Big rip

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The Big Rip (English for "The Great Ripping", occasionally also called "End Bang") is in cosmology next to the Big Crunch ("The great collapse") and the Big Freeze ("The great freezing", eternal expansion [also referred to as Big Chill or Big Whimper ]) a third hypothetical end of the universe . The rate of expansion, driven by a growing phantom energy density, increases faster and faster and finally diverges in the singular event called Big Rip . Phantom energy is a form of dark energy . The universe would be torn apart from the largest to the smallest structures. First it hits galaxy clusters, then galaxies, the solar system, the earth, atoms, etc.

Models

According to the 2003 model by Robert Caldwell ( Dartmouth College , New Hampshire ), Marc Kamionkowski and Nevin N. Weinberg, a continuous expansion of the universe in itself might not last forever, but could become unstable and degenerate into a big rip .

The authors of this model received the following formula for the time from the present point in time to the point in time of the explosive divergence: ${\displaystyle t_{0}}$ ${\displaystyle t_{\rm {rip}}}$

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

It is

• ${\displaystyle w}$a measure of the strength of expansion due to dark energy; an example is included in the work . ${\displaystyle w=-1{,}5}$
• ${\displaystyle H_{0}}$the Hubble constant
• ${\displaystyle \Omega _{m}}$the reduced value for the current density of matter in the universe.

Although the physical nature of dark energy is still unknown, it can be thought of as a kind of ideal gas that has an equation of state with the so-called -parameter. Here denotes the pressure, the energy density of the dark energy, the density and the speed of light. To force an accelerated expansion of the universe, the parameter would have to be smaller than . The cosmological constant introduced by Einstein leads to a value of . With the underlying value of , the universe would degenerate in about 22 billion years. ${\displaystyle p=w\rho c^{2}}$ ${\displaystyle w}$ ${\displaystyle p}$ ${\displaystyle \rho c^{2}}$ ${\displaystyle \rho }$ ${\displaystyle c}$ ${\displaystyle w}$ ${\displaystyle -1/3}$ ${\displaystyle w=-1}$ ${\displaystyle w=-1{,}5}$

Assuming a constant parameter, Riess et al. 2009 from the measurement data of the Hubble space telescope a w-parameter by and Komatsu et al. 2011 with the help of the WMAP measurement data a w-parameter of . If the assumption of a constant -parameter is dropped, the observations still show that apparently little changes over time. Assumptions that such disruptive events could occur locally are improbable because previous observations show that the universe is homogeneous on large scales. ${\displaystyle w}$ ${\displaystyle w=-1{,}12\pm 0{,}12}$ ${\displaystyle w=-1{,}10\pm 0{,}14}$ ${\displaystyle w}$ ${\displaystyle w}$

literature

• Robert R. Caldwell, Marc Kamionkowski, Nevin N. Weinberg Phantom Energy and Cosmic Doomsday , Phys. Rev. Lett., 91, 2003, 071301, Arxiv

Web links

• End of the universe scenario at Astro News
• Big Rip, Big Crunch and Big Whimper as the possible end of the universe
• Astronomy Lexicon: Big Rip

credentials

1. ^ Andreas Müller: Big Rip ( Memento from October 12, 2014 in the Internet Archive ). AstroWissen, 2007.
2. ↑ From the Big Bang to Modern Humans: The Development of the World in 10 Steps ; Peter Ulmschneider; Google Books; accessed in September 2014