Parametrization of Deceleration Parameter in <b><i>f</i></b>(<b><i>Q</i></b>) Gravity
In this paper, we investigate the modified symmetric teleparallel gravity or <inline-formula><math xmlns="http://www.w3.org/1998/Math/MathML" display="inline"><semantics><mrow><mi>f</mi><mo>(</mo><mi>Q</mi><mo>)<...
| Main Authors: | , , |
|---|---|
| Format: | Article |
| Language: | English |
| Published: |
MDPI AG
2022-12-01
|
| Series: | Physics |
| Subjects: | |
| Online Access: | https://www.mdpi.com/2624-8174/4/4/90 |
| _version_ | 1827637149064757248 |
|---|---|
| author | Gaurav N. Gadbail Sanjay Mandal Pradyumn Kumar Sahoo |
| author_facet | Gaurav N. Gadbail Sanjay Mandal Pradyumn Kumar Sahoo |
| author_sort | Gaurav N. Gadbail |
| collection | DOAJ |
| description | In this paper, we investigate the modified symmetric teleparallel gravity or <inline-formula><math xmlns="http://www.w3.org/1998/Math/MathML" display="inline"><semantics><mrow><mi>f</mi><mo>(</mo><mi>Q</mi><mo>)</mo></mrow></semantics></math></inline-formula> gravity, where <i>Q</i> is the nonmetricity, to study the evolutionary history of the universe by considering the functional form of <inline-formula><math xmlns="http://www.w3.org/1998/Math/MathML" display="inline"><semantics><mrow><mi>f</mi><mrow><mo>(</mo><mi>Q</mi><mo>)</mo></mrow><mo>=</mo><mi>α</mi><msup><mi>Q</mi><mi>n</mi></msup></mrow></semantics></math></inline-formula>, where <inline-formula><math xmlns="http://www.w3.org/1998/Math/MathML" display="inline"><semantics><mi>α</mi></semantics></math></inline-formula> and <i>n</i> are constants. Here, we consider the parametrization form of the deceleration parameter as <inline-formula><math xmlns="http://www.w3.org/1998/Math/MathML" display="inline"><semantics><mrow><mi>q</mi><mo>=</mo><msub><mi>q</mi><mn>0</mn></msub><mo>+</mo><mrow><msub><mi>q</mi><mn>1</mn></msub><mspace width="0.166667em"></mspace><mi>z</mi></mrow><mo>/</mo><msup><mrow><mo>(</mo><mn>1</mn><mo>+</mo><mi>z</mi><mo>)</mo></mrow><mn>2</mn></msup></mrow></semantics></math></inline-formula> (with the parameters <inline-formula><math xmlns="http://www.w3.org/1998/Math/MathML" display="inline"><semantics><msub><mi>q</mi><mn>0</mn></msub></semantics></math></inline-formula><inline-formula><math xmlns="http://www.w3.org/1998/Math/MathML" display="inline"><semantics><mrow><mo>(</mo><mi>q</mi></mrow></semantics></math></inline-formula> at <inline-formula><math xmlns="http://www.w3.org/1998/Math/MathML" display="inline"><semantics><mrow><mi>z</mi><mo>=</mo><mn>0</mn><mo>)</mo></mrow></semantics></math></inline-formula>, <inline-formula><math xmlns="http://www.w3.org/1998/Math/MathML" display="inline"><semantics><msub><mi>q</mi><mn>1</mn></msub></semantics></math></inline-formula>, and the redshift, <i>z</i>), which provides the desired property for a sign flip from a decelerating to an accelerating phase. We obtain the solution of the Hubble parameter by examining the mentioned parametric form of <i>q</i>, and then we impose the solution in Friedmann equations. Employing the Bayesian analysis for the Observational Hubble data (OHD), we estimated the constraints on the associated free parameters <inline-formula><math xmlns="http://www.w3.org/1998/Math/MathML" display="inline"><semantics><mrow><mo>(</mo><msub><mi>H</mi><mn>0</mn></msub><mo>,</mo><msub><mi>q</mi><mn>0</mn></msub><mo>,</mo><msub><mi>q</mi><mn>1</mn></msub><mo>)</mo></mrow></semantics></math></inline-formula> with <inline-formula><math xmlns="http://www.w3.org/1998/Math/MathML" display="inline"><semantics><msub><mi>H</mi><mn>0</mn></msub></semantics></math></inline-formula> the current Hubble parameter to determine if this model may challenge the <inline-formula><math xmlns="http://www.w3.org/1998/Math/MathML" display="inline"><semantics><mi mathvariant="normal">Λ</mi></semantics></math></inline-formula>CDM (<inline-formula><math xmlns="http://www.w3.org/1998/Math/MathML" display="inline"><semantics><mi mathvariant="normal">Λ</mi></semantics></math></inline-formula> cold dark matter with the cosmological constant, <inline-formula><math xmlns="http://www.w3.org/1998/Math/MathML" display="inline"><semantics><mi mathvariant="normal">Λ</mi></semantics></math></inline-formula>) limitations. Furthermore, the constrained current value of the deceleration parameter <inline-formula><math xmlns="http://www.w3.org/1998/Math/MathML" display="inline"><semantics><mrow><msub><mi>q</mi><mn>0</mn></msub><mo>=</mo><mo>−</mo><mn>0</mn><mo>.