Galaxy rotation curve

Last updated
Rotation curve of spiral galaxy Messier 33 (yellow and blue points with error bars), and a predicted one from distribution of the visible matter (gray line). The discrepancy between the two curves can be accounted for by adding a dark matter halo surrounding the galaxy. Rotation curve of spiral galaxy Messier 33 (Triangulum).png
Rotation curve of spiral galaxy Messier 33 (yellow and blue points with error bars), and a predicted one from distribution of the visible matter (gray line). The discrepancy between the two curves can be accounted for by adding a dark matter halo surrounding the galaxy.
Left: A simulated galaxy without dark matter. Right: Galaxy with a flat rotation curve that would be expected with dark matter.

The rotation curve of a disc galaxy (also called a velocity curve) is a plot of the orbital speeds of visible stars or gas in that galaxy versus their radial distance from that galaxy's centre. It is typically rendered graphically as a plot, and the data observed from each side of a spiral galaxy are generally asymmetric, so that data from each side are averaged to create the curve. A significant discrepancy exists between the experimental curves observed, and a curve derived by applying gravity theory to the matter observed in a galaxy. Theories involving dark matter are the main postulated solutions to account for the variance. [3]

Contents

The rotational/orbital speeds of galaxies/stars do not follow the rules found in other orbital systems such as stars/planets and planets/moons that have most of their mass at the centre. Stars revolve around their galaxy's centre at equal or increasing speed over a large range of distances. In contrast, the orbital velocities of planets in planetary systems and moons orbiting planets decline with distance according to Kepler’s third law. This reflects the mass distributions within those systems. The mass estimations for galaxies based on the light they emit are far too low to explain the velocity observations. [4]

The galaxy rotation problem is the discrepancy between observed galaxy rotation curves and the theoretical prediction, assuming a centrally dominated mass associated with the observed luminous material. When mass profiles of galaxies are calculated from the distribution of stars in spirals and mass-to-light ratios in the stellar disks, they do not match with the masses derived from the observed rotation curves and the law of gravity. A solution to this conundrum is to hypothesize the existence of dark matter and to assume its distribution from the galaxy's center out to its halo.

Though dark matter is by far the most accepted explanation of the rotation problem, other proposals have been offered with varying degrees of success. Of the possible alternatives, one of the most notable is modified newtonian dynamics (MOND), which involves modifying the laws of gravity. [5]

History

In 1932, Jan Hendrik Oort became the first to report that measurements of the stars in the solar neighborhood indicated that they moved faster than expected when a mass distribution based upon visible matter was assumed, but these measurements were later determined to be essentially erroneous. [6] In 1939, Horace Babcock reported in his PhD thesis measurements of the rotation curve for Andromeda which suggested that the mass-to-luminosity ratio increases radially. [7] He attributed that to either the absorption of light within the galaxy or to modified dynamics in the outer portions of the spiral and not to any form of missing matter. Babcock's measurements turned out to disagree substantially with those found later, and the first measurement of an extended rotation curve in good agreement with modern data was published in 1957 by Henk van de Hulst and collaborators, who studied M31 with the newly commissioned Dwingeloo 25 meter telescope. [8] A companion paper by Maarten Schmidt showed that this rotation curve could be fit by a flattened mass distribution more extensive than the light. [9] In 1959, Louise Volders used the same telescope to demonstrate that the spiral galaxy M33 also does not spin as expected according to Keplerian dynamics. [10]

Reporting on NGC 3115, Jan Oort wrote that "the distribution of mass in the system appears to bear almost no relation to that of light... one finds the ratio of mass to light in the outer parts of NGC 3115 to be about 250". [11] On page 302–303 of his journal article, he wrote that "The strongly condensed luminous system appears imbedded in a large and more or less homogeneous mass of great density" and although he went on to speculate that this mass may be either extremely faint dwarf stars or interstellar gas and dust, he had clearly detected the dark matter halo of this galaxy.

