Big Rip

The Big Rip is a cosmological hypothesis about the ultimate fate of the universe, in which the matter of the universe, from stars and galaxies to atoms and subatomic particles, and even spacetime itself, is progressively torn apart by the expansion of the universe at a certain time in the future. According to the hypothesis, first published in 2003, the scale factor of the universe and with it all distances in the universe will become infinite at a finite time in the future. The possibility of sudden singularities and crunch or rip singularities at late times occur only for hypothetical matter with implausible physical properties.^[1]

Definition and overview

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also see {{Human timeline}} and {{Life timeline}}

The hypothesis relies crucially on the type of dark energy in the universe. The key value is the equation of state parameter $w$, the ratio between the dark energy pressure and its energy density. If $w$ < −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

$t_{rip}-t_{0}\approx {\frac {2}{3|1+w|H_{0}{\sqrt {1-\Omega _{m}}}}}$

where $w$ is defined above, H₀ is Hubble's constant and Ω_m is the present value of the density of all the matter in the universe.

In their paper, the authors consider an example with $w$ = −1.5, H₀ = 70 km/s/Mpc and Ω_m = 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 $w$ to be very close to −1 in our universe, which makes $w$ the dominating term in the equation. The closer that $w$ is to −1, the closer the denominator is to zero and the further the Big Rip is in the future. If $w$ were exactly equal to −1, the Big Rip could not happen, regardless of the values of H₀ or Ω_m.

What will happen

In their scenario for $w$ = −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 the Solar System 22 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. At the end of the universe, spacetime itself will be ripped apart.^[2]

Experimental data

According to the latest cosmological data available, the uncertainties are still too large to discriminate among the three cases $w$ < −1, $w$ = −1, and $w$ > −1.^[3][4]

See also

• Accelerating universe
• Big Bounce
• Big Crunch
• Big Freeze
• Cyclic Model
• Dark energy
• Entropy (arrow of time)
• Future of an expanding universe
• Heat death of the universe
• List of astronomical topics
• Phantom energy
• Timeline of the far future
• Ultimate fate of the universe

References

1. Ellis, George F. R., R. Maartens, and M. A. H. MacCallum. Relativistic Cosmology. Cambridge: Cambridge UP, 2012. 146-47. Print.
2. Caldwell, Robert R.; Kamionkowski, Marc; 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.
3. http://wmap.gsfc.nasa.gov/news/
4. 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.

External links

• New York Times article