Is this project an undergraduate, graduate, or faculty project?
Undergraduate
Project Type
individual
Campus
Daytona Beach
Authors' Class Standing
Jadia Ewing, Senior
Lead Presenter's Name
Jadia Ewing
Lead Presenter's College
DB College of Arts and Sciences
Faculty Mentor Name
Stephen Gillam
Abstract
Rapidly oscillating Ap (rOAp) stars are a rare subclass of chemically peculiar A-type stars that exhibit high-frequency pulsations driven by strong magnetic fields and ionization zones in the photosphere. These pulsations, observed between 1–4 mHz provide insight into stellar interiors and magnetic fields. Pulsations were analyzed between 0–10 mHz. Studying these oscillations allows for a better understanding of magneto-acoustic coupling in stellar atmospheres and the evolution of peculiar main sequence stars. In this study, photometric time-series analysis was used to extract the dominant oscillation frequencies of a candidate rOAp star observed with the Southeastern Association for Research in Astronomy telescope at the Kitt Peak National Optical Observatory. We observed a potential rOAp star, NGC 2264-196, located in the young open cluster NGC2264. Fourier analysis and least-squared fitting were applied to the extracted light curve to estimate the initial frequencies. These frequencies and amplitudes were refined, and the phases were found by least-squares fitting to the light curve. The amplitude spectrum of NGC2264-196 exhibits the following frequencies within the rOAp range: principal frequency at 0.5464 mHz with an amplitude of 0.0018 mag which may be a possible Delta Scuti frequency. Secondary rOAp frequencies were detected at 2.6805 mHz with an amplitude of 0.0022 mag, 3.0220 mHz with an amplitude of 0.0021 mag, and 3.8558 mHz with an amplitude of 0.0017 mag. More observational analysis is needed to confirm these frequencies.
Did this research project receive funding support (Spark, SURF, Research Abroad, Student Internal Grants, Collaborative, Climbing, or Ignite Grants) from the Office of Undergraduate Research?
No
Looking for new rOAp Stars in the Young Open Cluster NGC2264
Rapidly oscillating Ap (rOAp) stars are a rare subclass of chemically peculiar A-type stars that exhibit high-frequency pulsations driven by strong magnetic fields and ionization zones in the photosphere. These pulsations, observed between 1–4 mHz provide insight into stellar interiors and magnetic fields. Pulsations were analyzed between 0–10 mHz. Studying these oscillations allows for a better understanding of magneto-acoustic coupling in stellar atmospheres and the evolution of peculiar main sequence stars. In this study, photometric time-series analysis was used to extract the dominant oscillation frequencies of a candidate rOAp star observed with the Southeastern Association for Research in Astronomy telescope at the Kitt Peak National Optical Observatory. We observed a potential rOAp star, NGC 2264-196, located in the young open cluster NGC2264. Fourier analysis and least-squared fitting were applied to the extracted light curve to estimate the initial frequencies. These frequencies and amplitudes were refined, and the phases were found by least-squares fitting to the light curve. The amplitude spectrum of NGC2264-196 exhibits the following frequencies within the rOAp range: principal frequency at 0.5464 mHz with an amplitude of 0.0018 mag which may be a possible Delta Scuti frequency. Secondary rOAp frequencies were detected at 2.6805 mHz with an amplitude of 0.0022 mag, 3.0220 mHz with an amplitude of 0.0021 mag, and 3.8558 mHz with an amplitude of 0.0017 mag. More observational analysis is needed to confirm these frequencies.