The Carnegie telescope (Carnegie Double Astrograph) was intended to study this problem of Galactic rotation. [12]

In the late 1960s and early 1970s, Vera Rubin, an astronomer at the Department of Terrestrial Magnetism at the Carnegie Institution of Washington, worked with a new sensitive spectrograph that could measure the velocity curve of edge-on spiral galaxies to a greater degree of accuracy than had ever before been achieved. [13] Together with fellow staff-member Kent Ford, Rubin announced at a 1975 meeting of the American Astronomical Society the discovery that most stars in spiral galaxies orbit at roughly the same speed, [14] and that this implied that galaxy masses grow approximately linearly with radius well beyond the location of most of the stars (the galactic bulge). Rubin presented her results in an influential paper in 1980. [15] These results suggested either that Newtonian gravity does not apply universally or that, conservatively, upwards of 50% of the mass of galaxies was contained in the relatively dark galactic halo. Although initially met with skepticism, Rubin's results have been confirmed over the subsequent decades. [16]

If Newtonian mechanics is assumed to be correct, it would follow that most of the mass of the galaxy had to be in the galactic bulge near the center and that the stars and gas in the disk portion should orbit the center at decreasing velocities with radial distance from the galactic center (the dashed line in Fig. 1).

Observations of the rotation curve of spirals, however, do not bear this out. Rather, the curves do not decrease in the expected inverse square root relationship but are "flat", i.e. outside of the central bulge the speed is nearly a constant (the solid line in Fig. 1). It is also observed that galaxies with a uniform distribution of luminous matter have a rotation curve that rises from the center to the edge, and most low-surface-brightness galaxies (LSB galaxies) have the same anomalous rotation curve.

The rotation curves might be explained by hypothesizing the existence of a substantial amount of matter permeating the galaxy outside of the central bulge that is not emitting light in the mass-to-light ratio of the central bulge. The material responsible for the extra mass was dubbed dark matter, the existence of which was first posited in the 1930s by Jan Oort in his measurements of the Oort constants and Fritz Zwicky in his studies of the masses of galaxy clusters. The existence of non-baryonic cold dark matter (CDM) is today a major feature of the Lambda-CDM model that describes the cosmology of the universe.

Halo density profiles

In order to accommodate a flat rotation curve, a density profile for a galaxy and its environs must be different than one that is centrally concentrated. Newton's version of Kepler's Third Law implies that the spherically symmetric, radial density profile ρ(r) is:

where v(r) is the radial orbital velocity profile and G is the gravitational constant. This profile closely matches the expectations of a singular isothermal sphere profile where if v(r) is approximately constant then the density ρr−2 to some inner "core radius" where the density is then assumed constant. Observations do not comport with such a simple profile, as reported by Navarro, Frenk, and White in a seminal 1996 paper. [17]

The authors then remarked that a "gently changing logarithmic slope" for a density profile function could also accommodate approximately flat rotation curves over large scales. They found the famous Navarro–Frenk–White profile, which is consistent both with N-body simulations and observations given by

where the central density, ρ0, and the scale radius, Rs, are parameters that vary from halo to halo. [18] Because the slope of the density profile diverges at the center, other alternative profiles have been proposed, for example the Einasto profile, which has exhibited better agreement with certain dark matter halo simulations. [19] [20]

Observations of orbit velocities in spiral galaxies suggest a mass structure according to:

with Φ the galaxy gravitational potential.

Since observations of galaxy rotation do not match the distribution expected from application of Kepler's laws, they do not match the distribution of luminous matter. [15] This implies that spiral galaxies contain large amounts of dark matter or, alternatively, the existence of exotic physics in action on galactic scales. The additional invisible component becomes progressively more conspicuous in each galaxy at outer radii and among galaxies in the less luminous ones.[ clarification needed ]

A popular interpretation of these observations is that about 26% of the mass of the Universe is composed of dark matter, a hypothetical type of matter which does not emit or interact with electromagnetic radiation. Dark matter is believed to dominate the gravitational potential of galaxies and clusters of galaxies. Under this theory, galaxies are baryonic condensations of stars and gas (namely hydrogen and helium) that lie at the centers of much larger haloes of dark matter, affected by a gravitational instability caused by primordial density fluctuations.

Many cosmologists strive to understand the nature and the history of these ubiquitous dark haloes by investigating the properties of the galaxies they contain (i.e. their luminosities, kinematics, sizes, and morphologies). The measurement of the kinematics (their positions, velocities and accelerations) of the observable stars and gas has become a tool to investigate the nature of dark matter, as to its content and distribution relative to that of the various baryonic components of those galaxies.

Further investigations

Comparison of rotating disc galaxies in the present day (left) and the distant Universe (right). Comparison of rotating disc galaxies in the distant Universe and the present day.jpg
Comparison of rotating disc galaxies in the present day (left) and the distant Universe (right).

