Rotation Curves of Ursa Major Galaxies in the Context of Modified Newtonian Dynamics

1998 ◽  
Vol 503 (1) ◽  
pp. 97-108 ◽  
Author(s):  
R. H. Sanders ◽  
M. A. W. Verheijen
Keyword(s):  
Rotation Curves ◽  
Modified Newtonian Dynamics ◽  
Newtonian Dynamics

scholarly journals A method for discriminating between dark matter models and MOND modified inertia via galactic rotation curves

2020 ◽  
Vol 496 (2) ◽  
pp. 1077-1091
Author(s):  
Jonas Petersen ◽  
Mads T Frandsen
Keyword(s):  
Dark Matter ◽  
Galactic Centre ◽  
Galactic Rotation ◽  
Baryonic Matter ◽  
Rotation Curves ◽  
Density Profiles ◽  
Closed Curves ◽  
Modified Newtonian Dynamics ◽  
Newtonian Dynamics ◽  
Systematic Uncertainties

ABSTRACT Dark matter (DM) and modified Newtonian dynamics (MOND) models of rotationally supported galaxies lead to curves with different geometries in (gN, gtot)-space (g2-space). Here, gtot is the total acceleration and gN is the acceleration as obtained from the baryonic matter via Newtonian dynamics. In MOND modified inertia (MI) models, the curves in g2-space are closed with zero area and so curve segments at radii r ≥ rN (large radii) and r < rN (small radii) coincide, where rN is the radius where gN is greatest. In DM models with cored density profiles where gtot is also zero at the Galactic Centre, the curves are again closed, but the area of the closed curves are in general non-zero because the curve segments at radii r ≥ rN and r < rN do not coincide. Finally in DM models with cuspy density profiles such as the NFW profile where gtot is formally non-zero at the galactic origin the curves are open, and again the curve segments at radii r ≥ rN and r < rN do not coincide. We develop a test of whether data at small and large radii coincide and investigate rotation curves from the SPARC data base in order to discriminate between the above geometries. Due to loosely quantified systematic uncertainties, we do not underline the result of the test, but instead conclude that the test illustrates the relevance of this type of analysis and demonstrate the ability to discriminate between the considered DM and MI models in this way.

scholarly journals The prediction of rotation curves in gas-dominated dwarf galaxies with modified dynamics

2019 ◽  
Vol 485 (1) ◽  
pp. 513-521 ◽  
Author(s):  
R H Sanders
Keyword(s):  
Surface Density ◽  
Surface Brightness ◽  
Dark Halo ◽  
Baryonic Matter ◽  
Rotation Curves ◽  
Stellar Disc ◽  
Modified Newtonian Dynamics ◽  
Newtonian Dynamics ◽  
Low Surface Brightness ◽  
Low Surface Brightness Galaxies

ABSTRACT I consider the observed rotation curves of 12 gas-dominated low-surface-brightness galaxies – objects in which the mass of gas ranges between 2.2 and 27 times the mass of the stellar disc (mean = 9.4). This means that, in the usual decomposition of rotation curves into those resulting from various mass components, the mass-to-light ratio of the luminous stellar disc effectively vanishes as an additional adjustable parameter. It is seen that the observed rotation curves reflect the observed structure in gas surface density distribution often in detail. This fact is difficult to comprehend in the context of the dark matter paradigm where the dark halo completely dominates the gravitational potential in the low surface density systems; however it is an expected result in the context of modified Newtonian dynamics (MOND) in which the baryonic matter is the only component. With MOND the calculated rotation curves are effectively parameter-free predictions.

scholarly journals Halo acceleration relation

2019 ◽  
Vol 488 (1) ◽  
pp. L41-L46 ◽  
Author(s):  
Yong Tian (田雍) ◽  
Chung-Ming Ko (高仲明)
Keyword(s):  
Dark Matter ◽  
Spiral Galaxies ◽  
Rotation Curves ◽  
Radial Acceleration ◽  
Modified Newtonian Dynamics ◽  
Newtonian Dynamics ◽  
Total Acceleration

ABSTRACT Recently, from the new Spitzer Photometry and Accurate Rotation Curves data, McGaugh, Lelli & Schombert reported a tight radial acceleration relation between the observed total acceleration and the acceleration produced by baryons in spiral galaxies. The relation can be fitted by different functions. However, these functions can be discerned if we express the data in the form of a halo acceleration relation. The data reveals a maximum in the halo acceleration. We examined the NFW (cusp) and Burkert (core) profiles in the context of dark matter and different parameter families of the interpolating function in the framework of modified Newtonian dynamics.

Missing Mass as Evidence for Modified Newtonian Dynamics at Low Accelerations

2003 ◽  
Vol 18 (27) ◽  
pp. 1861-1875 ◽  
Author(s):  
R. H. Sanders
Keyword(s):  
Structure Formation ◽  
Spiral Galaxies ◽  
Elliptical Galaxies ◽  
Additional Parameter ◽  
Rotation Curves ◽  
Dynamical Mass ◽  
Missing Mass ◽  
Critical Acceleration ◽  
Modified Newtonian Dynamics ◽  
Newtonian Dynamics

Milgrom has proposed that the appearance of discrepancies between the Newtonian dynamical mass and the directly observable mass in astronomical systems could be due to a breakdown of Newtonian dynamics in the limit of low accelerations rather than the presence of unseen matter. Milgrom's hypothesis, modified Newtonian dynamics or MOND, has been remarkably successful in explaining systematic properties of spiral and elliptical galaxies and predicting in detail the observed rotation curves of spiral galaxies with only one additional parameter — a critical acceleration which is on the order of the cosmologically interesting value of cH0. Here we review the empirical successes of this idea and discuss its possible extension to cosmology and structure formation.

scholarly journals Newtonian and modified newtonian gravitational simulation of spiral galaxies

2019 ◽  
Vol 11 (21) ◽  
pp. 20-27
Author(s):  
Bushra A. Ahmed
Keyword(s):  
Dark Matter ◽  
Rotation Curve ◽  
Spiral Galaxies ◽  
Stellar Dynamics ◽  
Gravitational Attraction ◽  
Rotation Curves ◽  
Modified Newtonian Dynamics ◽  
Newtonian Dynamics ◽  
Rotational Curve ◽  
Good Agreement

One of the most powerful tools for any stellar dynamics is the N-body simulation. In an N-body simulation the motion of N particles is followed under their mutual gravitational attraction. In this paper the gravitational N-body simulation is described to investigate Newtonian and non- Newtonian (modified Newtonian dynamics) interaction between the stars of spiral galaxies. It is shown that standard Newtonian interaction requires dark matter to produce the flat rotational curves of the systems under consideration, while modified Newtonian dynamics (MOND) theorem provides a flat rotational curve and gives a good agreement with the observed rotation curve; MOND was tested as an alternative to the dark matter hypothesis. So that MOND hypothesis has generated better rotation curves than Newtonian theorem.

Sign in / Sign up

Export Citation Format

Share Document