Determination of X-Ray Flare Behavior during Solar Activity with OPEA Model
Makaleler > Tam Makale · 2024
Yazarlar: YOLDAŞ, Ezgi
Zenodo (CERN European Organization for Nuclear Research), Uluslararası, 2024
Özet
Within the scope of this study, it was tested whether the change detected in the solar flare activity during the doctoral thesis study was also seen in other stars. In the thesis study, it has been shown that the OPEA models obtained with solar flare data created at one-month time intervals change even in a one-month time interval. However, the literature shows that the OPEA model obtained for dMe stars is constant in each star and does not change over time, and that the OPEA model is shaped according to the B-V color index of that star. However, not only did the OPEA model obtained with solar data change over time, but it was also observed that the model exhibited division in the same time period. Although there are divisions in OPEA models in a few examples in the literature, the real reason for this division is not understood because those sources are double stars. The results obtained in this study showed that although no division could be observed in the models created with V1005 Ori's flare data, the OPEA model exhibited division in almost every observation data of AD Leo. The physical reasons why the OPEA model of one of the two sources exhibits division in almost every period, while the OPEA model of the other source remains stable, are unclear. Both sources are dMe type young main sequence stars. Although there are some debates in the literature, it is known that the sources are single stars. Thus, the split in AD Leo's OPEA model appears to be related to the stellar dynamo process.