The rotational dynamics of galaxies are well characterized by their position on the Tully–Fisher relation, which shows that for spiral galaxies the rotational velocity is uniquely related to their total luminosity. A consistent way to predict the rotational velocity of a spiral galaxy is to measure its bolometric luminosity and then read its rotation rate from its location on the Tully–Fisher diagram. Conversely, knowing the rotational velocity of a spiral galaxy gives its luminosity. Thus the magnitude of the galaxy rotation is related to the galaxy's visible mass. [22]

While precise fitting of the bulge, disk, and halo density profiles is a rather complicated process, it is straightforward to model the observables of rotating galaxies through this relationship. [23] [ better source needed ] So, while state-of-the-art cosmological and galaxy formation simulations of dark matter with normal baryonic matter included can be matched to galaxy observations, there is not yet any straightforward explanation as to why the observed scaling relationship exists. [24] [25] Additionally, detailed investigations of the rotation curves of low-surface-brightness galaxies (LSB galaxies) in the 1990s [26] and of their position on the Tully–Fisher relation [27] showed that LSB galaxies had to have dark matter haloes that are more extended and less dense than those of galaxies with high surface brightness, and thus surface brightness is related to the halo properties. Such dark-matter-dominated dwarf galaxies may hold the key to solving the dwarf galaxy problem of structure formation.

Very importantly, the analysis of the inner parts of low and high surface brightness galaxies showed that the shape of the rotation curves in the centre of dark-matter dominated systems indicates a profile different from the NFW spatial mass distribution profile. [28] [29] This so-called cuspy halo problem is a persistent problem for the standard cold dark matter theory. Simulations involving the feedback of stellar energy into the interstellar medium in order to alter the predicted dark matter distribution in the innermost regions of galaxies are frequently invoked in this context. [30] [31]

Alternatives to dark matter

There have been a number of attempts to solve the problem of galaxy rotation by modifying gravity without invoking dark matter. One of the most discussed is Modified Newtonian Dynamics (MOND), originally proposed by Mordehai Milgrom in 1983, which modifies the Newtonian force law at low accelerations to enhance the effective gravitational attraction. MOND has had a considerable amount of success in predicting the rotation curves of low-surface-brightness galaxies, [32] matching the baryonic Tully–Fisher relation, [33] and the velocity dispersions of the small satellite galaxies of the Local Group. [34]

Using data from the Spitzer Photometry and Accurate Rotation Curves (SPARC) database, a group has found that the radial acceleration traced by rotation curves could be predicted just from the observed baryon distribution (that is, including stars and gas but not dark matter). [35] The same relation provided a good fit for 2693 samples in 153 rotating galaxies, with diverse shapes, masses, sizes, and gas fractions. Brightness in the near infrared, where the more stable light from red giants dominates, was used to estimate the density contribution due to stars more consistently. The results are consistent with MOND, and place limits on alternative explanations involving dark matter alone. However, cosmological simulations within a Lambda-CDM framework that include baryonic feedback effects reproduce the same relation, without the need to invoke new dynamics (such as MOND). [36] Thus, a contribution due to dark matter itself can be fully predictable from that of the baryons, once the feedback effects due to the dissipative collapse of baryons are taken into account. MOND is not a relativistic theory, although relativistic theories which reduce to MOND have been proposed, such as tensor–vector–scalar gravity (TeVeS), [5] [37] scalar–tensor–vector gravity (STVG), and the f(R) theory of Capozziello and De Laurentis. [38]

A model of galaxy based on a general relativity metric was also proposed, showing that the rotation curves for the Milky Way, NGC 3031, NGC 3198 and NGC 7331 are consistent with the mass density distributions of the visible matter, avoiding the need for a massive halo of exotic dark matter. [39] [40]

According to a 2020 analysis of the data produced by the Gaia spacecraft, it would seem possible to explain at least the Milky Way's rotation curve without requiring any dark matter if instead of a Newtonian approximation the entire set of equations of general relativity is adopted. [41]

In March 2021, Gerson Otto Ludwig published a model based on general relativity that explains galaxy rotation curves with gravitoelectromagnetism. [42]

