We usually have an image of scientists who study the Universe doing so peering through a telescope. And, effectively, this is what astrophysicists do: gather data about the observable phenomena of the Universe.
However, in order to interpret this data, i.e. to explain the majority of the phenomena occurring in the Universe, complicated calculations with a computer are required and which have to be based on appropriate mathematical models. This is what the Gravitation and Cosmology research team at the University of the Basque Country (UPV/EHU) is involved in: analysing models capable of explaining the evolution of the Universe.
Supernovas, witnesses to acceleration
One of the phenomena that standard models of physics have not yet been able to explain is that of the accelerated expansion of the Universe. Although Einstein proposed a static model to describe the Cosmos, today it is well known, thanks to supernovas amongst other things, that it is, in fact, expanding. Supernovas are very brilliant stellar explosions that, precisely due to this, provide useful data for exploring very distant regions of the Universe. By measuring the quantity of light that gets to us from a supernova, we can calculate its distance from us, and its colour indicates the speed at which it is distancing itself from us – the more reddish it is, the faster it is travelling. In other words, comparing two supernovas, the one that is distancing itself more slowly from us is a more bluish colour. According to observations by astrophysiscists, besides supernovas distancing themselves from us, they are doing so more and more rapidly, i.e. distancing themselves at an accelerated velocity, just like the rest of the material of the Universe.
Looking for dark energy
The energy known to exist in the Universe, however, is not sufficient to cause such acceleration. Thus, the theory most widely accepted within the scientific community is that there exists a ‘dark energy’, i.e. an energy that we cannot detect except by the gravitational force that it produces. In fact, it is believed that 73% of the energy of the Universe is dark. The dark energy debate is not just any theory: its existence has not been proved but, without it, standard models of physics would not be able to explain many of the phenomena occurring in the Universe.
So, what is dark energy exactly? What are its characteristics and have these properties always been the same or have they changed over time? These are questions, amongst others, that researchers at the Faculty of Science and Technology at the UPV/EHU, under the direction of Dr. Alexander Feinstein, are seeking to answer.
The unique characteristic of dark energy known to us is that it possesses repulsive gravitational force. That is, unlike the gravity we know on Earth, this force tends to distance stars, galaxies and the rest of the structures of the Universe from each other. This would explain why the expansion of the Universe is not constant, but accelerated. Nevertheless, this phenomenon can only be detected when achieving observationally enormous, almost unimaginable distances. This is why it is so difficult to understand the nature of dark energy.
The theory of phantom energy
To what point can the Universe expand? If this repulsive force is ever more intense, might it be infinite? This is one of the problems that the UPV/EHU researchers are focusing on. Such powerful dark energy is known as phantom energy, with which the Universe is able to expand to such an extent that the structures we know today would disappear.
This research group considers that the phantom energy model may be the most suitable to explain the accelerated expansion of the Universe. Amongst other things, the team has come to this conclusion after analysing the distribution of galaxies and the background microwave radiation which has inundated all of the Cosmos since shortly after the Big Bang. These waves travel in every direction and enable the exploration of what occurred at tremendously remote instants in time, moments close to the start of it all.
Lucía Álvarez | alfa
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