Expansion of the universe - Quiz
A) As an optical illusion caused by the movement of the Milky Way B) As a purely random quantum fluctuation without a starting condition C) As resulting from an initial condition in which contents are flying apart D) As a contraction phase that has reversed into expansion
A) It causes the universe to immediately begin contracting B) It gradually slows the expansion over time C) It has no effect on the scale factor D) It accelerates the expansion indefinitely
A) They disappear over time B) They are countered by the speed of light C) Their density is too low D) Their gravitational constant is negative
A) The cosmological constant alone without dark energy B) Ultrarelativistic particles C) Nonrelativistic matter D) Dark energy
A) The pressure of dark energy B) The total mass of the universe C) The average separation between objects like galaxies D) The speed of light in a vacuum
A) It is smaller B) It was infinite C) It is larger D) It is exactly the same
A) It remains constant at 1 B) It is always zero C) It is larger D) It is smaller
A) 10.500 ± 0.100 billion years ago B) 13.787 ± 0.020 billion years ago C) 20.000 ± 0.050 billion years ago D) 5.250 ± 0.010 billion years ago
A) Negative one B) One C) Zero D) Infinity
A) The universe stopping expansion and beginning to contract B) The universe reaching zero temperature C) The universe maintaining a static size D) The universe expanding at an infinite speed
A) Kerr metric B) FLRW metric C) Minkowski metric D) Schwarzschild metric
A) Schrödinger equations B) Maxwell equations C) Navier-Stokes equations D) Friedmann equations
A) The geometric curvature of a static universe B) How quantum particles decay into dark matter C) The exact temperature of the cosmic microwave background D) How the contents of the universe influence its expansion rate
A) Cosmological constant B) Gravitational constant C) Energy density D) Speed of light
A) Gravitational potential B) Pressure of the cosmic fluid C) Scale factor derivative D) Energy density within the universe
A) Density B) Period C) Parallax D) Pressure
A) Speed of light B) Compression factor C) Cosmic constant D) Curvature parameter
A) Lambda baryon mass B) Cosmological constant C) Deceleration limit D) Wavelength of radiation
A) No effect on acceleration B) Deceleration of the expansion C) Immediate contraction of the universe D) Infinite acceleration
A) It neutralizes gravity completely B) It accelerates expansion C) It further decelerates expansion D) It stabilizes the scale factor
A) Zero pressure like nonrelativistic matter B) Positive pressure equal to ρc²/3 C) Sufficiently negative pressure with p < -ρc²/3 D) Infinite positive pressure
A) Photon gas density B) Nonrelativistic matter C) Ultrarelativistic particle gas D) The cosmological constant
A) It equals the speed of light squared B) It has extreme negative pressure C) It has extreme positive pressure D) It is essentially pressureless
A) Pressure is greater than ρc² B) Absolute pressure is much less than ρc² C) Pressure is exactly equal to ρc² D) Pressure is negative and exceeds ρc²
A) Neutron gas B) Dark matter gas C) Hydrogen gas D) Photon gas
A) p = -ρc²/3 B) p = ρc²/3 C) p = -ρc² D) p = 0
A) Yes, through direct particle accelerators B) Yes C) Only in laboratory settings D) No
A) From quantum mechanical calculations alone B) From direct laboratory synthesis C) From the laws of thermodynamics in a closed box D) From astronomical observations
A) ä = 1 B) ä = 0 C) ä < 0 D) ä > 0
A) Kepler's law B) Hubble's law C) Einstein's theory D) Newton's law
A) Composed of a single element B) Constantly changing C) The same everywhere D) The same in all directions
A) Logarithmically B) Chaotically C) Asymmetrically D) Uniformly
A) Exponential relationship B) Quadratic relationship C) Linear relationship D) Inverse relationship
A) Accelerations B) Time intervals C) Temperatures D) Positions
A) x0 B) v0 C) t0 D) H0
A) The Friedmann-Lemaître model B) The Lambda-CDM model C) The Big Bang metric D) The inflation model
A) Redshifting B) Late-time acceleration C) Dark energy acceleration D) Inflation
A) Alexander Friedmann B) Edwin Hubble C) Knut Lundmark D) Vesto Slipher
A) Walter Baade B) Adam Riess C) Knut Lundmark D) David Spergel
A) Knut Lundmark B) Georges Lemaître C) Vesto Slipher D) Edwin Hubble