See also

Footnotes

  1. Corbelli, E.; Salucci, P. (2000). "The extended rotation curve and the dark matter halo of M33". Monthly Notices of the Royal Astronomical Society . 311 (2): 441–447. arXiv: astro-ph/9909252 . Bibcode: 2000MNRAS.311..441C . doi: 10.1046/j.1365-8711.2000.03075.x .
  2. The explanation of the mass discrepancy in spiral galaxies by means of massive and extensive dark component was first put forward by A. Bosma in a PhD dissertation, see
    Bosma, A. (1978). The Distribution and Kinematics of Neutral Hydrogen in Spiral Galaxies of Various Morphological Types (PhD). Rijksuniversiteit Groningen . Retrieved December 30, 2016 via NASA/IPAC Extragalactic Database.
    See also
    Rubin, V.; Thonnard, N.; Ford, W. K. Jr. (1980). "Rotational Properties of 21 Sc Galaxies With a Large Range of Luminosities and Radii from NGC 4605 (R=4kpc) to UGC 2885 (R=122kpc)". The Astrophysical Journal . 238: 471–487. Bibcode: 1980ApJ...238..471R . doi: 10.1086/158003 .
    Begeman, K. G.; Broeils, A. H.; Sanders, R.H. (1991). "Extended Rotation Curves of Spiral Galaxies: Dark Haloes and Modified Dynamics". Monthly Notices of the Royal Astronomical Society . 249 (3): 523–537. Bibcode: 1991MNRAS.249..523B . doi: 10.1093/mnras/249.3.523 .
  3. Hammond, Richard (May 1, 2008). The Unknown Universe: The Origin of the Universe, Quantum Gravity, Wormholes, and Other Things Science Still Can't Explain. Franklin Lakes, NJ: Career Press.
  4. Bosma, A. (1978). The Distribution and Kinematics of Neutral Hydrogen in Spiral Galaxies of Various Morphological Types (PhD). Rijksuniversiteit Groningen . Retrieved December 30, 2016 via NASA/IPAC Extragalactic Database.
  5. 1 2 For an extensive discussion of the data and its fit to MOND see Milgrom, M. (2007). "The MOND Paradigm". arXiv: 0801.3133 [astro-ph].
  6. Oxford Dictionary of Scientists. Oxford: Oxford University Press. 1999. ISBN   978-0-19-280086-2.
  7. Babcock, H. W. (1939). "The rotation of the Andromeda Nebula". Lick Observatory Bulletin . 19: 41–51. Bibcode: 1939LicOB..19...41B . doi: 10.5479/ADS/bib/1939LicOB.19.41B .
  8. Van de Hulst, H.C; et al. (1957). "Rotation and density distribution of the Andromeda nebula derived from observations of the 21-cm line". Bulletin of the Astronomical Institutes of the Netherlands . 14: 1. Bibcode: 1957BAN....14....1V .
  9. Schmidt, M (1957). "Rotation and density distribution of the Andromeda nebula derived from observations of the 21-cm line". Bulletin of the Astronomical Institutes of the Netherlands . 14: 17. Bibcode: 1957BAN....14...17S .
  10. Volders, L. (1959). "Neutral hydrogen in M 33 and M 101". Bulletin of the Astronomical Institutes of the Netherlands . 14 (492): 323. Bibcode: 1959BAN....14..323V .
  11. Oort, J.H. (1940), Some Problems Concerning the Structure and Dynamics of the Galactic System and the Elliptical Nebulae NGC 3115 and 4494
  12. "1947PASP...59..182S Page 182". adsabs.harvard.edu. Retrieved 2019-11-17.
  13. Rubin, V.; Ford, W. K. Jr. (1970). "Rotation of the Andromeda Nebula from a Spectroscopic Survey of Emission Regions". The Astrophysical Journal . 159: 379. Bibcode: 1970ApJ...159..379R . doi: 10.1086/150317 .
  14. Rubin, V.C.; Thonnard, N.; Ford, W.K. Jr. (1978). "Extended rotation curves of high-luminosity spiral galaxies. IV – Systematic dynamical properties, SA through SC". The Astrophysical Journal Letters . 225: L107–L111. Bibcode: 1978ApJ...225L.107R . doi: 10.1086/182804 .
