Cosmic rays are rays of energetic particles and radiation, with their composition in our own Galaxy being dominated by protons. Ellis Owen, a final-year PhD student working on cosmic rays, star-formation and galaxy evolution, tells us about his research on them.
One of the main challenges in modern cosmology is to understand how the very low-density matter between galaxies (known as the inter-galactic medium, or IGM) came to be hot and ionized today, reaching temperatures of up to 10 million degrees. It hasn’t always been this way – after the Big Bang the Universe expanded and cooled, eventually reaching temperatures low enough for much of the Hydrogen and Helium plasma within it to combine and form a neutral atoms in a process known as recombination around 378,000 years after the Big Bang. After this, the expansion and cooling of the Universe continued for hundreds of millions of years, leaving it in a dark and increasingly cold state – an era cosmologists refer to as the ‘Dark Ages’.
Hi, I’m Ellis Owen and I’m a first-year PhD student in the Theoretical Astrophysics Group here at MSSL. My work is focused on the Epoch of Reionization, a time when the Universe was only a few hundred million years old, when the first stars were beginning to form.