Dark Energy: When the Universe Defies Its Own Gravity

Discovery of Cosmic Acceleration

In 1998, two independent teams led by Saul Perlmutter (1959-), Brian P. Schmidt (1967-), and Adam Riess (1969-) discovered, through the study of Type Ia supernovae, that the expansion of the Universe was not slowing down due to gravity as previously thought, but was actually accelerating. To explain this observation, cosmologists introduced the concept of dark energy, a mysterious component representing about 70% of the total energy content of the Universe.

Hypothetical Nature of Dark Energy

Dark energy is sometimes equated with a cosmological constant \(\Lambda\), a term added to Einstein's equations of general relativity (1915). It can be interpreted as an intrinsic property of the quantum vacuum (quantum vacuum: minimal energy state of quantum field theory), or as a form of dynamic scalar field (quintessence). Its negative pressure would exert a gravitational repulsion, causing the acceleration of the expansion. However, its physical origin remains unknown.

Cosmological Equations

Within the framework of the Friedmann-Lemaître-Robertson-Walker model, the expansion equation is written as: \(\;H^2 = \frac{8\pi G}{3}\rho - \frac{k}{a^2} + \frac{\Lambda}{3}\;\) where \(H\) is the Hubble constant, \(\rho\) is the total matter-energy density, \(k\) is the spatial curvature, and \(\Lambda\) is the cosmological constant. A term \(\Lambda >0\) leads to accelerated expansion.

Accelerated Expansion and Multiverse Hypotheses

Some cosmological theories propose the existence of a multiverse (multiverse: hypothetical set of distinct universes), where our Universe would be just one bubble among others. In this context, it has been suggested that accelerated expansion could result not only from intrinsic dark energy but also from gravitational interactions or energy flows between neighboring universes.

According to these models, each universe would have its own physical constants and energy density. The gravitational forces exerted by neighboring universes could induce an apparent effect of repulsion or acceleration of the expansion of our cosmic bubble. This hypothesis remains speculative and difficult to test with current observations, but it offers an alternative to standard models based solely on the cosmological constant \(\Lambda\).

Theoretical work using string theory and branes suggests that fluctuations in the quantum vacuum or variations in the tension of universal membranes could influence the expansion of our observable Universe. These ideas have been discussed notably by Lisa Randall (1962-) and Juan Maldacena (1968-) in the context of brane models.

N.B.:
String theory proposes that fundamental particles are vibrating strings in a 10- or 11-dimensional space. Each possible configuration of the extra dimensions (Calabi-Yau manifolds) defines a "vacuum" with its own physical constants. This multitude of possible solutions is called the landscape (landscape: set of possible solutions of string theory), and it naturally leads to the idea of a multiverse (multiverse: hypothetical set of distinct universes): our universe would then be just one bubble among a set of universes with different physical properties.

Comparison with Other Components of the Universe

Dark energy now dominates cosmological evolution, ahead of dark matter and ordinary matter. This imbalance was established about 5 billion years ago, when the density of matter decreased to the point of becoming less than that of dark energy.

• Sources: NASA WMAP (new window), ESA Planck Mission (new window), Nobel Prize in Physics 2011 (new window).

N.B.:
Dark energy remains a cosmological hypothesis. It is not observed directly but deduced from dynamic effects on expansion.