  15. 1 2 Rubin, V.; Thonnard, N.; Ford, W. K. Jr. (1980). "Rotational Properties of 21 Sc Galaxies with a Large Range of Luminosities and Radii from NGC 4605 (R=4kpc) to UGC 2885 (R=122kpc)". The Astrophysical Journal . 238: 471. Bibcode: 1980ApJ...238..471R . doi: 10.1086/158003 .
  16. Persic, M.; Salucci, P.; Stel, F. (1996). "The universal rotation curve of spiral galaxies – I. The dark matter connection". Monthly Notices of the Royal Astronomical Society . 281 (1): 27–47. arXiv: astro-ph/9506004 . Bibcode: 1996MNRAS.281...27P . doi: 10.1093/mnras/278.1.27 .
  17. Navarro, J. F.; Frenk, C. S.; White, S. D. M. (1996). "The Structure of Cold Dark Matter Halos". The Astrophysical Journal . 463: 563. arXiv: astro-ph/9508025 . Bibcode: 1996ApJ...462..563N . doi: 10.1086/177173 .
  18. Ostlie, Dale A.; Carroll, Bradley W. (2017). An Introduction to Modern Astrophysics. Cambridge University Press. p. 918.
  19. Merritt, D.; Graham, A.; Moore, B.; Diemand, J.; Terzić, B. (2006). "Empirical Models for Dark Matter Halos. I. Nonparametric Construction of Density Profiles and Comparison with Parametric Models". The Astronomical Journal . 132 (6): 2685–2700. arXiv: astro-ph/0509417 . Bibcode: 2006AJ....132.2685M . doi: 10.1086/508988 .
  20. Merritt, D.; Navarro, J. F.; Ludlow, A.; Jenkins, A. (2005). "A Universal Density Profile for Dark and Luminous Matter?". The Astrophysical Journal . 624 (2): L85–L88. arXiv: astro-ph/0502515 . Bibcode: 2005ApJ...624L..85M . doi: 10.1086/430636 .
  21. "Dark Matter Less Influential in Galaxies in Early Universe – VLT observations of distant galaxies suggest they were dominated by normal matter". www.eso.org. Retrieved 16 March 2017.
  22. Yegorova, I. A.; Salucci, P. (2007). "The radial Tully-Fisher relation for spiral galaxies – I". Monthly Notices of the Royal Astronomical Society . 377 (2): 507–515. arXiv: astro-ph/0612434 . Bibcode:2007MNRAS.377..507Y. doi:10.1111/j.1365-2966.2007.11637.x.
  23. Dorminey, Bruce (30 Dec 2010). "Reliance on Indirect Evidence Fuels Dark Matter Doubts". Scientific American.
  24. Weinberg, David H.; et, al. (2008). "Baryon Dynamics, Dark Matter Substructure, and Galaxies". The Astrophysical Journal. 678 (1): 6–21. arXiv: astro-ph/0604393 . Bibcode:2008ApJ...678....6W. doi:10.1086/524646.
  25. Duffy, Alan R.; al., et (2010). "Impact of baryon physics on dark matter structures: a detailed simulation study of halo density profiles". Monthly Notices of the Royal Astronomical Society. 405 (4): 2161–2178. arXiv: 1001.3447 . Bibcode:2010MNRAS.405.2161D. doi:10.1111/j.1365-2966.2010.16613.x.
  26. de Blok, W. J. G.; McGaugh, S. (1997). "The dark and visible matter content of low surface brightness disc galaxies". Monthly Notices of the Royal Astronomical Society . 290 (3): 533–552. arXiv: astro-ph/9704274 . Bibcode:1997MNRAS.290..533D. doi:10.1093/mnras/290.3.533.
  27. Zwaan, M. A.; van der Hulst, J. M.; de Blok, W. J. G.; McGaugh, S. S. (1995). "The Tully-Fisher relation for low surface brightness galaxies: implications for galaxy evolution". Monthly Notices of the Royal Astronomical Society . 273: L35–L38. arXiv: astro-ph/9501102 . Bibcode:1995MNRAS.273L..35Z. doi:10.1093/mnras/273.1.l35.
  28. Gentile, G.; Salucci, P.; Klein, U.; Vergani, D.; Kalberla, P. (2004). "The cored distribution of dark matter in spiral galaxies". Monthly Notices of the Royal Astronomical Society. 351 (3): 903–922. arXiv: astro-ph/0403154 . Bibcode:2004MNRAS.351..903G. doi:10.1111/j.1365-2966.2004.07836.x.
