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Astronomers at the University of Toulouse in France have revealed the nature of the star TIC 441725813, revealing it to be a hybrid pulsating subdwarf star. The report said the findings have been published on the arXiv preprint server Japanese. Az refer to Lenta.ru.
TIC 441725813 (also known as TYC 4427-1021-1) is a hybrid hot subdwarf B (sdB) star, a special type of star called a pulsating star. In the core of these dense, hot objects, helium burning occurs, while a thin shell consists of hydrogen. Two types of pulsations are known: short-period pressure modes (p-modes) and long-period gravity modes (g-modes).
The researchers analyzed photometric data from NASA’s TESS satellite and performed a detailed analysis of the light curve of TIC 441725813. They identified a variety of features, including low and high frequencies, and the presence of g-modes and p-modes.
Based on the frequencies of the two modes, the rotation periods of the core and shell of the star were estimated. The core of the star rotates slowly, with a period of about 85.3 days, while the shell rotates much faster, with a period of about 17.9 days.
The study authors suggest that TIC 441725813 could be part of a short-period binary system consisting of a B subdwarf and a white dwarf, with an orbital period of about 6.7 hours. This would explain the significant difference in the rotation speeds of the stellar core and outer shell. However, additional spectroscopic observations are needed to confirm this hypothesis.
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