Astronomers have conducted a photometric and spectroscopic study of an Algol-type binary, known as XZ Ursae Majoris (or XZ UMa for short). Results of the study, presented in a paper published December 21 on the pre-print server arXiv, indicate that this binary is a pulsating system.
XZ UMa is a semi-detached Algol-type system with a spectral type of A5+F9. It has an orbital period of approximately 1.22 days and the primary component of the system is estimated to have an effective temperature of about 7,766 K.
Previous observations have suggested that XZ UMa exhibits pulsations; however, no evidence confirming this hypothesis has been found. Some studies also found that the orbital period of XZ UMa changed over the years, which pointed to the presence of a third object in the system about half as massive as the sun.
In order to verify these theories, a team of astronomers led by Jae Woo Lee of the Korea Astronomy and Space Science Institute in Daejeon, South Korea, have conducted high-resolution spectroscopic observations of XZ UMa with the Bohyunsan Observatory Echelle Spectrograph and the 1.8-m telescope at Bohyunsan Optical Astronomy Observatory (BOAO). The study was complemented by photometric data from NASA’s Transiting Exoplanet Survey Satellite (TESS).
Lee’s team managed to identify at least six possible independent pulsation frequencies of XZ UMa. Their periods and constants of these pulsations were measured to be between 28 and 37 minutes, and 0.013–0.016 days, respectively. The pulsational-orbital-period ratios for the high frequencies turned out to be 0.016–0.021, suggesting that the primary star XZ UMa A is a Delta Scuti-type pulsator.
2024-01-04 21:00:04
Original from phys.org rnrn