</mo><msubsup><mn>832</mn><mrow><mo>−</mo><mn>0.091</mn></mrow><mrow><mo>+</mo><mn>0.091</mn></mrow></msubsup></mrow></semantics></math></inline-formula> shows that the present universe is accelerating. We also investigate the evolutionary trajectory of the energy density, pressure, and EoS (equation-of-state) parameters to conclude the accelerating behavior of the universe. Finally, we try to demonstrate that the considered parametric form of the deceleration parameter is compatible with <inline-formula><math xmlns="http://www.w3.org/1998/Math/MathML" display="inline"><semantics><mrow><mi>f</mi><mo>(</mo><mi>Q</mi><mo>)</mo></mrow></semantics></math></inline-formula> gravity. |
| first_indexed | 2024-03-09T15:57:11Z |
| format | Article |
| id | doaj.art-2ed270c13f86414193a7ac4989df8c05 |
| institution | Directory Open Access Journal |
| issn | 2624-8174 |
| language | English |
| last_indexed | 2024-03-09T15:57:11Z |
| publishDate | 2022-12-01 |
| publisher | MDPI AG |
| record_format | Article |
| series | Physics |
| spelling | doaj.art-2ed270c13f86414193a7ac4989df8c052023-11-24T17:26:41ZengMDPI AGPhysics2624-81742022-12-01441403141210.3390/physics4040090Parametrization of Deceleration Parameter in <b><i>f</i></b>(<b><i>Q</i></b>) GravityGaurav N. Gadbail0Sanjay Mandal1Pradyumn Kumar Sahoo2Department of Mathematics, Birla Institute of Technology and Science-Pilani, Hyderabad Campus, Hyderabad 500078, IndiaDepartment of Mathematics, Birla Institute of Technology and Science-Pilani, Hyderabad Campus, Hyderabad 500078, IndiaDepartment of Mathematics, Birla Institute of Technology and Science-Pilani, Hyderabad Campus, Hyderabad 500078, IndiaIn this paper, we investigate the modified symmetric teleparallel gravity or <inline-formula><math xmlns="http://www.w3.org/1998/Math/MathML" display="inline"><semantics><mrow><mi>f</mi><mo>(</mo><mi>Q</mi><mo>)</mo></mrow></semantics></math></inline-formula> gravity, where <i>Q</i> is the nonmetricity, to study the evolutionary history of the universe by considering the functional form of <inline-formula><math xmlns="http://www.w3.org/1998/Math/MathML" display="inline"><semantics><mrow><mi>f</mi><mrow><mo>(</mo><mi>Q</mi><mo>)</mo></mrow><mo>=</mo><mi>α</mi><msup><mi>Q</mi><mi>n</mi></msup></mrow></semantics></math></inline-formula>, where <inline-formula><math xmlns="http://www.w3.org/1998/Math/MathML" display="inline"><semantics><mi>α</mi></semantics></math></inline-formula> and <i>n</i> are constants. Here, we consider the parametrization form of the deceleration parameter as <inline-formula><math xmlns="http://www.w3.org/1998/Math/MathML" display="inline"><semantics><mrow><mi>q</mi><mo>=</mo><msub><mi>q</mi><mn>0</mn></msub><mo>+</mo><mrow><msub><mi>q</mi><mn>1</mn></msub><mspace width="0.166667em"></mspace><mi>z</mi></mrow><mo>/</mo><msup><mrow><mo>(</mo><mn>1</mn><mo>+</mo><mi>z</mi><mo>)</mo></mrow><mn>2</mn></msup></mrow></semantics></math></inline-formula> (with the parameters <inline-formula><math xmlns="http://www.w3.org/1998/Math/MathML" display="inline"><semantics><msub><mi>q</mi><mn>0</mn></msub></semantics></math></inline-formula><inline-formula><math xmlns="http://www.w3.org/1998/Math/MathML" display="inline"><semantics><mrow><mo>(</mo><mi>q</mi></mrow></semantics></math></inline-formula> at <inline-formula><math xmlns="http://www.w3.org/1998/Math/MathML" display="inline"><semantics><mrow><mi>z</mi><mo>=</mo><mn>0</mn><mo>)</mo></mrow></semantics></math></inline-formula>, <inline-formula><math xmlns="http://www.w3.org/1998/Math/MathML" display="inline"><semantics><msub><mi>q</mi><mn>1</mn></msub></semantics></math></inline-formula>, and