Dark energy and the fate of the universe

Jul 26, 2012
Light from distant galaxies is stretched by foreground matter in this Hubble image. Similar distortions - called weak lensing - are less obvious, but their widespread nature can help reveal the nature of dark energy. Credit: NASA, Andrew Fruchter and the ERO Team [Sylvia Baggett (STScI), Richard Hook (ST-ECF), Zoltan Levay (STScI)] (STScI)

New research on dark energy is helping scientists understand the potential fate of the Universe.

makes up about 70 percent of the current content of the Universe and thus holds the ultimate fate of our Universe. Several possible scenarios are possible depending on the properties of dark energy; one is that the Universe will end in a so-called big rip. This interesting topic was recently explored by five researchers from the University of Science and Technology of China, the Institute of Theoretical Physics at the , Northeastern University, and Peking University. Their work, entitled "Dark energy and fate of the Universe", was published in Sci China-Phys Mech Astron. 2012, Vol. 55 No. 7.

For millennia, human beings have been pondering two ultimate questions: "Where do we come from?" and "Where are we going?" Over that time, these questions have spurred theological and philosophical debate. Thanks to the rapid development of modern cosmology in the past three decades, scientists nowadays have obtained some important clues to answer these questions. The standard "inflation + hot " framework has been developed to explain the origin of the Universe. However, to forecast the destiny of the Universe, researchers have realized that the nature of dark energy is key.

In the absence of a consensus on what dark energy is, a phenomenological description of the equation-of-state parameter w—the ratio of pressure and density of dark energy—provides an important means for investigating dark energy dynamics. Properties of dark energy will decide the ultimate fate of the Universe. In particular, if w<-1 at some time in the future, dark energy density will grow to infinity in finite time, and its gravitational repulsion will tear apart all the objects in the Universe. This "big rip" (or "cosmic doomsday") scenario is the major focus of the paper. "We want to infer from the current data what the worst fate would be for the Universe", said the authors.

To foresee that fate, it is important to choose an appropriate parameterization that covers the overall expansion history of the Universe. The most popular Chevallier-Polarski-Linder (CPL) parameterization, in fact, is not suitable in predicting the future evolution of the Universe because in this form w will diverge when the redshift parameter approaches -1. Thus, the authors invoke a divergence-free parameterization, called the Ma-Zhang (MZ) parameterization, to predict the evolution of the Universe.

One of the more intriguing questions is: "If a doomsday exists, how far are we from it?" After constraining the MZ parameter space via a Markov Chain Monte Carlo method, the authors found that by using the current observational data tBR – t0 = 103.5 Gyr for the best-fit result, and tBR – t0 = 16.7 Gyr at the 95.4% confidence level (CL) lower limit. Here tBR denotes the time of the big rip, and t0 denotes the present day. "In other words, at worst (95.4% CL), the time remaining before the Universe ends in a big rip is 16.7 Gyr", said the authors.

Thus the constrained parameter space indicates that it is very likely that in the future w<-1. If so, one may ask another interesting question: "How about the destinies of the gravitationally bound objects in the , such as galaxies and stars?" In fact, if w indeed ever becomes less than -1, dark energy's gravitational repulsion will continuously increase until it overcomes all forces holding objects together and all objects will be torn apart. No object would escape this fate, but obviously systems more tightly bound would exist for longer. Using the MZ parameterization, the authors speculated on a series of possible consequences before the cosmic doomsday. For example, for the worst situation, namely the 95.4% CL lower limit, the Milky Way will be torn apart 32.9 Myr before the big rip; two months before doomsday, the Earth will be ripped from the Sun; five days before the doomsday, the moon will be ripped from the Earth; the Sun will be destroyed 28 min before the end of time; and 16 min before the end, the Earth will explode.

However, from what we already know of the dynamical properties of dark energy, one thing is all very clear, we still have a very long future ahead.

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ritwik
1 / 5 (5) Jul 27, 2012
the present model of universe is not true

if DE&DM makes up ~96% of the universe and matter only paltry 4% how do physicists assume homogeneity and isotropy ?
matter portion might be just clumped on one spot surrounded by infinite emptiness

secondly inflation & metric expansion of space has no solid proof nor makes sense to unadulterated mind

cosmic bg radiation might be just the aggregate of radiation of all stars

to unravel more mysteries all the present brain dead haughty physicists have to pass out and new people have to come upwithout all the present prejudices
Fleetfoot
5 / 5 (5) Jul 27, 2012
if DE&DM makes up ~96% of the universe and matter only paltry 4% how do physicists assume homogeneity and isotropy?


They don't assume it, the fact that it is homogenous at large scales is measured from surveys.

matter portion might be just clumped on one spot surrounded by infinite emptiness


Such a structure would be unstable, the universe would have collapsed.

secondly inflation & metric expansion of space has no solid proof


Expansion is directly observed as the Hubble Law. Inflation is still a working hypothesis.

cosmic bg radiation might be just the aggregate of radiation of all stars


The sum of radiation would have a flat spectrum, what is observed is an almost perfect black-body curve, so accurate it cannot be matched even by a single star never mind an aggregate.

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