Hubble volume

Visualization of the three-dimensional large-scale structure of the universe in the Hubble volume. The scale is such that the fine grains of light represent collections of large numbers of superclusters. The Virgo Supercluster - home of our own galaxy - is at the center of our Hubble volume, but is too small to be seen in the image.

In cosmology, a Hubble volume, or Hubble sphere, is a spherical region of the Universe surrounding an observer beyond which objects recede from that observer at a rate greater than the speed of light due to the expansion of the Universe.[1] The Hubble volume is approximately 1031 cubic light years.

The proper radius of a Hubble sphere (known as the Hubble radius or the Hubble length) is c/H_0, where c is the speed of light and H_0 is the Hubble constant. The surface of a Hubble sphere is called the microphysical horizon,[2] the Hubble surface, or the Hubble limit.

More generally, the term "Hubble volume" can be applied to any region of space with a volume of order (c/H_0)^3. However, the term is also frequently (but mistakenly) used as a synonym for the observable universe; the latter is larger than the Hubble volume.[3][4]

Relationship to age of the universe

The Hubble length c/H_0 is 14 billion light years in the standard cosmological model, somewhat larger than c times the age of the universe, 13.8 billion years.

Hubble limit as an event horizon

Objects at the Hubble limit have an average proper speed of c relative to an observer on the Earth so that, in a universe with constant Hubble parameter, light emitted at the present time by objects outside the Hubble limit would never be seen by an observer on Earth. That is, Hubble limit would coincide with a cosmological event horizon (a boundary separating events visible at some time and those that are never visible[5]). See Hubble horizon for more details.

However, the Hubble parameter is not constant in various cosmological models[3] so that the Hubble limit does not, in general, coincide with a cosmological event horizon. For example in a decelerating Friedmann universe the Hubble sphere expands faster than the Universe and its boundary overtakes light emitted by receding galaxies so that light emitted at earlier times by objects outside the Hubble sphere still may eventually arrive inside the sphere and be seen by us.[3] Conversely, in an accelerating universe, the Hubble sphere expands more slowly than the Universe, and bodies move out of the Hubble sphere.[1]

Observations indicate that the universe is accelerating,[6] so that some objects that we can currently exchange signals with will one day cross our Hubble limit.

See also

References

  1. 1 2 Edward Robert Harrison (2003). Masks of the Universe. Cambridge University Press. p. 206. ISBN 0-521-77351-2.
  2. ↑ N. Carlevaro & G. Montani (2009). "Study of the Quasi-isotropic Solution near the Cosmological Singularity in Presence of Bulk-Viscosity". arXiv:0711.1952.
  3. 1 2 3 For a discussion of why objects that are outside the Earth's Hubble sphere can be seen from Earth, see TM Davis & CH Linewater (2003). "Expanding Confusion: common misconceptions of cosmological horizons and the superluminal expansion of the universe". arXiv:astro-ph/0310808.
  4. ↑ For an example of mistaken usage, see Max Tegmark (2004). "Parallel Universes". In Barrow, J. D.; Davies, J. D.; Harper, C. L. Science and Ultimate Reality: From Quantum to Cosmos. Cambridge University Press. pp. 459ff. ISBN 0-521-83113-X.
  5. ↑ Edward Robert Harrison (2000). Masks of the Universe. Cambridge University Press. p. 439. ISBN 0-521-66148-X.
  6. ↑ John L Tonry; et al. (2003). "Cosmological Results from High-z Supernovae". Astrophys J 594: 1. arXiv:astro-ph/0305008. Bibcode:2003ApJ...594....1T. doi:10.1086/376865.

External links

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