The characteristics of the multiple star "sigma Orionis" are determined
Some three million years ago hundreds of stars formed from a dense cloud of gas and dust in the constellation of Orion (“the Hunter”). The star which swallowed the largest part of the mass was sigma Orionis (sigma Ori), which is now the fourth brightest star in the belt of Orion, and which illuminates the famous Horsehead Nebula. At the same time as sigma Orionis, a large number of stars with a full range of masses formed in its neighbourhood, as well as brown dwarfs, and “rogue” planets (objects similar in mass to that of a Jupiter but which do not rotate around a star, rather they move freely in the star cluster). The smallest objects in Orion´s belt have 10,000 times less mass than sigma Orionis.
To understand the frequency of the birth of low mass stars, brown dwarfs, and rogue planets, and how they evolve, we need first to know what happens to their high mass, blue neighbours. With this in mind, an international team of astronomers led by the Spanish researchers Sergio Simón-Díaz, (IAC/ULL), Jose A. Caballero (CAB, CSIC-INTA), and Javier Lorenzo ( University of Alicante), with the participation of the Institute of Astrophysics of Andalusia, have studied in great detail the multiple star sigma Orionis.
Localización de la estrella “sigma Orionis”. Fuente: IAC.
Even eons after their deaths one can observe the unique imprint of high mass stars on almost everything around them: our own chemical composition, the distribution in space of the stars and the nebulae which they leave behind after they have exploded, the form of the spiral arms of the galaxies, and even, curiously enough, the number of low mass stars. “This latter effect –explains Sergio Simón-Díaz, who is first author on the paper- is due to the fact that low mass stars, and brown dwarfs (which are objects with masses between those of the smallest stars and the largest planets) are just the left-overs from the banquets of high mass stars”.
The star sigma Orionis is 3 million years old and has a high temperature: its surface temperature is 30,000K five times hotter than that of the Sun. This very high temperature makes the star have a blueish colour, in contrast to less massive stars which have reddish colours. “In 2011” –remembers Caballero- “we showed that sigma Orionis is really a multiple star consisting of six stars instead as five, as previously thought: two of them are very high mass stars, which are very close together, rotating mutually around each other with an orbital period of some 143 days. A third star, also massive, is orbiting at 100 astronomical units (100 times the distance from the Earth to the Sun) from the other two, and rotates with a much longer period, of some 157 years. The cluster is completed with three other stars, a little cooler and less massive, as well as numerous stellar remnants”.
Now these researchers, together with 11 others from Spain, Germany, Chile, the USA, Belgium, and Hungary, have observed in more detail the central trio of these stars, (sigma Ori Aa, sigma Ori Ab, and sigma Ori B), and have measured their physical parameters with unprecedented accuracy. “ The period of the closest pair, of around 143 days, has now been determined with an uncertainty of only 11 minutes” –points out Simón-Díaz-,” which makes it feasible to programme specific observations at certain phases, for example with X-ray telescopes in space at periastron, the point where the two central stars are separated by their smallest distance”.
The study has also allowed us to determine very accurately the masses of the three stars using different methods. “The sum of the masses of the trio is bigger than 40 times the mass of the Sun”, emphasizes Simón-Díaz. “These observations, together with interferometric observations now in progress, are an excellent input to theoretical modes which aim at explaining the structure and the fate of these “gobbler stars”.
“We have also measured” –adds Caballero- “the rate of emission of high energy photons from the trio. These photons, emitted by sigma Orionis Aa, Ab, and B and those which ‘comb the mane’ of the Horsehead Nebula, and announce the start of a new banquet of high mass stars in the region. In just a few million years, when sigma Orionis Aa (and perhaps Ab) explodes as a supernova, and cleans out the region around it, a large number of smaller, cooler stars will continue to exist, as well as a few large, massive, very hot stars, which at the present moment are inside the dense clouds near the Horsehead Nebula”.