Is this project an undergraduate, graduate, or faculty project?
Undergraduate
group
What campus are you from?
Daytona Beach
Authors' Class Standing
Aakash Rathinam Thiyagarajan, Senior Soren Barnier III, Junior Avery Reynolds, Junior Jacob Romeo, Senior Diveyeshwari Vansadia, Senior Laina Tallman Bogusta, Senior Leila Alamos, Graduate Savannah Caldwell, Graduate Lillyanne Pepe, Graduate
Lead Presenter's Name
Aakash Rathinam Thiyagarajan
Faculty Mentor Name
Dr. Stephen Gillam
Abstract
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.
Did this research project receive funding support from the Office of Undergraduate Research.
Yes, Collaborative Grant
Investigating Frequency Variability and Rotational Rate of KIC7582608
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.