  29. de Blok, W. J. G.; Bosma, A. (2002). "High-resolution rotation curves of low surface brightness galaxies" (PDF). Astronomy & Astrophysics . 385 (3): 816–846. arXiv: astro-ph/0201276 . Bibcode:2002A&A...385..816D. doi:10.1051/0004-6361:20020080.
  30. Salucci, P.; De Laurentis, M. (2012). "Dark Matter in galaxies: Leads to its Nature" (PDF). Proceedings of Science (DSU 2012): 12. arXiv: 1302.2268 . Bibcode:2013arXiv1302.2268S.
  31. de Blok, W. J. G. (2010). "The Core-Cusp Problem". Advances in Astronomy . 2010: 789293. arXiv: 0910.3538 . Bibcode:2010AdAst2010E...5D. doi:10.1155/2010/789293.
  32. S. S. McGaugh; W. J. G. de Blok (1998). "Testing the Hypothesis of Modified Dynamics with Low Surface Brightness Galaxies and Other Evidence". Astrophysical Journal. 499 (1): 66–81. arXiv: astro-ph/9801102 . Bibcode:1998ApJ...499...66M. doi:10.1086/305629.
  33. S. S. McGaugh (2011). "Novel Test of Modified Newtonian Dynamics with Gas Rich Galaxies". Physical Review Letters. 106 (12): 121303. arXiv: 1102.3913 . Bibcode:2011PhRvL.106l1303M. doi:10.1103/PhysRevLett.106.121303. PMID   21517295.
  34. S. S. McGaugh; M. Milgrom (2013). "Andromeda Dwarfs in Light of Modified Newtonian Dynamics". The Astrophysical Journal. 766 (1): 22. arXiv: 1301.0822 . Bibcode:2013ApJ...766...22M. doi:10.1088/0004-637X/766/1/22.
  35. Stacy McGaugh; Federico Lelli; Jim Schombert (2016). "The Radial Acceleration Relation in Rotationally Supported Galaxies". Physical Review Letters. 117 (20): 201101. arXiv: 1609.05917 . Bibcode:2016PhRvL.117t1101M. doi:10.1103/physrevlett.117.201101. PMID   27886485.
  36. Keller, B. W.; Wadsley, J. W. (23 January 2017). "Λ is Consistent with SPARC Radial Acceleration Relation". The Astrophysical Journal. 835 (1): L17. arXiv: 1610.06183 . Bibcode:2017ApJ...835L..17K. doi:10.3847/2041-8213/835/1/L17.
  37. J. D. Bekenstein (2004). "Relativistic gravitation theory for the modified Newtonian dynamics paradigm". Physical Review D. 70 (8): 083509. arXiv: astro-ph/0403694 . Bibcode:2004PhRvD..70h3509B. doi:10.1103/PhysRevD.70.083509.
  38. J. W. Moffat (2006). "Scalar tensor vector gravity theory". Journal of Cosmology and Astroparticle Physics. 3 (3): 4. arXiv: gr-qc/0506021 . Bibcode:2006JCAP...03..004M. doi:10.1088/1475-7516/2006/03/004..S. Capozziello; M. De Laurentis (2012). "The dark matter problem from f(R) gravity viewpoint". Annalen der Physik. 524 (9–10): 545–578. Bibcode:2012AnP...524..545C. doi: 10.1002/andp.201200109 .
  39. Cooperstock, Fred I., and S. Tieu. "General relativity resolves galactic rotation without exotic dark matter." arXiv preprint astro-ph/0507619 (2005).
  40. Cooperstock, F. I.; Tieu, S. (2007-05-20). "GALACTIC DYNAMICS VIA GENERAL RELATIVITY: A COMPILATION AND NEW DEVELOPMENTS". International Journal of Modern Physics A. 22 (13): 2293–2325. arXiv: astro-ph/0610370 . doi:10.1142/S0217751X0703666X. ISSN   0217-751X.
  41. Crosta, Mariateresa; Giammaria, Marco; Lattanzi, Mario G.; Poggio, Eloisa (August 2020). "On testing CDM and geometry-driven Milky Way rotation curve models with Gaia DR2". Monthly Notices of the Royal Astronomical Society . OUP. 496 (2): 2107–2122. arXiv: 1810.04445 . doi:10.1093/mnras/staa1511.
  42. Ludwig, G. O. (2021-02-23). "Galactic rotation curve and dark matter according to gravitomagnetism". The European Physical Journal C. 81 (2): 186. doi: 10.1140/epjc/s10052-021-08967-3 .

