![]() Previous studies for the scaling between halo central density and core radius have different slopes for different model fits. The R-square value (the percentage of data variation that can be explained by model) of the fit is 0.82 with root-mean-square scatter of all data around 0.3dex. These include vats of liquid xenon stored miles underground, and telescopes looking for dark matter particles decaying into things we can see and measure, like gamma rays. The black dash line shows the least-square fit to data from all 248 galaxies with the best slope of − 1.36 \(\pm \,0.05\) that is very close to − 4/3. 7) is also plotted for comparison with coefficients \(\beta _r = 1.26\) and \(\alpha _r = 5.28\) obtained from these data. Strong correlation exists between core density and scale radius with a Pearson correlation coefficient of − 0.91. Most modern-day astronomers think dark matter likely consists of subatomic particles with properties that are rather different from more familiar protons and neutrons. The kinetic energy is cascaded in dark matter from small to large scales involves a constant rate \(\varepsilon _u\) ( \(\approx -\,4.6\times 10^\) as suggested by SPS models.įor pseudo-isothermal (pISO) and NFW density, we haveįigure 6 presents the variation of typical density \(\rho _s\) with scale \(r_s\) obtained from three different sources of galaxy rotation curves. Dark energy, in contrast to both forms of matter, is relatively uniform in time and space and is gravitationally repulsive, not attractive, within the volume it occupies. The remaining portion of the universe consists of ordinary matter and dark matter. A cascade theory for dark matter is proposed to provide extra insights, similar to the cascade phenomenon in hydrodynamic turbulence. dark energy, repulsive force that is the dominant component (69.4 percent) of the universe. ![]() Smalls scale challenges suggest some missing pieces in our current understanding of dark matter.
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