MOND from galaxies that are fractal

[kodama]

TL;DR Summary

origin of the MOND critical acceleration scale

I found these papers,

the first is that galaxies are fractal based on observation

Fractal Analysis of the UltraVISTA Galaxy Survey
Sharon Teles (1), Amanda R. Lopes (2), Marcelo B. Ribeiro (1,3) ((1) Valongo Observatory, Universidade Federal do Rio de Janeiro, Brazil, (2) Department of Astronomy, Observatório Nacional, Rio de Janeiro, Brazil, (3) Physics Institute, Universidade Federal do Rio de Janeiro, Brazil)

This paper seeks to test if the large-scale galaxy distribution can be characterized as a fractal system.

the second paper calculates

Gravitational force distribution in fractal structures
A. Gabrielli, F. Sylos Labini, S. Pellegrini

https://www.researchgate.net/publication/1840875_Gravitational_force_distribution_in_fractal_structures

so if galaxies are fractal, and Gravitational force distribution in fractal structures

putting both sets of ideas together there's this paper

arXiv:2111.01700

The origin of the MOND critical acceleration scale
David Roscoe

The irrefutable successes of MOND are predicated upon the idea that a critical gravitational acceleration scale, a0, exists. But, beyond its role in MOND, the question: 'Why should a critical gravitational acceleration scale exist at all?' remains unanswered. There is no deep understanding about what is going on.
Over roughly the same period that MOND has been a topic of controversy, Baryshev, Sylos Labini, Pietronero and others have been arguing, with equal controversy in earlier years, that, on medium scales at least, material in the universe is distributed in a quasi-fractal D≈2 fashion. There is a link: if the idea of a quasi-fractal D≈2 universe on medium scales is taken seriously then there is an associated characteristic mass surface density scale, ΣF say, and an associated characteristic gravitational acceleration scale, aF=4πGΣF. If, furthermore, the quasi-fractal structure is taken to include the inter-galactic medium, then it is an obvious step to consider the possibility that a0 and aF are the same thing.
Through the lens of very old ideas rooted in a Leibniz-Mach worldview we obtain a detailed understanding of the critical acceleration scale which, applied to the SPARC sample of galaxies with a stellar MLR, Υ∗∈(0.5,1.0), and using standard photometric mass models, provides a finite algorithm to recover the information that aF≈1.2×10−10mtrs/sec2. This, combined with the fact that the Baryonic Tully-Fisher Relationship (BTFR) arises directly from the same source, but with a0 replaced by aF, leads to the unambiguous conclusion that a0 and aF are, in fact, one and the same thing.

Comments: arXiv admin note: substantial text overlap with arXiv:2006.08148
Subjects: Astrophysics of Galaxies (astro-ph.GA)
Cite as: arXiv:2111.01700 [astro-ph.GA]

any reviews

 

[ohwilleke]

Interesting idea. On the lookout for more from these authors. Not sufficiently compelling by itself to convince me, but I don't rule it out.

 

[kodama]

[Submitted on 15 Jun 2020]

Conservative MOND from first principles​

D F Roscoe

The primary argument levelled against Milgrom's MOND is that it has no theoretical support, even though considerable effort has been expended in attempting to provide it. Against that criticism, MOND irrefutably enjoys an expanding portfolio of success and so is almost certainly tapping into something fundamental. But what?
Over roughly the same period that MOND has been a topic of controversy, Baryshev, Sylos Labini and others have been claiming, with equal controversy in earlier years, that, on medium scales at least, material in the universe is distributed in a quasi-fractal D≈2 fashion. There is a link: if the idea of a quasi-fractal D≈2 universe on medium scales is taken seriously, then there is an associated characteristic mass surface density, ΣF say, and an associated characteristic acceleration scale aF=4πGΣF.
The whole success of MOND is predicated upon the idea of a critical acceleration scale, a0. It is an obvious step to make the association a0∼aF and then to consider the MOND critical acceleration boundary simply as a marker for a characteristic mass surface density boundary separating 'galaxy' from an environment characterized by ΣF. This provides a route to the synthesis of conservative MOND from first principles.
The radial acceleration relation (RAR) for conservative MOND when applied to the SPARC sample is the unity line. There is no mass discrepancy.

Comments:	42 pages. 6 figures
Subjects:	Astrophysics of Galaxies (astro-ph.GA)
Cite as:	arXiv:2006.08148 [astro-ph.GA]

 

[kodama]

Submitted on 10 Aug 2021]

The Dependence of the Hierarchical Distribution of Star Clusters on Galactic Environment​

Shyam H. Menon, Kathryn Grasha, Bruce G. Elmegreen, Christoph Federrath, Mark R. Krumholz, Daniela Calzetti, Néstor Sánchez, Sean T. Linden, Angela Adamo, Matteo Messa, David O. Cook, Daniel A. Dale, Eva K. Grebel, Michele Fumagalli, Elena Sabbi, Kelsey E. Johnson, Linda J. Smith, Robert C. Kennicutt

