English |
| last_indexed | 2024-03-12T13:20:30Z |
| publishDate | 2023-09-01 |
| publisher | Elsevier |
| record_format | Article |
| series | Nuclear Physics B |
| spelling | doaj.art-80861ae53e6849cf9749c1f15206622c2023-08-26T04:42:42ZengElsevierNuclear Physics B0550-32132023-09-01994116305Isotropic compact stellar model in Rastall's gravitational theoryG.G.L. Nashed0Centre for Theoretical Physics, The British University in Egypt, P.O. Box 43, El Sherouk City, Cairo 11837, Egypt; Center for Space Research, North-West University, Potchefstroom 2520, South Africa; Correspondence to: Centre for Theoretical Physics, The British University in Egypt, P.O. Box 43, El Sherouk City, Cairo 11837, Egypt.Is Rastall's theory of gravity equivalent to Einstein's general relativity theory? This question has sparked a significant debate, prompting researchers to delve into the topic. To investigate further, we apply Rastall's theory's field equation to a spacetime characterized by spherical symmetry. This leads us to encounter a system of non-linear differential equations that is overdetermined. To address this, we make assumptions about the specific form of the metric potential's temporal component, denoted as gtt. Additionally, we impose constraints to eliminate the anisotropic condition, resulting in a vanishing effect. These steps allow us to determine the form of grr and ultimately achieve an isotropic spacetime. Furthermore, our investigation focuses on the potential of obtaining a set of parameters that align with the observed behavior of pulsars. To achieve this, we employ junction conditions to match the interior spacetime with the exterior Schwarzschild configuration, thereby constraining the model's relevant constants. Subsequently, we employ the pulsar SAXJ1748.9−2021, characterized by a measured mass of M=1.81±0.31,M⊙ and a radius of R=11.7±1.7 km, to numerically explore the physical properties of the model. Stability is assessed using the Tolman-Oppenheimer-Volkoff equation and the adiabatic index. Our findings suggest that Rastall's parameter, a key distinction of Rastall's theory from Einstein's general relativity, can play a crucial role in forming a realistic, compact object consistent with observational data. Furthermore, we verify the model's validity by comparing it with various observed masses and radii of different pulsars, ensuring a satisfactory fit between the model proposed in this study and the observed data.http://www.sciencedirect.com/science/article/pii/S0550321323002341 |
| spellingShingle | G.G.L. Nashed Isotropic compact stellar model in Rastall's gravitational theory Nuclear Physics B |
| title | Isotropic compact stellar model in Rastall's gravitational theory |
| title_full | Isotropic compact stellar model in Rastall's gravitational theory |
| title_fullStr | Isotropic compact stellar model in Rastall's gravitational theory |
| title_full_unstemmed | Isotropic compact stellar model in Rastall's gravitational theory |
| title_short | Isotropic compact stellar model in Rastall's gravitational theory |
| title_sort | isotropic compact stellar model in rastall s gravitational theory |
| url | http://www.sciencedirect.com/science/article/pii/S0550321323002341 |
| work_keys_str_mv | AT gglnashed isotropiccompactstellarmodelinrastallsgravitationaltheory |