Cosmological perturbation theory in f(Q,T) gravity
We developed the cosmological linear theory of perturbations for f(Q, T) gravity, which is an extension of symmetric teleparallel gravity, with Q the non-metricity and T the trace of the stress-energy tensor. By considering an ansatz of f(Q, T) = f1(Q)+f2(T), which has been broadly studied in the li...
| Autores principales: | , |
|---|---|
| Formato: | Artículo |
| Lenguaje: | inglés |
| Publicado: |
IOP Publishing
2022
|
| Acceso en línea: | http://eprints.uanl.mx/29982/7/29982.pdf |
| _version_ | 1836640497280483328 |
|---|---|
| author | Nájera, Antonio Fajardo, Amanda |
| author_facet | Nájera, Antonio Fajardo, Amanda |
| author_sort | Nájera, Antonio |
| collection | Repositorio Institucional |
| description | We developed the cosmological linear theory of perturbations for f(Q, T) gravity, which is an extension of symmetric teleparallel gravity, with Q the non-metricity and T the trace of the stress-energy tensor. By considering an ansatz of f(Q, T) = f1(Q)+f2(T), which has been broadly studied in the literature and the coincident gauge where the connection vanishes, we got equations consistent with f(Q) gravity when fT = 0. In the case of the tensor perturbations, the propagation of gravitational waves was found to be identical to f(Q), as expected. For scalar perturbations, outside the limit fT = 0, we got that the coupling between Q and T in the Lagrangian produces a coupling between the perturbation of the density and the pressure. This coupling is preserved when considering the weak coupling limit between Q and T. On the other hand, in the strong coupling limit with a generic function of the form f2(T) = αT + βT2, the perturbative equations are heavily driven by the f2(T) derivatives when β 6= 0. However, when β = 0, the perturbative equations are identical to the weak coupling limit even though this case is a non-minimally coupling one. The presence of T in the Lagrangian breaks the equation of the conservation of energy, which in turn breaks
the standard ρ 0 + 3H(ρ + p) = 0 relation. We also derived a coupled system of differential equations between δ, the density contrast and v in the H << k limit and with negligible time derivative of the scalar perturbation potentials, which will be useful in future studies to see whether this class of theories constitute a good alternative to dark matter. These results might also enable to test f(Q, T) gravity with CMB and standard siren data that will help to determine if these models can reduce the Hubble constant tension and if they can constitute an alternative to the ΛCDM model. |
| format | Article |
| id | eprints-29982 |
| institution | UANL |
| language | English |
| publishDate | 2022 |
| publisher | IOP Publishing |
| record_format | eprints |
| spelling | eprints-299822025-07-02T15:15:00Z http://eprints.uanl.mx/29982/ Cosmological perturbation theory in f(Q,T) gravity Nájera, Antonio Fajardo, Amanda We developed the cosmological linear theory of perturbations for f(Q, T) gravity, which is an extension of symmetric teleparallel gravity, with Q the non-metricity and T the trace of the stress-energy tensor. By considering an ansatz of f(Q, T) = f1(Q)+f2(T), which has been broadly studied in the literature and the coincident gauge where the connection vanishes, we got equations consistent with f(Q) gravity when fT = 0. In the case of the tensor perturbations, the propagation of gravitational waves was found to be identical to f(Q), as expected. For scalar perturbations, outside the limit fT = 0, we got that the coupling between Q and T in the Lagrangian produces a coupling between the perturbation of the density and the pressure. This coupling is preserved when considering the weak coupling limit between Q and T. On the other hand, in the strong coupling limit with a generic function of the form f2(T) = αT + βT2, the perturbative equations are heavily driven by the f2(T) derivatives when β 6= 0. However, when β = 0, the perturbative equations are identical to the weak coupling limit even though this case is a non-minimally coupling one. The presence of T in the Lagrangian breaks the equation of the conservation of energy, which in turn breaks the standard ρ 0 + 3H(ρ + p) = 0 relation. We also derived a coupled system of differential equations between δ, the density contrast and v in the H << k limit and with negligible time derivative of the scalar perturbation potentials, which will be useful in future studies to see whether this class of theories constitute a good alternative to dark matter. These results might also enable to test f(Q, T) gravity with CMB and standard siren data that will help to determine if these models can reduce the Hubble constant tension and if they can constitute an alternative to the ΛCDM model. IOP Publishing 2022 Article PeerReviewed text en cc_by_nc_nd http://eprints.uanl.mx/29982/7/29982.pdf http://eprints.uanl.mx/29982/7.haspreviewThumbnailVersion/29982.pdf Nájera, Antonio y Fajardo, Amanda (2022) Cosmological perturbation theory in f(Q,T) gravity. Journal of Cosmology and Astroparticle Physics, 2022 (03). 020. ISSN 1475-7516 doi:10.1088/1475-7516/2022/03/020 |
| spellingShingle | Nájera, Antonio Fajardo, Amanda Cosmological perturbation theory in f(Q,T) gravity |
| thumbnail | https://rediab.uanl.mx/themes/sandal5/images/online.png |
| title | Cosmological perturbation theory in f(Q,T) gravity |
| title_full | Cosmological perturbation theory in f(Q,T) gravity |
| title_fullStr | Cosmological perturbation theory in f(Q,T) gravity |
| title_full_unstemmed | Cosmological perturbation theory in f(Q,T) gravity |
| title_short | Cosmological perturbation theory in f(Q,T) gravity |
| title_sort | cosmological perturbation theory in f q t gravity |
| url | http://eprints.uanl.mx/29982/7/29982.pdf |
| work_keys_str_mv | AT najeraantonio cosmologicalperturbationtheoryinfqtgravity AT fajardoamanda cosmologicalperturbationtheoryinfqtgravity |