The white-light superflares from cool stars in GWAC triggers
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arXiv
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| Main Authors: | , , , , , , , , , , , , , , , , , , |
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| Format: | Preprint |
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2024
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| author | Li, Guang-Wei Wang, Liang Yuan, Hai-Long Xin, Li-Ping Wang, Jing Wu, Chao Li, Hua-Li Haerken, Hasitieer Wang, Wei-Hua Cai, Hong-Bo Han, Xu-Hui Xu, Yang Huang, Lei Lu, Xiao-Meng Bai, Jian-Ying Wang, Xiang-Yu Dai, Zi-Gao Liang, En-Wei Wei, Jian-Yan |
| author_facet | Li, Guang-Wei Wang, Liang Yuan, Hai-Long Xin, Li-Ping Wang, Jing Wu, Chao Li, Hua-Li Haerken, Hasitieer Wang, Wei-Hua Cai, Hong-Bo Han, Xu-Hui Xu, Yang Huang, Lei Lu, Xiao-Meng Bai, Jian-Ying Wang, Xiang-Yu Dai, Zi-Gao Liang, En-Wei Wei, Jian-Yan |
| contents | M-type stars are the ones that flare most frequently, but how big their maximum flare energy can reach is still unknown. We present 163 flares from 162 individual M2 through L1-type stars that triggered the GWAC, with flare energies ranging from $10^{32.2}$ to $10^{36.4}$ erg . The flare amplitudes range from $\triangle G = 0.84$ to $\sim 10$ mag. Flare energy increases with stellar surface temperature ($T_{\rm eff}$) but both $\triangle G$ and equivalent duration $\log_{10}(ED)$ seem to be independent of $T_{\rm eff}$. Combining periods detected from light curves of TESS and K2, spectra from LAMOST, SDSS and the 2.16 m Telescope, and the Gaia DR3 data, we found that these GWAC flare stars are young. For the stars that have spectra, we found that these stars are in or very near to the saturation region, and $\log_{10}(L_{\rm Hα}/L_{\rm bol})$ is lower for M7-L1 stars than for M2-M6 stars. We also studied the relation between GWAC flare bolometric energy $E_{\rm bol}$ and stellar hemispherical area $S$, and found that $\log_{10}E_{\rm bol}$ (in erg) increases with increasing $S$ (in cm$^2$), and the maximum flare energy $\log_{10}E_{\rm bol, max} \geqslant \log_{10}S + 14.25$. For M7-L1 stars, there seem to be other factors limiting their maximum flare energies in addition to stellar hemispherical area. |
| format | Preprint |
| id |
arxiv_https___arxiv_org_abs_2407_08183 |
| institution | arXiv |
| publishDate | 2024 |
| record_format | arxiv |
| spellingShingle | The white-light superflares from cool stars in GWAC triggers Li, Guang-Wei Wang, Liang Yuan, Hai-Long Xin, Li-Ping Wang, Jing Wu, Chao Li, Hua-Li Haerken, Hasitieer Wang, Wei-Hua Cai, Hong-Bo Han, Xu-Hui Xu, Yang Huang, Lei Lu, Xiao-Meng Bai, Jian-Ying Wang, Xiang-Yu Dai, Zi-Gao Liang, En-Wei Wei, Jian-Yan Solar and Stellar Astrophysics M-type stars are the ones that flare most frequently, but how big their maximum flare energy can reach is still unknown. We present 163 flares from 162 individual M2 through L1-type stars that triggered the GWAC, with flare energies ranging from $10^{32.2}$ to $10^{36.4}$ erg . The flare amplitudes range from $\triangle G = 0.84$ to $\sim 10$ mag. Flare energy increases with stellar surface temperature ($T_{\rm eff}$) but both $\triangle G$ and equivalent duration $\log_{10}(ED)$ seem to be independent of $T_{\rm eff}$. Combining periods detected from light curves of TESS and K2, spectra from LAMOST, SDSS and the 2.16 m Telescope, and the Gaia DR3 data, we found that these GWAC flare stars are young. For the stars that have spectra, we found that these stars are in or very near to the saturation region, and $\log_{10}(L_{\rm Hα}/L_{\rm bol})$ is lower for M7-L1 stars than for M2-M6 stars. We also studied the relation between GWAC flare bolometric energy $E_{\rm bol}$ and stellar hemispherical area $S$, and found that $\log_{10}E_{\rm bol}$ (in erg) increases with increasing $S$ (in cm$^2$), and the maximum flare energy $\log_{10}E_{\rm bol, max} \geqslant \log_{10}S + 14.25$. For M7-L1 stars, there seem to be other factors limiting their maximum flare energies in addition to stellar hemispherical area. |
| title | The white-light superflares from cool stars in GWAC triggers |
| topic | Solar and Stellar Astrophysics |
| url | https://arxiv.org/abs/2407.08183 |