We use the angular Two Point Correlation Function (TPCF) to investigate the hierarchical distribution of young star clusters in 12 local (3--18 Mpc) star-forming galaxies using star cluster catalogues obtained with the \textit{Hubble Space Telescope} (\textit{HST}) as part of the Treasury Program LEGUS (Legacy ExtraGalactic UV Survey). The sample spans a range of different morphological types, allowing us to infer how the physical properties of the galaxy affect the spatial distribution of the clusters. We also prepare a range of physically motivated toy models to compare with and interpret the observed features in the TPCFs. We find that, conforming to earlier studies, young clusters ($T \la 10\, \mathrm{Myr}$) have power-law TPCFs that are characteristic of fractal distributions with a fractal dimension D2, and this scale-free nature extends out to a maximum scale lcorr beyond which the distribution becomes Poissonian. However, lcorr, and D2 vary significantly across the sample, and are correlated with a number of host galaxy physical properties, suggesting that there are physical differences in the underlying star cluster distributions. We also find that hierarchical structuring weakens with age, evidenced by flatter TPCFs for older clusters ($T \ga 10\, \mathrm{Myr}$), that eventually converges to the residual correlation expected from a completely random large-scale radial distribution of clusters in the galaxy in ∼100Myr. Our study demonstrates that the hierarchical distribution of star clusters evolves with age, and is strongly dependent on the properties of the host galaxy environment.

Comments:	19 pages, 8 figures. Accepted for publication in MNRAS. Code for analysis and reproducing results available at this https URL
Subjects:	Astrophysics of Galaxies (astro-ph.GA); Solar and Stellar Astrophysics (astro-ph.SR)
Cite as:	arXiv:2108.04387 [astro-ph.GA]

 

[kodama]

Observational evidence of fractality in the large-scale distribution of galaxies​

T. Canavesi, T.E. Tapia

Using a sample of 133 991 galaxies distributed in the sky region 100∘<α<270∘ and 7∘<δ<65∘, extracted from the SDSS NASA/AMES Value Added Galaxy Catalog (AMES-VAGC), we estimate the fractal dimension using two different methods. First, using an algorithm to estimate the correlation dimension. The second method, in a novel approach, creates a graph from the data and estimates the graph dimension purely from connectivity information. In both methods we found a dimension D≈2 in scales below 20 Mpc, which agrees with previous works. This result shows the non-homogeneity of galaxies distribution at certain scales.

Subjects:	Cosmology and Nongalactic Astrophysics (astro-ph.CO)
Cite as:	arXiv:2102.09010 [astro-ph.CO]

 

[kodama]

[Submitted on 27 Oct 2020]

Hierarchical star formation in nearby galaxies​

María Jimena Rodríguez, Gustavo Baume, Carlos Feinstein

Aims: The purpose of this work is to study the properties of the spatial distribution of the young population in three nearby galaxies in order to better understand the first stages of star formation.
Methods: We used ACS/HST photometry and the "path-linkage criterion" in order to obtain a catalog of young stellar groups (YSGs) in the galaxy NGC 2403. We studied the internal distribution of stars in these YSGs using the Q parameter. We extended these analyses to the YSGs detected in in NGC 300 and NGC 253 our previous works. We built the young stars' density maps for these three galaxies. Through these maps, we were able to identify and study young stellar structures on larger scales.
Results: We found 573 YSGs in the galaxy NGC 2403, for which we derived their individual sizes, densities, luminosity function,and other fundamental characteristics. We find that the vast majority of the YSGs in NGC 2403, NGC 300 and NGC 253 present inner clumpings, following the same hierarchical behavior that we observed in the young stellar structures on larger scales in these galaxies. We derived values of the fractal dimension for these structures between ~ 1.5 and 1.6. These values are very similar to those obtained in other star forming galaxies and in the interstellar medium, suggesting that the star formation process is regulated by supersonic turbulence.

Comments:	10 pages, 10 figures, 2 tables, Accepted for publication in A&A
Subjects:	Astrophysics of Galaxies (astro-ph.GA)
Cite as:	arXiv:2010.14419 [astro-ph.GA]

 

[kodama]

Field Fractal Cosmological Model As an Example of Practical Cosmology Approach​

Yu. V. Baryshev (Astron.Inst.St.-Petersburg Univ.)

The idea of the global gravitational effect as the source of cosmological redshift was considered by de Sitter (1916, 1917), Eddington (1923), Tolman (1929) and Bondi (1947). Also Hubble (1929) called the discovered distance-redshift relation as "De Sitter effect". For homogeneous matter distribution cosmological gravitational redshift is proportional to square of distance: z_grav ~ r^2. However for a fractal matter distribution having the fractal dimension D=2 the global gravitational redshift is the linear function of distance: z_grav ~ r, which gives possibility for interpretation of the Hubble law without the space expansion. Here the field gravity fractal cosmological model (FGF) is presented, which based on two initial principles. The first assumption is that the Feynman's field gravity approach describes the gravitational interaction, which delivers a natural basis for the conceptual unity of all fundamental physical interactions within the framework of the relativistic and quantum fields in Minkowski space. The second hypothesis is that the spatial distribution of gravitating matter is a fractal at all scales up to the Hubble radius. The fractal dimension of matter distribution is assumed to be D = 2, which implies that the global gravitational redshift is the explanation of the observed linear Hubble law. In the frame of the FGF all three phenomena - the cosmic background radiation, the fractal large scale structure, and the Hubble law, - could be the consequence of a unique large scale structure evolution process of the initially homogeneous ordinary matter without nonbaryonic matter and dark energy.

