scholarly journals Law of Physics 20th-Century Scientists Overlooked (Part 5): Centrifugal Effect Negation

2021 ◽  
Vol 13 (2) ◽  
pp. 13
Author(s):  
Conrad Ranzan
Keyword(s):  
Dark Matter ◽  
Neutron Star ◽  
Structural Integrity ◽  
Spiral Galaxies ◽  
Extreme Condition ◽  
Theoretical Limit ◽  
Centrifugal Effect ◽  
Profound Implication ◽  
Universal Space ◽  
Fundamental Law

Explored is another application of the phenomenally successful DSSU’s aether theory of gravity. It is explained how rotational motion with respect to the universal space medium (aether) determines the centrifugal effect. The article details the conditions involved in the attenuation of the Effect; and the extreme condition under which complete negation occurs. Included is a description of how a totally collapsed star —called a Terminal neutron star— is unable to manifest any centrifugal effects; and how, consequently, it can have no theoretical limit on its rate of rotation. Revealed is the fundamental law governing circular motion. This long-overlooked principle of physics leads to a startling and profound implication: Spiral galaxies are able to maintain their structural integrity without the need for so-called dark matter.

Dark Matter in Spiral Galaxies

1983 ◽  
Vol 248 (6) ◽  
pp. 96-108 ◽  
Author(s):  
Vera C. Rubin
Keyword(s):  
Dark Matter ◽  
Spiral Galaxies

scholarly journals The relation between the gas, dust and total mass in edge-on spiral galaxies

2014 ◽  
Vol 10 (S309) ◽  
pp. 297-297
Author(s):  
Flor Allaert
Keyword(s):  
Dark Matter ◽  
Total Mass ◽  
Spiral Galaxies ◽  
3D Structure ◽  
Early Type ◽  
Interstellar Gas ◽  
Data Set ◽  
Unique Role ◽  
Radio Data ◽  
Multi Wavelength

AbstractEach component of a galaxy plays its own unique role in regulating the galaxy's evolution. In order to understand how galaxies form and evolve, it is therefore crucial to study the distribution and properties of each of the various components, and the links between them, both radially and vertically. The latter is only possible in edge-on systems. We present the HEROES project, which aims to investigate the 3D structure of the interstellar gas, dust, stars and dark matter in a sample of 7 massive early-type spiral galaxies based on a multi-wavelength data set including optical, NIR, FIR and radio data.

scholarly journals Rotation of Galaxy Dark Matter Halos

2006 ◽  
Vol 2 (S235) ◽  
pp. 104-104
Author(s):  
Stéphane Herbert-Fort ◽  
Dennis Zaritsky ◽  
Yeun Jin Kim ◽  
Jeremy Bailin ◽  
James E. Taylor
Keyword(s):  
Dark Matter ◽  
Angular Momentum ◽  
Numerical Simulations ◽  
Galaxy Formation ◽  
Spiral Galaxy ◽  
Observational Studies ◽  
Spiral Galaxies ◽  
Satellite System ◽  
Dark Matter Halos ◽  
The Mean

AbstractThe degree to which outer dark matter halos of spiral galaxies rotate with the disk is sensitive to their accretion history and may be probed with associated satellite galaxies. We use the Steward Observatory Bok telescope to measure the sense of rotation of nearby isolated spirals and combine these data with those of their associated satellites (drawn from SDSS) to directly test predictions from numerical simulations. We aim to constrain models of galaxy formation by measuring the projected component of the halo angular momentum that is aligned with that of spiral galaxy disks, Jz. We find the mean bulk rotation of the ensemble satellite system to be co-rotating with the disk with a velocity of 22 ± 13 km/s, in general agreement with previous observational studies and suggesting that galaxy disks could be formed by halo baryons collapsing by a factor of ≈10. We also find a prograde satellite fraction of 51% and Jz, of the satellite system to be positively correlated with the disk, albeit at low significance (2655 ± 2232 kpc km/s).

scholarly journals Detecting dark matter with neutron star spectroscopy

2019 ◽  
Vol 2019 (09) ◽  
pp. 051-051 ◽  
Author(s):  
Daniel A. Camargo ◽  
Farinaldo S. Queiroz ◽  
Riccardo Sturani
Keyword(s):  
Dark Matter ◽  
Neutron Star

scholarly journals The Dark Matter Content of Barred Spiral Galaxies

2004 ◽  
Vol 220 ◽  
pp. 277-278
Author(s):  
Glen Petitpas ◽  
Mousumi Das ◽  
Peter Teuben ◽  
Stuart Vogel
Keyword(s):  
Dark Matter ◽  
Spiral Galaxies ◽  
Velocity Fields ◽  
Matter Content ◽  
Two Dimensional ◽  
Disk Model ◽  
Barred Galaxies ◽  
Preliminary Results ◽  
Nearby Galaxies ◽  
Barred Spiral Galaxies

Two-dimensional velocity fields have been used to determine the dark matter properties of a sample of barred galaxies taken from the BIMA Survey of Nearby Galaxies (SONG). Preliminary results indicate that the maximal disk model is not appropriate in several galaxies in our sample, but higher resolution results will be needed to confirm this.

DARK MATTER AND DYNAMICS IN HERCULES CLUSTER

1994 ◽  
Vol 03 (supp01) ◽  
pp. 93-100
Author(s):  
Christina M. Bird ◽  
John M. Dickey ◽  
E.E. Salpeter
Keyword(s):  
Dark Matter ◽  
Total Mass ◽  
Virial Theorem ◽  
Spiral Galaxies ◽  
Large Body ◽  
Statistical Test ◽  
Mass Determination ◽  
Dynamical Mass ◽  
Cluster Galaxies ◽  
Abell Cluster

We present new 21-cm observations of faint (15.7<mpg<16.5) spiral galaxies in the Abell cluster 2151. These results, when combined with the large body of velocities available in the literature for Hercules, permit us to study the dynamics throughout the cluster core, out to a projected radius of 1.8h−1 Mpc. We calculate the global dynamical mass of Hercules using 3 different but related methods: two versions of the virial theorem and the projected mass estimator. These masses lie in the range 3–6×1014 M⊙. We investigate the importance of subclustering in A2151 using the statistical test of Dressler and Shectman1 and the effects of the detected substructure on the dynamical mass determination. The clumpy distribution of galaxies is interpreted as a sign that the galaxies in the cluster have not reached dynamical equilibrium in the gravitational potential, which means that dynamical mass estimates are prone to significant errors. In spite of this uncertainty, we estimate that the virial theorem errors due to the presence of substructure are not larger than 30% in A2151. Finally, we use the 21-cm linewidths to estimate the minimum total mass in the cluster which is contained within the HI radii of the cluster galaxies is about 3×1014 M⊙. This number may be compared with the dynamical mass and used to separate the contribution of dark matter inside and outside the HI envelopes of galaxies, and the fraction of DM which cannot be associated with individual galaxies, about 90–95%.

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