The Big Rip is a cosmological hypothesis first published in 2003, about the ultimate fate of the universe, in which the matter of the universe, from stars and galaxies to atoms and subatomic particles, is progressively torn apart by the expansion of the universe at a certain time in the future. According to the hypothesis, the scale factor of the universe and with it all distances in the universe will become infinite at a finite time in the future. It is important to note that the possibility of sudden singularities and crunch or rip singularities at late times occur only for hypothetical matter with implausible physical properties.
Definition and overview
The hypothesis relies crucially on the type of dark energy in the universe. The key value is the equation of state parameter , the ratio between the dark energy pressure and its energy density. At < −1, the universe will eventually be pulled apart. Such energy is called phantom energy, an extreme form of quintessence.
A universe dominated by phantom energy expands at an ever-increasing rate. However, this implies that the size of the observable universe is continually shrinking; the distance to the edge of the observable universe which is moving away at the speed of light from any point moves ever closer. When the size of the observable universe becomes smaller than any particular structure, no interaction by any of the fundamental forces (gravitational, electromagnetic, weak, or strong) can occur between the most remote parts of the structure. When these interactions become impossible, the structure is "ripped apart". The model implies that after a finite time there will be a final singularity, called the "Big Rip", in which all distances diverge to infinite values.
The authors of this hypothesis, led by Robert Caldwell of Dartmouth College, calculate the time from the present to the end of the universe as we know it for this form of energy to be
where is defined above, H0 is Hubble's constant and Ωm is the present value of the density of all the matter in the universe.
In their paper, the authors consider an example with = −1.5, H0 = 70 km/s/Mpc and Ωm = 0.3, in which case the end of the universe is approximately 22 billion years from the present. This is not considered a prediction, but a hypothetical example. The authors note that evidence indicates to be very close to −1 in our universe, which makes the dominating term in the equation. The closer that the quantity (1 + ) is to zero, the closer the denominator is to zero and the further the Big Rip is in the future. If were exactly equal to −1, the Big Rip could not happen, regardless of the values of H0 or Ωm.
In their scenario for = −1.5, the galaxies would first be separated from each other. About 60 million years before the end, gravity would be too weak to hold the Milky Way and other individual galaxies together. Approximately three months before the end, the solar system (or systems similar to our own at this time, as the fate of our own solar system 7.5 billion years in the future is questionable) would be gravitationally unbound. In the last minutes, stars and planets would be torn apart, and an instant before the end, atoms would be destroyed.
- List of astronomical topics
- Accelerating universe
- Heat-death of the Universe
- Big Crunch
- Big Bounce
- Big Freeze
- Entropy (arrow of time)
- Ultimate fate of the Universe
- Phantom energy
- Cyclic Model
- Dark energy
- Ellis, George F. R., R. Maartens, and M. A. H. MacCallum. Relativistic Cosmology. Cambridge: Cambridge UP, 2012. 146-47. Print.
- Caldwell, Robert R.; Kamionkowski, Marc and Weinberg, Nevin N. (2003). "Phantom Energy and Cosmic Doomsday". Physical Review Letters 91 (7): 071301. arXiv:astro-ph/0302506. Bibcode:2003PhRvL..91g1301C. doi:10.1103/PhysRevLett.91.071301. PMID 12935004.
- Allen, S. W.; Rapetti, D. A.; Schmidt, R. W.; Ebeling, H.; Morris, R. G.; Fabian, A. C. (2008). "Improved constraints on dark energy from Chandra X-ray observations of the largest relaxed galaxy clusters". Monthly Notices of the Royal Astronomical Society 383 (3): 879. arXiv:0706.0033. Bibcode:2008MNRAS.383..879A. doi:10.1111/j.1365-2966.2007.12610.x.