Dark matter halo - Quiz
A) A byproduct of black hole radiation B) A type of visible galaxy C) A theoretical error in general relativity D) A basic unit of cosmological structure
A) It is actively being created by cosmic expansion B) It expands faster than the universe C) It has decoupled from cosmic expansion D) It is unaffected by the expansion of space
A) Virialized clumps of dark matter bound by gravity B) Smaller galaxies that orbit the Milky Way C) Gaseous clouds within the galactic disc D) Regions of space devoid of any matter
A) They may contain galaxies B) They replace galaxies entirely C) They only exist outside of galaxies D) They are created by galaxy collisions
A) Only to the edge of the visible galactic disc B) Well beyond the edge of the visible galaxy C) It is confined within the visible stars D) Only to the center of the galactic bulge
A) No B) Yes, using particle detectors in space C) Yes, using optical telescopes D) Yes, using infrared scanners
A) By measuring the heat emitted by the halo B) Through effects on star and gas motion and gravitational lensing C) Through direct visual observation D) By counting the number of galaxies in a cluster
A) Solar wind particles B) Cold dark matter (CDM) C) Dark energy plasma D) Galactic magnetic resonance
A) The rotation slows down significantly at the edges B) The presence of dark matter C) The absence of mass at large distances D) The galaxy is shrinking toward the center
A) It would increase B) It would decrease C) It would cease entirely D) It would remain constant
A) X-ray bursts from the galactic core B) Cosmic microwave background radiation C) 21 cm Hydrogen line D) Ultraviolet light emissions
A) It fluctuates randomly B) It drops off sharply C) It flattens out D) It increases exponentially
A) Albert Einstein B) Edwin Hubble C) Ken Freeman D) Isaac Newton
A) NGC 300 and M33 B) Centaurus A and Sombrero C) The Milky Way and Andromeda D) The Triangulum and the Magellanic Clouds
A) General relativity is incomplete B) Intergalactic dust interference C) The presence of black holes at every star system D) Excessive solar radiation
A) It lacked sufficient mass. B) It was interacting too strongly with dark energy. C) It was moving too slowly to form structures. D) Its temperature was too high.
A) Radiative pressure modeling B) Spherical collapse C) Linear expansion D) Baryonic oscillation
A) Ellipsoidal B) Flat disk C) Irregular filamentary D) Perfectly spherical
A) The central density is infinite at the core radius. B) The core radius is not defined for large distances. C) It does not provide a good fit to rotation curve data. D) The enclosed mass fails to converge as the radius tends to infinity.
A) NFW profile B) Spherical-collapse profile C) Pseudo-isothermal profile D) Einasto profile
A) Finite central density B) Scale radius C) Characteristic density D) Critical density
A) Central density B) Characteristic density C) Scale radius D) Critical density
A) Mergers associated with hierarchical formation. B) The critical density of the universe is too low. C) The scale radius is always zero. D) The mass converges too quickly.
A) The radius where the density is zero. B) The scale radius rs. C) The core radius rc. D) An overdensity 200 times greater than the critical density.
A) Yes B) Only at the center. C) Only at the scale radius. D) No, it diverges to infinity.
A) Perfectly spherical B) Aspherical C) Flat disks D) Cubical
A) Dark energy repulsion B) Surface friction C) Electromagnetic radiation D) Strong tidal forces
A) Uniform distribution B) Exponential distribution C) Log-normal distribution D) Normal distribution
A) 0.100 B) 0.035 C) 0.001 D) 0.050
A) About 50% B) About 95% C) About 75% D) About 25%
A) 6×1011 M☉ B) 9×1010 M☉ C) 3×1012 M☉ D) 1×109 M☉
A) 0.88 M☉ pc-3 B) 0.0088 M☉ pc-3 C) 0.00088 M☉ pc-3 D) 0.088 M☉ pc-3 |
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