the redshift, <i>z</i>), which provides the desired property for a sign flip from a decelerating to an accelerating phase. We obtain the solution of the Hubble parameter by examining the mentioned parametric form of <i>q</i>, and then we impose the solution in Friedmann equations. Employing the Bayesian analysis for the Observational Hubble data (OHD), we estimated the constraints on the associated free parameters <inline-formula><math xmlns="http://www.w3.org/1998/Math/MathML" display="inline"><semantics><mrow><mo>(</mo><msub><mi>H</mi><mn>0</mn></msub><mo>,</mo><msub><mi>q</mi><mn>0</mn></msub><mo>,</mo><msub><mi>q</mi><mn>1</mn></msub><mo>)</mo></mrow></semantics></math></inline-formula> with <inline-formula><math xmlns="http://www.w3.org/1998/Math/MathML" display="inline"><semantics><msub><mi>H</mi><mn>0</mn></msub></semantics></math></inline-formula> the current Hubble parameter to determine if this model may challenge the <inline-formula><math xmlns="http://www.w3.org/1998/Math/MathML" display="inline"><semantics><mi mathvariant="normal">Λ</mi></semantics></math></inline-formula>CDM (<inline-formula><math xmlns="http://www.w3.org/1998/Math/MathML" display="inline"><semantics><mi mathvariant="normal">Λ</mi></semantics></math></inline-formula> cold dark matter with the cosmological constant, <inline-formula><math xmlns="http://www.w3.org/1998/Math/MathML" display="inline"><semantics><mi mathvariant="normal">Λ</mi></semantics></math></inline-formula>) limitations. Furthermore, the constrained current value of the deceleration parameter <inline-formula><math xmlns="http://www.w3.org/1998/Math/MathML" display="inline"><semantics><mrow><msub><mi>q</mi><mn>0</mn></msub><mo>=</mo><mo>−</mo><mn>0</mn><mo>.</mo><msubsup><mn>832</mn><mrow><mo>−</mo><mn>0.091</mn></mrow><mrow><mo>+</mo><mn>0.091</mn></mrow></msubsup></mrow></semantics></math></inline-formula> shows that the present universe is accelerating. We also investigate the evolutionary trajectory of the energy density, pressure, and EoS (equation-of-state) parameters to conclude the accelerating behavior of the universe. Finally, we try to demonstrate that the considered parametric form of the deceleration parameter is compatible with <inline-formula><math xmlns="http://www.w3.org/1998/Math/MathML" display="inline"><semantics><mrow><mi>f</mi><mo>(</mo><mi>Q</mi><mo>)</mo></mrow></semantics></math></inline-formula> gravity.https://www.mdpi.com/2624-8174/4/4/90<i>f</i>(<i>Q</i>) gravityaccelerated expansiondeceleration parameterEoS (equation-of-state) parametercosmic chronometer datasetobservational constraint |
| spellingShingle | Gaurav N. Gadbail Sanjay Mandal Pradyumn Kumar Sahoo Parametrization of Deceleration Parameter in <b><i>f</i></b>(<b><i>Q</i></b>) Gravity Physics <i>f</i>(<i>Q</i>) gravity accelerated expansion deceleration parameter EoS (equation-of-state) parameter cosmic chronometer dataset observational constraint |
| title | Parametrization of Deceleration Parameter in <b><i>f</i></b>(<b><i>Q</i></b>) Gravity |
| title_full | Parametrization of Deceleration Parameter in <b><i>f</i></b>(<b><i>Q</i></b>) Gravity |
| title_fullStr | Parametrization of Deceleration Parameter in <b><i>f</i></b>(<b><i>Q</i></b>) Gravity |
| title_full_unstemmed | Parametrization of Deceleration Parameter in <b><i>f</i></b>(<b><i>Q</i></b>) Gravity |
| title_short | Parametrization of Deceleration Parameter in <b><i>f</i></b>(<b><i>Q</i></b>) Gravity |
| title_sort | parametrization of deceleration parameter in b i f i b b i q i b gravity |
| topic | <i>f</i>(<i>Q</i>) gravity accelerated expansion deceleration parameter EoS (equation-of-state) parameter cosmic chronometer dataset observational constraint |
| url | https://www.mdpi.com/2624-8174/4/4/90 |
| work_keys_str_mv | AT gauravngadbail parametrizationofdecelerationparameterinbifibbiqibgravity AT sanjaymandal parametrizationofdecelerationparameterinbifibbiqibgravity AT pradyumnkumarsahoo parametrizationofdecelerationparameterinbifibbiqibgravity |