Further reading

Bibliography

Related Research Articles

Dark matter Hypothetical form of matter comprising most of the matter in the universe

Dark matter is a hypothetical form of matter thought to account for approximately 85% of the matter in the universe. Its presence is implied in a variety of astrophysical observations, including gravitational effects that cannot be explained by accepted theories of gravity unless more matter is present than can be seen. For this reason, most experts think that dark matter is abundant in the universe and that it has had a strong influence on its structure and evolution. Dark matter is called dark because it does not appear to interact with the electromagnetic field, which means it does not absorb, reflect or emit electromagnetic radiation, and is therefore difficult to detect.

Galaxy formation and evolution from a homogeneous beginning, the formation of the first galaxies, the way galaxies change over time

The study of galaxy formation and evolution is concerned with the processes that formed a heterogeneous universe from a homogeneous beginning, the formation of the first galaxies, the way galaxies change over time, and the processes that have generated the variety of structures observed in nearby galaxies. Galaxy formation is hypothesized to occur from structure formation theories, as a result of tiny quantum fluctuations in the aftermath of the Big Bang. The simplest model in general agreement with observed phenomena is the Lambda-CDM model—that is, that clustering and merging allows galaxies to accumulate mass, determining both their shape and structure.

Andromeda Galaxy Barred spiral galaxy within the Local Group

The Andromeda Galaxy, also known as Messier 31, M31, or NGC 224 and originally the Andromeda Nebula, is a barred spiral galaxy approximately 2.5 million light-years from Earth and the nearest large galaxy to the Milky Way. The galaxy's name stems from the area of Earth's sky in which it appears, the constellation of Andromeda, which itself is named after the Ethiopian princess who was the wife of Perseus in Greek mythology.

In cosmology and physics, cold dark matter (CDM) is a hypothetical type of dark matter. Observations indicate that approximately 85% of the matter in the universe is dark matter, with only a small fraction being the ordinary baryonic matter that composes stars, planets, and living organisms. Cold refers to the fact that the dark matter moves slowly compared to the speed of light, while dark indicates that it interacts very weakly with ordinary matter and electromagnetic radiation.

Spiral galaxy Class of galaxy having a number of arms of younger stars

Spiral galaxies form a class of galaxy originally described by Edwin Hubble in his 1936 work The Realm of the Nebulae and, as such, form part of the Hubble sequence. Most spiral galaxies consist of a flat, rotating disk containing stars, gas and dust, and a central concentration of stars known as the bulge. These are often surrounded by a much fainter halo of stars, many of which reside in globular clusters.

Galactic bulge Tightly packed group of stars within a larger formation

In astronomy, a galactic bulge is a tightly packed group of stars within a larger star formation. The term almost exclusively refers to the central group of stars found in most spiral galaxies. Bulges were historically thought to be elliptical galaxies that happened to have a disk of stars around them, but high-resolution images using the Hubble Space Telescope have revealed that many bulges lie at the heart of a spiral galaxy. It is now thought that there are at least two types of bulges: bulges that are like ellipticals and bulges that are like spiral galaxies.

Tully–Fisher relation Trend in astronomy

In astronomy, the Tully–Fisher relation (TFR) is an empirical relationship between the mass or intrinsic luminosity of a spiral galaxy and its asymptotic rotation velocity or emission line width. It was first published in 1977 by astronomers R. Brent Tully and J. Richard Fisher. The luminosity is calculated by multiplying the galaxy's apparent brightness by , where is its distance from us, and the spectral-line width is measured using long-slit spectroscopy.

A galactic halo is an extended, roughly spherical component of a galaxy which extends beyond the main, visible component. Several distinct components of galaxies comprise the halo:

The cuspy halo problem refers to a discrepancy between the inferred dark matter density profiles of low-mass galaxies and the density profiles predicted by cosmological N-body simulations. Nearly all simulations form dark matter halos which have "cuspy" dark matter distributions, with density increasing steeply at small radii, while the rotation curves of most observed dwarf galaxies suggest that they have flat central dark matter density profiles ("cores").

