The Newtonian limit at intermediate energies
By Javier Román Cembranos. 2005
134 citations recorded by the source corpus.
We study the metric solutions for the gravitational equations in Modified Gravity Models (MGMs). In models with negative powers of the scalar curvature, we show that the Newtonian Limit (NL) is well defined as a limit at intermediate energies, in contrast with the usual low energy interpretation. Indeed, we show that the gravitational interaction is modified at low densities or low curvatures.
Subfields: Astronomy and Astrophysics, Nuclear and High Energy Physics
View Paper: https://www.semanticscholar.org/paper/16c318c2258fe1700c307a2b88aff008ee0f0032
How researchers see this paper
The researchers whose trusted networks rank it highest, strongest advocate first. Every researcher gets a different order.
In Astronomy and Astrophysics
- S. Tsujikawa
- Antonio de Felice
- Salvatore Capozziello
- Valerio Faraoni
- T. Sotiriou
- Francisco S. N. Lobo
- Tiberiu Harko
- Sergei D. Odintsov
In Nuclear and High Energy Physics
- S. Tsujikawa
- Antonio de Felice
- Salvatore Capozziello
- Valerio Faraoni
- T. Sotiriou
- Francisco S. N. Lobo
- Sergei D. Odintsov
- Tiberiu Harko
Citations in the corpus
- Low surface brightness galaxy rotation curves in the low energy limit of Rn gravity: no need for dark matter? (2006, result): “Unfortunately, here a strong debate is still open with different papers drawing contrasting results arguing in favour (Dick 2004; Sotiriou 2006; Cembranos 2006; Navarro & van Acoleyen 2005; Allemandi et al. 2005; Capozziello & Troisi 2005) or against (Dolgov 2003; Chiba 2003; Olmo 2005) such models.”
- Equivalence Principle Implications of Modified Gravity Models (2009, background): “Curvatureinvariant theories such as f(R) screen the scalar via the so-called chameleon mechanism, essentially by giving the scalar a mass that depends on the local density [18, 19, 20, 21, 22, 23, 24].”
- f(R) Theories Of Gravity (2008, background): “The chameleon effect can be applied to metric f(R) gravity (Cembranos, 2006; Faulkner et al., 2007; Navarro and Van Acoleyen, 2007; Starobinsky, 2007), with the result that theories of the kind (Amendola et al., 2007a,b,c; Carroll et al., 2004) f(R) = R − (1− n)µ2 ( R µ2 )n (134) are compatible…”
- f(R) Theories (2010, background): “tibility of f(R) models with local gravity constraints (see [469, 470, 245, 233, 154, 448, 251] for early works, and [31, 306, 134] for experimental constraints on viable f(R) dark energy models, and [101, 210, 330, 332, 471, 629, 149, 625, 329, 45, 511, 277, 534, 133, 445, 309, 89] for other relate”