cosmological constant

Why does the cosmological constant have the value that it has?

The cosmological constant is a very old idea, going back to Einstein in 1917.

For many years the cosmological constant was almost universally considered to be 0.

Q. And if the cosmological constant is there - what does that do to your work?

Moreover, there's no reason that the cosmological constant should be equal to 0.

The cosmological constant plays a similar role in general relativity.

The cosmological constant should be the same inside and outside of the embedded lens.

The current estimates for the cosmological constant are all very small, almost (but not quite) zero.

The identification of dark energy as a cosmological constant does not appear to be consistent with the data.

As noted above, the measured cosmological constant is smaller than this by a factor of 10.

Like gravity, the cosmological constant is a creature of geometry.

The cosmological constant has regained attention in recent decades as a hypothesis for dark energy.

For example, if the cosmological constant was, say, 10 percent of the maximum value consistent with life, that would be acceptable, he said.

The decay of the cosmological constant will be fatal, astronomers agree.

On the other hand, such models typically predict huge cosmological constants.

Here was where the cosmological constant came in.

The vanishing of the cosmological constant is the best example of this.

The cosmological constant is a sort of 'dark energy' that fills space and subspace.

Later on, the cosmological constant is introduced and problems with the amount of energy produced from virtual particles.

Following this realization, the cosmological constant was largely ignored as a historical curiosity.

The small but finite value of the cosmological constant can be regarded as a successful prediction in this sense.

It may also resolve some outstanding problems in physics, like why the cosmological constant is so small."

Curiously, the cosmological constant is once again in vogue.

These changes could modify significantly the physics of the early universe, if the cosmological constant was bigger back then.

The phases with negative cosmological constant will end in a Big Crunch.