Weak-field limit of Kaluza–Klein models with spherically symmetric static scalar field: observational constraints
Abstract In a multidimensional Kaluza–Klein model with Ricci-flat internal space, we study the gravitational field in the weak-field limit. This field is created by two coupled sources. First, this is a point-like massive body which has a dust-like equation of state in the external space and an arbi...
| Main Authors: | , , , , |
|---|---|
| Format: | Article |
| Language: | English |
| Published: |
SpringerOpen
2017-10-01
|
| Series: | European Physical Journal C: Particles and Fields |
| Online Access: | http://link.springer.com/article/10.1140/epjc/s10052-017-5311-x |
| _version_ | 1818056637922934784 |
|---|---|
| author | Alexander Zhuk Alexey Chopovsky Seyed Hossein Fakhr Valerii Shulga Han Wei |
| author_facet | Alexander Zhuk Alexey Chopovsky Seyed Hossein Fakhr Valerii Shulga Han Wei |
| author_sort | Alexander Zhuk |
| collection | DOAJ |
| description | Abstract In a multidimensional Kaluza–Klein model with Ricci-flat internal space, we study the gravitational field in the weak-field limit. This field is created by two coupled sources. First, this is a point-like massive body which has a dust-like equation of state in the external space and an arbitrary parameter $$\varOmega $$ Ω of equation of state in the internal space. The second source is a static spherically symmetric massive scalar field centered at the origin where the point-like massive body is. The found perturbed metric coefficients are used to calculate the parameterized post-Newtonian (PPN) parameter $$\gamma $$ γ . We define under which conditions $$\gamma $$ γ can be very close to unity in accordance with the relativistic gravitational tests in the solar system. This can take place for both massive or massless scalar fields. For example, to have $$\gamma \approx 1$$ γ ≈ 1 in the solar system, the mass of scalar field should be $$\mu \gtrsim 5.05\times 10^{-49}$$ μ ≳ 5.05 × 10 - 49 g $$\sim 2.83\times 10^{-16}$$ ∼ 2.83 × 10 - 16 eV. In all cases, we arrive at the same conclusion that to be in agreement with the relativistic gravitational tests, the gravitating mass should have tension: $$\varOmega = -\,1/2$$ Ω = - 1 / 2 . |
| first_indexed | 2024-12-10T12:32:01Z |
| format | Article |
| id | doaj.art-48386d75328440de910590a9f22f5177 |
| institution | Directory Open Access Journal |
| issn | 1434-6044 1434-6052 |
| language | English |
| last_indexed | 2024-12-10T12:32:01Z |
| publishDate | 2017-10-01 |
| publisher | SpringerOpen |
| record_format | Article |
| series | European Physical Journal C: Particles and Fields |
| spelling | doaj.art-48386d75328440de910590a9f22f51772022-12-22T01:48:46ZengSpringerOpenEuropean Physical Journal C: Particles and Fields1434-60441434-60522017-10-0177111710.1140/epjc/s10052-017-5311-xWeak-field limit of Kaluza–Klein models with spherically symmetric static scalar field: observational constraintsAlexander Zhuk0Alexey Chopovsky1Seyed Hossein Fakhr2Valerii Shulga3Han Wei4The International Center of Future Science of the Jilin UniversityAstronomical Observatory, Odessa National UniversityAstronomical Observatory, Odessa National UniversityThe International Center of Future Science of the Jilin UniversityThe International Center of Future Science of the Jilin UniversityAbstract In a multidimensional Kaluza–Klein model with Ricci-flat internal space, we study the gravitational field in the weak-field limit. This field is created by two coupled sources. First, this is a point-like massive body which has a dust-like equation of state in the external space and an arbitrary parameter $$\varOmega $$ Ω of equation of state in the internal space. The second source is a static spherically symmetric massive scalar field centered at the origin where the point-like massive body is. The found perturbed metric coefficients are used to calculate the parameterized post-Newtonian (PPN) parameter $$\gamma $$ γ . We define under which conditions $$\gamma $$ γ can be very close to unity in accordance with the relativistic gravitational tests in the solar system. This can take place for both massive or massless scalar fields. For example, to have $$\gamma \approx 1$$ γ ≈ 1 in the solar system, the mass of scalar field should be $$\mu \gtrsim 5.05\times 10^{-49}$$ μ ≳ 5.05 × 10 - 49 g $$\sim 2.83\times 10^{-16}$$ ∼ 2.83 × 10 - 16 eV. In all cases, we arrive at the same conclusion that to be in agreement with the relativistic gravitational tests, the gravitating mass should have tension: $$\varOmega = -\,1/2$$ Ω = - 1 / 2 .http://link.springer.com/article/10.1140/epjc/s10052-017-5311-x |
| spellingShingle | Alexander Zhuk Alexey Chopovsky Seyed Hossein Fakhr Valerii Shulga Han Wei Weak-field limit of Kaluza–Klein models with spherically symmetric static scalar field: observational constraints European Physical Journal C: Particles and Fields |
| title | Weak-field limit of Kaluza–Klein models with spherically symmetric static scalar field: observational constraints |
| title_full | Weak-field limit of Kaluza–Klein models with spherically symmetric static scalar field: observational constraints |
| title_fullStr | Weak-field limit of Kaluza–Klein models with spherically symmetric static scalar field: observational constraints |
| title_full_unstemmed | Weak-field limit of Kaluza–Klein models with spherically symmetric static scalar field: observational constraints |
| title_short | Weak-field limit of Kaluza–Klein models with spherically symmetric static scalar field: observational constraints |
| title_sort | weak field limit of kaluza klein models with spherically symmetric static scalar field observational constraints |
| url | http://link.springer.com/article/10.1140/epjc/s10052-017-5311-x |
| work_keys_str_mv | AT alexanderzhuk weakfieldlimitofkaluzakleinmodelswithsphericallysymmetricstaticscalarfieldobservationalconstraints AT alexeychopovsky weakfieldlimitofkaluzakleinmodelswithsphericallysymmetricstaticscalarfieldobservationalconstraints AT seyedhosseinfakhr weakfieldlimitofkaluzakleinmodelswithsphericallysymmetricstaticscalarfieldobservationalconstraints AT valeriishulga weakfieldlimitofkaluzakleinmodelswithsphericallysymmetricstaticscalarfieldobservationalconstraints AT hanwei weakfieldlimitofkaluzakleinmodelswithsphericallysymmetricstaticscalarfieldobservationalconstraints |