2014/02/28 by Ian D. Howarth, K. J. F. Goss, I. R. Stevens +2
Physics and Astronomy · #Amplitude #Astro and Planetary Science #Astronomy #Astrophysics #Astrophysics and Star Formation Studies #Optics #Photometry (optics) #Physics #Satellite #Stars #Stellar, planetary, and galactic studies #astro-ph.SR
paper · pdf · doi:10.1093/mnras/stu398
MNRAS, in press
arxiv created 2014/03/08 · openalex publication_date 2014/03/25 · arxiv updated 2015/06/18 · openalex created_date 2025/10/10 · openalex updated_date 2026/08/05
We report a time series analysis of satellite photometry of the non-radially pulsating Oe star ζ Oph, principally using data from the Solar Mass Ejection Imager obtained during 2003–2008, but augmented with Microvariability and Oscillations of STars and Wide-field InfraRed Explorer results. Amplitudes of the strongest photometric signals, at 5.18, 2.96 and 2.67 d−1, each vary independently over the |5(1)/(2)|-year monitoring period (from ∼50 to ≲2 mmag at 5.18 d−1), on time-scales of hundreds of days. Signals at 7.19 and 5.18 d−1 have persisted (or recurred) for at least two decades. Supplementary spectroscopic observations show an Hα emission episode in 2006; this coincided with small increases in amplitudes of the three strongest photometric signals.