Galactic kinematics with modified Newtonian dynamics

O. Bienaymé*, B. Famaey, X. Wu, H. S. Zhao, D. Aubert

*Corresponding author for this work

Research output: Contribution to journalArticlepeer-review

31 Citations (Scopus)

Abstract

We look for observational signatures that could discriminate between Newtonian and modified Newtonian (MOND) dynamics in the Milky Way, in view of the advent of large astrometrie and spectroscopic surveys. Indeed, a typical signature of MOND is an apparent disk, of "phantom" dark matter, which is uniquely correlated with the visible disk-density distribution. Due to this phantom dark disk, Newtonian models with a spherical halo have different signatures from. MOND models close to the Galactic plane. The models can thus be differentiated by measuring dynamically (within Newtonian dynamics) the disk surface density at the solar radius, the radial mass gradient within the disk, or the velocity ellipsoid tilt angle above the Galactic plane. Using the most realistic possible baryonic mass model for the Milky Way, we predict that, if MOND applies, the local surface density measured by a Newtonist will be approximately 78 M⊙/pc2 within 1.1 kpc of the Galactic plane, the dynamically measured disk scale-length will be enhanced by a factor of 1.25 with respect to the visible disk scale-length, and the local vertical tilt of the velocity ellipsoid at 1 kpc above the plane will be approximately 6 degrees. None of these tests can be conclusive for the present-day accuracy of Milky Way data, but they will be of prime interest with, the advent of large surveys such as GAIA.

Original languageEnglish
Pages (from-to)801-805
Number of pages5
JournalAstronomy and Astrophysics
Volume500
Issue number2
DOIs
Publication statusPublished - 1 Jun 2009

Keywords

  • Galaxy: fundamental parameters
  • Galaxy: kinematics and dynamics
  • Galaxy: structure
  • Gravitation
  • Stars: kinematics

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