Non-evolutionary effects on period change in Magellanic Cepheids

TL;DR

This study investigates short-term, non-evolutionary period changes in Magellanic Cloud Cepheids using over two decades of OGLE data, revealing phenomena related to binarity and non-linear pulsation effects.

Contribution

It provides the first systematic analysis of non-evolutionary period changes in Magellanic Cepheids, expanding understanding beyond traditional evolutionary models.

Findings

Identification of non-evolutionary period change phenomena in Cepheids

Evidence of binary system influences on period variations

Detection of non-linear pulsation effects affecting period stability

Abstract

Classical Cepheids are a cornerstone class of pulsators, fundamental to testing stellar evolution and pulsation theories. Their secular period changes, characterized through $O-C$ (Observed minus Calculated) diagrams, offer valuable insights into their evolution. While evolutionary period changes are well understood from both observational and theoretical perspectives, shorter timescale period changes (on the order of ($\sim$ 10$^{2}$-10$^{4}$ days) - known as non-evolutionary period changes are yet to be systematically explored. In this work, we present a detailed and comprehensive search for non-evolutionary period changes using $O-C$ analysis of Magellanic Cloud (MC) Cepheids, based on 20+ years of OGLE photometry data. Our sample includes both the Large Magellanic Cloud (LMC) and the Small Magellanic Cloud (SMC) Cepheids, focusing on single radial mode Cepheids (both fundamental (FU) and first overtone (FO) modes). The results are grouped into two phenomena: (a) Cepheids in binary systems (b) Non-linear period changes.