The Magellanic Stream in Modified Newtonian Dynamics

Abstract

The dynamics of the Magellanic Stream (MS) as a series of clouds extending from the Magellanic Clouds (MCs) to the south Galactic pole is affected by the distribution and the amount of matter in the Milky Way. We calculate the gravitational effect of the Galactic disk on the MS in the framework of modified Newtonian dynamics(MOND) and compare with observations of the Stream's radial velocity. We consider the tidal force of the Galaxy, which strips material from the MCs to form the MS, and, using a no-halo model of the Galaxy, we ignore the effect of the drag of the Galactic halo on the MS. We also compare the MONDian dynamics with that in logarithmic and power-law dark halo models and show that the MOND theory seems plausible for describing the dynamics of satellite galaxies such as the MCs. Finally, we perform a maximum likelihood analysis to obtain the best MOND parameters for the Galactic disk.

11 pages, 6 figures

References in corpus (2)

• Refining MOND interpolating function and TeVeS Lagrangian
• Axisymmetric and triaxial MOND density-potential pairs

Cited by in corpus (8)

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• Vertical dynamics of disk galaxies in MOND
• Galactic kinematics with modified Newtonian dynamics
• Distant star clusters of the Milky Way in MOND
• Spherical Collapse in Modified Newtonian Dynamics (MOND)
• Galactic orbital motions in the Dark Matter, MOdified Newtonian Dynamics and MOdified Gravity scenarios
• Galactic orbital motions of star clusters: static versus semicosmological time-dependent Galactic potentials
• Observational Constraints on the Modified Gravity Model (MOG) Proposed by Moffat: Using the Magellanic System