Results 231 to 240 of about 51,405 (265)

Extreme energy in a relaxed galaxy group indicates the bursty nature of AGN feedback

Eckert D, Gastaldello F, Lovisari L, McGee S, Pasini T, Brienza M, Kolokythas K, O'Sullivan E, Simionescu A, Sun M, Bourne M, Chen Y, Cui W, Ettori S, Finoguenov A, Gozaliasl G, Kale R, Mernier F, Oppenheimer B, Schellenberger G, Seppi R, Tempel E.   +21 more
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A binary merger product as the direct progenitor of a Type II-P supernova

Niu* Z, Sun* N, Zapartas* E, Souropanis D, Cui Y, Maund JR, Andrews JJ, Briel MM, Fraser M, Gossage S, Kruckow MU, Liotine C, Liu Z, Srivas PM, Teng E, Wang X, Yang Y, Liu J.   +17 more
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Feedback mechanisms stopping the star formation in a pair of massive galaxies in the early Universe

Pérez-González P, D'Eugenio F, Pino BRD, Perna M, Uebler H, Maiolino R, Arribas S, Lamperti I, Bunker A, Carniani S, Charlot S, Willott C, Böker T, Parlanti E, Scholtz J, Venturi G, Barro G, Costantin L, Navarro IM, Dunlop J, Magee D, Cresci G.   +21 more
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The Rotation Curve of our Galaxy

Applied Mechanics and Materials, 2014
The rotation curve of our Galaxy is derived from a large sample of objects with known radial velocities and distances. We collect data as completely as possible, especially the data with accurately measured trigonometric parallaxes. These observations are used to construct a highly accurate rotation curve of the Galaxy.
Wei Bin Shi, Gui Ping Ruan
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Rotation curves in neutrino-dominated galaxies

Chinese Astronomy and Astrophysics, 1983
Abstract A massive neutrino halo will exert important effects on the motion of the galactic stars inside. In this paper, we give a fully relativistic treatment of the galactic velocity curve in the presence of a massive halo. The results are different from the classical Kepler motion, and provides a possible means of verifying the existence of ...
Shou-Ping Xiang, Jian-gong Gao, Chong-ming Xu   +2 more
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CDM confronts galaxy rotation curves

2010
What do rotation curves require of dark matter? The extended rotation curves of spiral galaxies are asymptotically flat. This is the essential result of three decades of 21-cm line observations carried out with radio telescopes – single-dish as well as interferometers. Every astronomer and physicist is familiar with this result and its interpretation
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Multidimensional gravitational interaction: Galaxy rotation curves

Journal of Experimental and Theoretical Physics, 2014
A description of gravitational interaction based on the assumption about a change of the spacetime dimension in anisotropic regions of galaxies is proposed. Analysis of the rotation curves for 60 galaxies has shown a good correspondence to the description at gravitational constants of (2.7 ± 0.4) × 10−31 m2 kg−1 s−2 and (3.0 ± 1.0) × 10−53 m kg−1 s−2 ...
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Rotation Curves of Giant LSB Galaxies

Bulletin of the American Astronomical Society, 1996
We present optical and H I rotation curves of a sample of giant, low surface brightness (LSB) galaxies including the prototype, Malin 1. The rotation curves of these diffuse systems are expected to more faithfully reflect the structure of their dark matter halos due to the reduced contribution of the disk to the overall gravitational potential. Indeed,
Pickering, T. E., Impey, C. D., Navarro, J. F., van Gorkom, J., Bothun, G. D.   +4 more
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The Dynamics of Galaxy Rotational Curves

Space 2006, 2006
During the 1980’s, the first astronomical evidence was obtained that appeared to indicate spiral galaxies, (see Figure 1) do not rotate according to Newton’s’ Second Law of Motion: F=MA. The observations suggest that the outer stars in galaxies seem to rotate too fast for the amount of matter we see in the galaxy.
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The Rotation Curve of the Galaxy

1983
The determination of the rotation curve of the Galaxy, θ(R), where θ is the circular velocity at galactocentric distance R, involves the synthesis of a large body of complementary (and sometimes contradictory) data. The synthesis has to be guided to some extent by theoretical considerations such as studying the distribution of mass in the Galaxy, i.e ...
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