Speaker
Description
Abstract
Flaring activity is traditionally associated with stars possessing convective envelopes and strong magnetic dynamos. Normal A-type stars, characterized by purely radiative envelopes, are therefore expected to be magnetically inactive. However, recent surveys have reported flare-like events in several normal A-type stars, challenging current models of stellar magnetism. This project aims to detect and characterize flare activity in normal A-type stars using high-precision Kepler photometry, with spectroscopic follow-up where available.
The study will employ strict data preparation procedures including quality masking, removal of invalid data points, jump correction across segment boundaries, segmentation of light curves, and polynomial detrending. Flare detection will utilized a robust 3σ threshold based on the median absolute deviation (MAD), together with strict filtering based on duration, amplitude, and event merging criteria. Detected flares will be characterized in terms of amplitude, duration, peak time, and energy. Pixel-level analysis and spectroscopy will be used to distinguish intrinsic stellar flares from contamination or unresolved companions.
By expanding the sample of studied normal A-type stars, this work will provide a statistically meaningful assessment of flare occurrence in intermediate-mass stars.
Existing theoretical magnetic models are expected to be limited, as they have been developed and tested using only a small number of normal A-type stars, making them unreliable for broader application. A revision of these models will have the potential to reshape our understanding of stellar interiors, populations, evolution, and lifetimes. To address this limitation and fill the existing knowledge gap, it will be essential to expand the sample of normal A-type stars studied for flare activity. The results of this work are expected to place strong constraints on stellar magnetic field theories and will contribute to a revised understanding of stellar interiors, evolution, and magnetic activity in radiative stars.
| Stream | Science or Engineering |
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