Aakash Rathinam Thiyagarajan Stephen Gillam Leila Alamos Lillyanne Pepe Savannah Caldwell Soren Barnier III Laina Tallman Bogusta Divyeshwari Vansadia Avery Reynolds Jacob Romeo
Embry-Riddle Aeronautical University
Rapidly Oscillating, chemically peculiar A (roAp) stars, positioned at the junction of the classical instability strip and the main sequence, are known for their unique pulsation behaviors. Our invest..
Rapidly Oscillating, chemically peculiar A (roAp) stars, positioned at the junction of the classical instability strip and the main sequence, are known for their unique pulsation behaviors. Our investigation centers on KIC7582608, distinguished by its intrinsically large amplitude pulsations, ensuring a detectable signal. Kepler mission data unveiled a single-mode oblique pulsation at 2.1034 mHz. While the κ-mechanism is the assumed driving force behind roAp star pulsations, We found intrinsic frequency variability that challenges this notion. Two interpretations emerge: intrinsic frequency variability due to pulsation cavity changes, or a binary companion causing Doppler shifts, leading to frequency modulation (FM). We observed KIC7582608 on a total of 18 nights utilizing Southeastern Association for Research in Astronomy telescopes and isolated the principal frequency using built-in Fourier analysis in PeriodO4. Our tentative result is that the principal pulsation (frequency 2.10688 mHz) varies in amplitude with a period of (20.45260699 +/- 0.0191056)mHz and an amplitude of (1.3083317 +/- 0.166450) mmag, indicates that we have measured the rotation rate of this KIC7582608. This study seeks the origins of the frequency variability, offering insights into the internal dynamics of roAp stars and the potential influences of external companions or circumstellar environments. By doing so, we contribute to a broader understanding of pulsating stars.
