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