Comments:	text and misprints corrected, 8 pages, proceedings of the International conference "Problems of Practical Cosmology", 23-27 June 2008, St.-Petersburg, Russia, see this http URL
Subjects:	General Relativity and Quantum Cosmology (gr-qc); Astrophysics (astro-ph); Cosmology and Nongalactic Astrophysics (astro-ph.CO)
Cite as:	arXiv:0810.0162 [gr-qc]

 

[kodama]

Gravitational force distribution in fractal structures​

A. Gabrielli, F. Sylos Labini, S. Pellegrini

We study the (Newtonian) gravitational force distribution arising from a fractal set of sources. We show that, in the case of real structures in finite samples, an important role is played by morphological properties and finite size effects. For dimensions smaller than d-1 (being d the space dimension) the convergence of the net gravitational force is assured by the fast decaying of the density, while for fractal dimension D>d-1 the morphological properties of the structure determine the eventual convergence of the force as a function of distance. We clarify the role played by the cut-offs of the distribution. Some cosmological implications are discussed.

Comments:	9 pages, latex, 2 postscript figures, also available at this http URL Accepted for Publication in Europhysics Letters. Minor modifications added
Subjects:	Astrophysics (astro-ph); Condensed Matter (cond-mat)
Cite as:	arXiv:astro-ph/9809234

 

[kodama]

[Submitted on 24 Apr 2006]

Gravitational Field of Fractal Distribution of Particles​

Vasily E. Tarasov

In this paper we consider the gravitational field of fractal distribution of particles. To describe fractal distribution, we use the fractional integrals. The fractional integrals are considered as approximations of integrals on fractals. Using the fractional generalization of the Gauss's law, we consider the simple examples of the fields of homogeneous fractal distribution. The examples of gravitational moments for fractal distribution are considered.

Comments:	14 pages, LaTeX
Subjects:	Astrophysics (astro-ph); Chaotic Dynamics (nlin.CD); Classical Physics (physics.class-ph); Space Physics (physics.space-ph)
Cite as:	arXiv:astro-ph/0604491

 

[kodama]

Fractal Cosmology in an Open Universe​

M. Joyce, P. W. Anderson, M. Montuori, L. Pietronero, F. Sylos Labini

The clustering of galaxies is well characterized by fractal properties, with the presence of an eventual cross-over to homogeneity still a matter of considerable debate. In this letter we discuss the cosmological implications of a fractal distribution of matter, with a possible cross-over to homogeneity at an undetermined scale R_{homo}. Contrary to what is generally assumed, we show that, even when R_{homo} -> \infty, this possibility can be treated consistently within the framework of the expanding universe solutions of Friedmann. The fractal is a perturbation to an open cosmology in which the leading homogeneous component is the cosmic background radiation (CBR). This cosmology, inspired by the observed galaxy distributions, provides a simple explanation for the recent data which indicate the absence of deceleration in the expansion (q_o \approx 0). Correspondingly the `age problem' is also resolved. Further we show that the model can be extended back from the curvature dominated arbitrarily deep into the radiation dominated era, and we discuss qualitatively the modifications to the physics of the anisotropy of the CBR, nucleosynthesis and structure formation.

Comments:	7 pages, no figures, to appear in Europhysics Letters
Subjects:	Astrophysics (astro-ph); Condensed Matter (cond-mat); General Relativity and Quantum Cosmology (gr-qc); High Energy Physics - Phenomenology (hep-ph)
Cite as:	arXiv:astro-ph/0002504

 

[kodama]

Fractal structures and the large scale distribution of galaxies​

Luciano Pietronero, Francesco Sylos Labini

Galaxy structures are certainly fractal up to a certain crossover scale \lambda_0. A clear determination of such a scale is still missing. Usually, the conceptual and practical implications of this property are neglected and the structures are only discussed in terms of their global amplitude. Here we present a compact summary of these implications. First, we discuss the problem of the identification of the crossover scale \lambda_0 and the proper characterization of the scaling. We then consider the implications of these properties with respect to various physical phenomena and to the corresponding characteristic values, i.e. r_0, \sigma_8, \Omega, etc. These implications crucially depend on the value of \lambda_0, but they are still important for a relatively small value, say \lambda_0 \approx 50 \hmp. Finally we consider the main theoretical consequences of these results.

Comments:	27 pages, 3 figures. To appear in the proceedings of the 7th Course in astrofundamental physics, Nato Advanced Study Institute, International Euroconference Erice, 5-16 December 1999
Subjects:	Astrophysics (astro-ph)
Cite as:	arXiv:astro-ph/0002124