Two-Component Variability of the Semi-Regular Pulsating Star U Delphini

TL;DR

This study analyzes the complex variability of the semi-regular star U Delphini, revealing multiple periodicities, amplitude variations, and phase shifts, using extensive photometric data and advanced analysis methods.

Contribution

It introduces a detailed analysis of U Delphini's variability, identifying multiple periodic components and their characteristics, which enhances understanding of semi-regular pulsating stars.

Findings

Main period of 1198 days with amplitude 0.499m

Faster oscillation period of 119.45 days with amplitude 0.303m

Detected phase jump near JD 2452589

Abstract

Photometric analysis of photometric variability of the semi-regular pulsating variable U Del is analyzed. From the international AFOEV database, 6231 brightness values in the time interval JD 2451602-55378 were chosen. For the periodogram analysis, we have used a trigonometric polynomial fit. Using the criterion of minimal variance of the approximation at arguments of observations, the optimal degree is s=1. Initial epoch for maximum is T0=JD2453340(3), the period P=1198(4)d. Mean brightness at maximum is 6.624(5), at minimum 7.124(5), i.e. the amplitude is 0.499(5)m. Besides this slow variability, there is a faster oscillation of a period of 119.45(6)d, amplitude 0.303(5)m and an initial epoch for maximum 2453215.1(5). These results are mean during the time interval after that analyzed in the catalogue of Chinarova and Andronov (2000). Also the method of "running sines" with a filter half-width Delta t=0.5P. The local mean (averaged over a short period) brightness varies in a range 6.58-7.41m, the semi-amplitude exhibits very strong variations from 0.01 to 0.46m. The phase is also variable - typically of a full amplitude of 0.5. Close to JD 2452589, occurred a phase jump by a complete period during a descending branch of a slow wave. This effect was not observed during other cycles. No significant correlation between mean brightness and amplitude of short-period oscillation was found. Despite significant variability of amplitude, the periodic contribution is not statistically significant. Also characteristics of individual brightness extrema were found. The study was made in a course of the international project "Inter-Longitude Astronomy" (Andronov et al., 2010) and national project "Ukrainian Virtual Observatory (Vavilova et al., 2012).