Be stars are young, massive, very hot stars with a high rotation speed that have a disk-shaped envelope around them, generated by material ejected from the star itself.<\/p>\n\n\n\n
These are stars classified as B, whose temperature ranges from 10,000 to 33,000 degrees and their radius is between 2 and 6.5 times the radius of our Sun. The letter \u00abe\u00bb is used to identify certain B-type stars that exhibit energy emission in the hydrogen spectral line H alpha. This emission is produced by the reprocessing of ultraviolet light from the star as it penetrates the surrounding gaseous disk.<\/p>\n\n\n\n
The high rotation speed slightly deforms the star at the equator, making it look more like a flattened ball. Some models indicate that the core rotates independently of the spin of the rest of the star.<\/p>\n\n\n\n
Theoretical models also point to the existence of seismological processes (such as earthquakes, but in stars, known as non-radial oscillations) in their interior that cause pulsations; that is, some parts of the star expand while other parts contract.<\/p>\n\n\n\n
The pulsations, along with the star’s high rotation speed and magnetic field, are responsible for the formation of the gas disk around it.<\/p>\n\n\n\n
Sometimes, Be stars can have a neutron star as a companion. These stars are very compact and have very strong magnetic fields, and their interaction with the disk of the Be produces the emission of light in X-rays. In these cases, the two-star system is classified as a BeX-type.<\/p>\n\n\n\n
In this model, the main characteristics of the theoretical model of a Be-type star have been represented.<\/p>\n\n\n\n
The center of the model is occupied by the star, shown as a slightly elongated bulge, like a melon. The bulge protrudes above and below the disc.<\/p>\n\n\n\n
The pulsations of the star have been represented as subtle protuberances on its surface.<\/p>\n\n\n\n
At the bottom, an opening has been left that allows access to the core of the star, represented by a ball. Since the core has a spin independent of the rest of the star, we have left this ball free, so that it can be spinned.<\/p>\n\n\n\n
Spiral-shaped structures depart from the star, representing ejected matter, as if it were water thrown out by a rotating sprinkler in a garden. This stellar gas remains for a while around the star forming the disk. As we move away from the star, the disk is scattered through space, a fact that is shown in the area of the outer edge of the model.<\/p>\n\n\n\n
This work has been carried out with a grant from the R&D&I \u2018Proof of Concept\u2019 2022 (PDC2022) call for projects, financed by the European Union through the NextGenerationEU Recovery, Transformation and Resilience Plan. Project\u2019s reference: PDC2022-133930-I00.<\/p>\n\n\n\n