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New Photometric and Spectroscopic Observations of the Eclipsing Binary V2080 Cygni

Dimitrov W., Kamiński K., Bąkowska K., Kamińska M. K., Tokarek J., Pawłowski M., Boneva D., Bartczak P., Kwiatkowski T., Schwarzenberg-Czerny A.

Acta Astronomica

2022

Vol. 72, No. 1

55--67

We present new spectroscopic and photometric measurements of the eclipsing binary V2080 Cyg. It is a detached system with similar components and an orbital period of 4.9 d. We collected spectroscopic data with two instruments, 1.88 m DDO telescope equipped with Cassegrain spectrograph and 0.5 m PST1 connected to a fiber-fed echell\'e spectrograph. We collected 127 measurements for each component, which significantly increase the number of available radial velocity measurements for the V2080 Cyg system. Obtained masses of the eclipsing components are M1=1.189± 0.007 and M2=1.138±0.007 M☉. We also collected a multicolor photometry. The three-band light curves obtained together with the radial velocity data enabled us to calculate the model of the system. New estimations of the orbital inclination and radii of the components were computed. We obtained as well new times of minima. The O-C diagrams indicate variation, which requires more recent data to be confirmed. The possible existence of a third body could cause a light-time effect in the system. In addition, we analyze the Gaia mission results. V2080 Cyg A has three visual companions. However, according to Gaia parallaxes and proper motions, they cannot be dynamically connected with the eclipsing binary and therefore are background stars.

Over a Century of δ Ceti Variability Investigation

Śreniawska E., Kamiński K., Kamińska M. K., Tokarek J., Zgórz M.

Acta Astronomica

2021

Vol. 71, No. 4

297--310

We present results of a 2014-2018 campaign of radial velocity measurements of δ Ceti. Combining our determination of pulsation period with historical data we conclude that the most likely explanation of observed changes is the presence of a secondary component with a minimum mass of 1.10±0.05 Mo on an orbit with a period of 169±6 yr. Consequently, we revised the intrinsic, evolutionary period change rate to be not larger than 0.018±0.004 s/century, which is significantly lower than previous estimations and is consistent with evolutionary models. We did not find any significant multiperiodic frequencies in radial velocity periodograms such as those reported in the photometric data from the MOST satellite. Using interferometric angular size of δ Ceti from JMMC Stellar Diameters Catalogue we determined several physical parameters of the star with bolometric flux method. They turned out to be consistent with most previous determinations, confirming lower mass and slower evolution of δ Ceti than obtained using different methods.