Alma detects for the first time a millimetre radiation of kelon stars

Alma detects for the first time a millimetre radiation of kelon stars

Short-period gamma flashes last only a fraction of a second, making it difficult to detect them, and they seem to occur mainly at the early stages of the history of the observed space. It is now generally assumed that these are the collisions of neutron stars that produce so-called kylon stars. There are still unsolved riddles, but it is now known that the body of the Alma radio telescope can help solve them by seeing them for the first time in its range of wave lengths.

Many of the advances in astronomy resulted from the opening of a new observation window in a new band of electromagnetic spectrum, with X-rays showing star black holes, infrared rays showing the interior of star shelters, and decimeter radio waves showing the structure of the Milky Way sleeve.

This is one of the reasons why the Atakam large millimeter/submillimeter array was developed. Another additional reason is that the array of radio telescopes built in this way allows the synthesis of apertures and thus has a very large virtual instrument without the need to create it.

Today we learn that the network of Alma radio telescopes has been used for the first time to observe astrophysical processes associated with kylons in millimetres and submillimeter radio bands, which are collisions of neutron stars that were first discovered in the form of short gamma flashes and whose nature has only recently been discovered, even though it has been suspected for decades. The energy available is enormous, making gamma flashes one of the most vivid phenomena in space.

A key point in this definition was the development of multichannel astronomy systems, with simultaneous detection of Ligo and Virgo gravitational waves from the GW170817 source, clearly linked in the sky to the emission of electromagnetic waves in X-ray and gamma ranges.

Clashes of neutron stars that produce gold and platinum

This time, astrophysicists published an article in The Astrophic Journal Letters, a version of which is freely available on arXiv, on the short gamma flash of GRB 211106A, which will be seen, as shown by the name of the gamma flash.

The result of the thermonuclear fusion was not only to produce a thermonuclear reaction that produced heavy elements such as gold and platinum, but also a competing beam of very high-speed particles, which also produced a collimated beam of high-energy gamma-fotons; the earth passed through that beam by accident as an observer lit by a lighthouse.

As particles and gamma-photons are introduced into the interstellar environment, it excites it and causes the matter to light up in return. This is the last light that was first discovered in the spectrum range that Alma had access to. Prior to the instrument, millimeters of telescopes were not sufficiently sensitive to detect these readings, because GRB is often visible billions of light years away from the Milky Way. Therefore, we observe only old GRB, and we suspect that for some unknown reason they were more numerous during the first few billion years of space history. In fact, GRB 211106A occurred when the age of the observed universe was only 40 per cent of its current age. Although the Kilons are well visible at a distance in gamma rays, this cannot be said to be after-light, which is much less pronounced.

Initially, when only GRB X-rays 211106A were detected using the Swift satellite, astrophysicists thought that a kilone could come from a nearby galaxy, although it could not be linked to it by visible Hubble observations, probably due to the presence of a large amount of dust in the line of visibility near GRB.

But finally, with Alma, it was possible to find a weak, distant galaxy where the gamma flash occurred. After determining the distance, it was concluded that this was one of the most powerful GRBs found to date.

Alma, combined with the observations of the James Webb Space Telescope, should allow further progress in the study of short gamma flashes.