Why Does 'a' Being Smaller Than 'a0' Eliminate μ in MOND?

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SUMMARY

The discussion centers on the Modified Newtonian Dynamics (MOND) theory and its implications for understanding galaxy rotation curves. Participants clarify that when the acceleration 'a' is smaller than the critical acceleration 'a0', the interpolation function μ becomes irrelevant, leading to a simplification in the equations. The conversation highlights the challenges of MOND, particularly its reliance on arbitrary 'fudge factors' and the lack of a consistent underlying theory, which contrasts with the more robust dark matter theory that explains a wider range of astronomical observations.

PREREQUISITES
  • Understanding of Modified Newtonian Dynamics (MOND)
  • Familiarity with gravitational theories and their applications in astrophysics
  • Knowledge of interpolation functions and their mathematical implications
  • Basic concepts of dark matter and its role in cosmology
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  • Research the mathematical formulation of MOND and its interpolation function μ(x)
  • Explore the differences between MOND and dark matter theories in explaining galaxy dynamics
  • Investigate the implications of MOND on large-scale structures in the universe
  • Examine case studies of Low Surface Brightness (LSB) galaxies and MOND predictions
USEFUL FOR

Astronomers, astrophysicists, and students of cosmology seeking to understand the complexities of galaxy dynamics and the ongoing debate between MOND and dark matter theories.

  • #31
mesa said:
I'm a little surprised that would work, how is the integretion setup? Is it a function of the gravity of each sun and it's affect on the next by putting together an artificail layout based on average distances apart or is it simply the sum of all the masses thrown into the center for the swept area of the galaxy by a particular star?

I was told by an astrophysicist that it has only been recently that papers were published changing the model from a spherical density to a more disc like shape, I found this surprising as well.

I don't know the practical details. For a simple case, I guess one could assume one could treat the mass as a series of rings of varying density surrounding a spherical nucleus. In a more complex cases one could use numerical methods to sum the effects of mass density over a modeled shape of the galaxy consistent with the observations. There's certainly no need to model the individual stars, because from sufficient distance the gravitational effect is essentially the same as that of a continuous medium with an appropriate average density.
 
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  • #32
Jonathan Scott said:
I don't know the practical details. For a simple case, I guess one could assume one could treat the mass as a series of rings of varying density surrounding a spherical nucleus. In a more complex cases one could use numerical methods to sum the effects of mass density over a modeled shape of the galaxy consistent with the observations. There's certainly no need to model the individual stars, because from sufficient distance the gravitational effect is essentially the same as that of a continuous medium with an appropriate average density.

Where do you think would be a good place to start to find the actual formulas used for these calculations? I looked online and came up with very little. Are there members on the board that would be helpful?

I am going to quiz the proffesors at school again and see if I can get a more complete answer. I was told by one it was basically the same as you stated originally; the mass is essentially summed and put into the center and then calculated.

That seems overly simplified and frankly I don't see how that could calculate anything properly.
 

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