Get access

The Milky Way rotation curve in Horava–Lifshitz theory

Authors

  • V. F. Cardone,

    Corresponding author
    1. Dipartimento di Scienze e Tecnologie dell’ Ambiente e del Territorio, Università degli Studi del Molise, Contrada Fonte Lappone, 86090 - Pesche (IS), Italy
    2. Dipartimento di Scienze Fisiche, Università degli Studi di Napoli ‘Federico II’, Complesso Universitario di Monte Sant’ Angelo, Edificio N, via Cinthia, 80126 - Napoli, Italy
    Search for more papers by this author
  • N. Radicella,

    1. Dipartimento di Fisica, Politecnico di Torino, Corso Duca degli Abruzzi 24, 10129 - Torino, Italy
    2. I.N.F.N. - Sezione di Torino, via Pietro Giuria 1, 10125 - Torino, Italy
    Search for more papers by this author
  • M. L. Ruggiero,

    1. Dipartimento di Fisica, Politecnico di Torino, Corso Duca degli Abruzzi 24, 10129 - Torino, Italy
    2. I.N.F.N. - Sezione di Torino, via Pietro Giuria 1, 10125 - Torino, Italy
    Search for more papers by this author
  • M. Capone

    1. I.N.F.N. - Sezione di Torino, via Pietro Giuria 1, 10125 - Torino, Italy
    2. Dipartimento di Matematica, Università degli Studi di Torino, Via Carlo Alberto 10, 10125 - Torino, Italy
    Search for more papers by this author

E-mail: winnyenodrac@gmail.com

ABSTRACT

The Horava–Lifshitz (HL) theory has recently attracted a lot of interest as a viable solution to some quantum gravity related problems and the presence of an effective cosmological constant able to drive the cosmic speed up. We show here that, in the weak field limit, the HL proposal leads to a modification of the gravitational potential because of two additive terms (scaling, respectively, as r2 and r−4) to the Newtonian 1/r potential. We then derive a general expression to compute the rotation curve of an extended system under the assumption that the mass density only depends on the cylindrical coordinates (R, z) showing that the HL modification induces a dependence of the circular velocity on the mass function which is a new feature of the theory. As a first exploratory analysis, we then try fitting the Milky Way rotation curve using its visible components only in order to see whether the HL modified potential can be an alternative to the dark matter framework. This turns out not to be the case so that we argue that dark matter is still needed, but the amount of dark matter and the dark halo density profile have to be revised according to the new HL potential.

Ancillary