| 1. | At large radii, radial velocity dispersion exhibit strange behavior.
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| 2. | The velocity dispersion of stars at the center of the cluster is.
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| 3. | Here, the velocity dispersion is much smaller.
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| 4. | Where ? V 2 is the velocity dispersion and G is the gravitational constant.
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| 5. | Typical velocity dispersion of galaxies within the Local Sheet is only in the radial direction.
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| 6. | When a wave propagates through subsurface materials both energy dissipation and velocity dispersion takes place.
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| 7. | Modal dispersion during propagation in the waveguide then provides group velocity dispersion to the signal.
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| 8. | Near the core, the stars have a velocity dispersion of 136 ?20 km / s.
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| 9. | The result of group velocity dispersion, whether negative or positive, is ultimately temporal spreading of the pulse.
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| 10. | The bulge component is similar to elliptical galaxies in that it is pressure supported by a central velocity dispersion.
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