A) Walter Baade B) David Spergel C) Wendy Freedman D) Edwin Hubble
A) Adam Riess's B) Knut Lundmark's C) Wendy Freedman's D) David Spergel's
A) 80±17 km⋅s-1⋅Mpc-1 B) 67±7 km⋅s-1⋅Mpc-1 C) 73±7 km⋅s-1⋅Mpc-1 D) 72±5 km⋅s-1⋅Mpc-1
A) Galaxy diameter measurements B) Visual-band light-curve shapes C) Cepheid variable calibrations D) Cosmic microwave background analysis
A) 80±17 km⋅s-1⋅Mpc-1 B) 72±5 km⋅s-1⋅Mpc-1 C) 73±7 km⋅s-1⋅Mpc-1 D) 67±7 km⋅s-1⋅Mpc-1
A) 80±17 km⋅s-1⋅Mpc-1 B) 67±7 km⋅s-1⋅Mpc-1 C) 73±7 km⋅s-1⋅Mpc-1 D) 50 to 90 km⋅s-1⋅Mpc-1
A) David Spergel's B) Wendy Freedman's C) Alexander Friedmann's D) Adam Riess's
A) Slipher Explorer B) Hubble Space Telescope C) Lemaître Space Observatory D) Wilkinson Microwave Anisotropy Probe satellite (WMAP)
A) 80±17 km⋅s-1⋅Mpc-1 B) 67±7 km⋅s-1⋅Mpc-1 C) 73±7 km⋅s-1⋅Mpc-1 D) 72±5 km⋅s-1⋅Mpc-1
A) Comoving coordinates B) Relativistic coordinates C) Spherical coordinates D) Cartesian coordinates
A) Three-dimensional spacetime B) Five-dimensional spacetime C) Four-dimensional spacetime D) Infinite-dimensional spacetime
A) Four-dimensional temporal surfaces B) One-dimensional linear curves C) Two-dimensional flat planes D) Three-dimensional spatial surfaces
A) Spheres B) Tori C) Cylinders D) Hyperboloids
A) Gravity B) Electromagnetism C) Dark matter density alone D) Thermal radiation
A) Irregularly curved B) Closed spheres C) Open hyperboloids D) Geometrically flat
A) 180 degrees B) 270 degrees C) 360 degrees D) 90 degrees
A) Infinite age B) Finite age C) Zero age D) Cyclical age
A) Event horizon B) Cosmic horizon C) Particle horizon D) Hubble horizon
A) Because stars burn out too quickly B) Due to excessive magnetic fields C) A cosmic event horizon induced by repulsive gravity D) Because light travels infinitely slowly
A) Hubble horizon B) Planck scale C) Event horizon D) Particle horizon
A) Thermal expansion B) Gravitational lensing C) The Doppler effect D) Photon decay
A) They dilute B) They multiply C) They concentrate D) They annihilate
A) a B) p C) rho D) w
A) One-third B) Zero C) Negative one D) Negative three
A) Around 10−32 seconds B) Around 1026 seconds C) At the very end of the universe D) Around 1 second
A) Ultrarelativistic particles B) Neutrino decoupling C) The inflaton D) Magnetic monopoles
A) A positive-energy false vacuum state B) A fluctuating thermal vacuum state C) A zero-energy stable vacuum state D) A negative-energy true vacuum state
A) Inflaton fields B) Standard Model particles C) Magnetic monopoles D) Cosmic scale factors
A) Neutrino decoupling B) Quantum fluctuations C) Thermal radiation D) Magnetic monopoles
A) About 1060 B) About 1032 C) About 1 D) About 1026
A) Radiation B) Inflation C) The horizon D) Quantum fluctuations
A) About 1026 seconds B) About 10−32 seconds C) About 1 second D) About e60 seconds
A) Nonrelativistic matter B) Cosmic microwave background C) Dark energy D) Neutron stars
A) Matter-dominated epoch B) Inflationary epoch C) Dark energy epoch D) Radiation era
A) Through the redshift B) By measuring gravitational lensing angles C) Using its apparent brightness D) Through time-delay cosmography
A) Type Ia supernovae B) Lensed quasars C) Neutron stars D) Cepheid variable stars
A) Time-delay cosmography B) Cepheid variable photometry C) CMB fluctuation sizing D) Redshift drift analysis
A) TDCOSMO cluster B) H0LiCOW cluster C) Planck foreground cluster D) MACS J0138-2155
A) MACS J0138-2155 B) GW170817 C) SN Requiem D) SN Refsdal
A) CMB fluctuation sizes B) Gravitational lensing time delays C) Standard candle brightness D) Redshift drift
A) Square Kilometre Array or Extremely Large Telescope B) H0LiCOW and TDCOSMO space probes C) Planck collaboration satellites D) Cepheid variable telescopes from Hubble's era
A) An infinite Euclidean universe B) A static spacetime C) A universal center D) A preferred rest frame
A) Only in flat spacetimes B) Yes C) No D) Only on small scales
A) Quantum mechanics B) General relativity C) Electromagnetism D) Special relativity
A) Andrew R. Liddle B) Charles H. Lineweaver C) Arthur Eddington D) Delo E. Mook
A) Cambridge University Press B) Scientific American C) Princeton University Press D) Press Syndicate of the University of Cambridge
A) March 2005 B) March 2000 C) March 1931 D) March 1991
A) Thomas Vargish B) Andrew R. Liddle C) Tamara M. Davis D) David H. Lyth |
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