Dark matter halo A theoretical component of a galaxy that envelops the galactic disc and extends well beyond the edge of the visible galaxy

According to modern models of physical cosmology, a dark matter halo is a basic unit of cosmological structure. It is a hypothetical region that has decoupled from cosmic expansion and contains gravitationally bound matter. A single dark matter halo may contain multiple virialized clumps of dark matter bound together by gravity, known as subhalos. Modern cosmological models, such as ΛCDM, propose that dark matter halos and subhalos may contain galaxies. The dark matter halo of a galaxy envelops the galactic disc and extends well beyond the edge of the visible galaxy. Thought to consist of dark matter, halos have not been observed directly. Their existence is inferred through observations of their effects on the motions of stars and gas in galaxies and gravitational lensing. Dark matter halos play a key role in current models of galaxy formation and evolution. Theories that attempt to explain the nature of dark matter halos with varying degrees of success include cold dark matter (CDM), warm dark matter, and massive compact halo objects (MACHOs).

Milky Way Barred spiral galaxy containing our Solar System

The Milky Way is the galaxy that includes the Solar System, with the name describing the galaxy's appearance from Earth: a hazy band of light seen in the night sky formed from stars that cannot be individually distinguished by the naked eye. The term Milky Way is a translation of the Latin via lactea, from the Greek γαλακτικός κύκλος, meaning "milky circle." From Earth, the Milky Way appears as a band because its disk-shaped structure is viewed from within. Galileo Galilei first resolved the band of light into individual stars with his telescope in 1610. Until the early 1920s, most astronomers thought that the Milky Way contained all the stars in the Universe. Following the 1920 Great Debate between the astronomers Harlow Shapley and Heber Curtis, observations by Edwin Hubble showed that the Milky Way is just one of many galaxies.

The Navarro–Frenk–White (NFW) profile is a spatial mass distribution of dark matter fitted to dark matter halos identified in N-body simulations by Julio Navarro, Carlos Frenk and Simon White. The NFW profile is one of the most commonly used model profiles for dark matter halos.

In astronomy, stellar kinematics is the observational study or measurement of the kinematics or motions of stars through space.

Modified Newtonian dynamics (MOND) is a hypothesis that proposes a modification of Newton's law of universal gravitation to account for observed properties of galaxies. It is an alternative to the hypothesis of dark matter in terms of explaining why galaxies do not appear to obey the currently understood laws of physics.

Stacy McGaugh is an American astronomer and professor in the Department of Astronomy at Case Western Reserve University in Cleveland, Ohio. His fields of specialty include low surface brightness galaxies, galaxy formation and evolution, tests of dark matter and alternative hypotheses, and measurements of cosmological parameters.

<i>Reinventing Gravity</i> Book by John Moffat

Reinventing Gravity: A Scientist Goes Beyond Einstein is a science text by John W. Moffat, which explains his controversial theory of gravity.

The stellar halo of a galaxy refers to the component of its galactic halo containing stars. The halo extends far outside a galaxy's brightest regions and typically contains its oldest and most metal poor stars.

NGC 7013 Spiral or lenticular galaxy in the constellation Cygnus

NGC 7013 is a relatively nearby spiral or lenticular galaxy estimated to be around 37 to 41.4 million light-years away from Earth in the constellation of Cygnus. NGC 7013 was discovered by English astronomer William Herschel on July 17, 1784 and was also observed by his son, astronomer John Herschel on September 15, 1828.

NGC 720 Elliptical galaxy in the constellation Cetus

NGC 720 is an elliptical galaxy located in the constellation Cetus. It is located at a distance of circa 80 million light years from Earth, which, given its apparent dimensions, means that NGC 720 is about 110,000 light years across. It was discovered by William Herschel on October 3, 1785. The galaxy is included in the Herschel 400 Catalogue. It lies about three and a half degrees south and slightly east from zeta Ceti.

NGC 2974 Lenticular galaxy in the constellation Sextans

NGC 2974 is a lenticular galaxy located in the constellation Sextans. It is located at a distance of circa 90 million light years from Earth, which, given its apparent dimensions, means that NGC 2974 is about 90,000 light years across. It was discovered by William Herschel on January 6, 1785. NGC 2974 is located in the sky about 2 and a half degrees south-south east of Iota Hydrae and more than 6 degrees northeast of Alphard. A 10th magnitude star lies next to the galaxy, thus making it a challenging object at low magnifications. NGC 2974 is part of the Herschel 400 Catalogue.