%0 Generic %1 citeulike:13944083 %A Gao, Qing %A Xin, Yu %A Liu, Ji-Feng %A Zhang, Xiao-Bin %A Gao, Shuang %D 2016 %K imported %T White-Light Flares on Close Binaries Observed with Kepler %U http://arxiv.org/abs/1602.07972 %X Based on Kepler data, we present the results of a search for white-light flares on 1049 close binaries. We identify 234 flare binaries, on which 6818 flares are detected. We compare the flare-binary fraction in different binary morphologies ("detachedness"). The result shows that the fractions in over-contact and ellipsoidal binaries are approximately 10-20 percent lower than those in detached and semi-detached systems. We calculate the binary flares activity level (AL) of all the flare binaries, and discuss its variations along the orbital period (P\_orb) and rotation period (P\_rot, calculated for only detached binaries). We find that AL increases with decreasing P\_orb or P\_rot up to the critical values at P\_orb near 3 days or P\_rot near 1.5 days, thereafter, the AL starts decreasing no matter how fast the stars rotate. We examine the flaring rate as a function of orbital phase in 2 eclipsing binaries on which a large number of flares are detected. It appears that there is no correlation between flaring rate and orbital phase in these 2 binaries. In contrast, when we examine the function with 203 flares on 20 non-eclipse ellipsoidal binaries, bimodal distribution of amplitude weighted flare numbers shows up at orbital phase 0.25 and 0.75. Such variation could be larger than what is expected from the cross-section modification.

@misc{citeulike:13944083, abstract = {{Based on Kepler data, we present the results of a search for white-light flares on 1049 close binaries. We identify 234 flare binaries, on which 6818 flares are detected. We compare the flare-binary fraction in different binary morphologies ("detachedness"). The result shows that the fractions in over-contact and ellipsoidal binaries are approximately 10-20 percent lower than those in detached and semi-detached systems. We calculate the binary flares activity level (AL) of all the flare binaries, and discuss its variations along the orbital period (P\_orb) and rotation period (P\_rot, calculated for only detached binaries). We find that AL increases with decreasing P\_orb or P\_rot up to the critical values at P\_orb near 3 days or P\_rot near 1.5 days, thereafter, the AL starts decreasing no matter how fast the stars rotate. We examine the flaring rate as a function of orbital phase in 2 eclipsing binaries on which a large number of flares are detected. It appears that there is no correlation between flaring rate and orbital phase in these 2 binaries. In contrast, when we examine the function with 203 flares on 20 non-eclipse ellipsoidal binaries, bimodal distribution of amplitude weighted flare numbers shows up at orbital phase 0.25 and 0.75. Such variation could be larger than what is expected from the cross-section modification.}}, added-at = {2019-03-25T08:20:55.000+0100}, archiveprefix = {arXiv}, author = {Gao, Qing and Xin, Yu and Liu, Ji-Feng and Zhang, Xiao-Bin and Gao, Shuang}, biburl = {https://www.bibsonomy.org/bibtex/296063c1fb33fcf80b023149bfe81c6ea/ericblackman}, citeulike-article-id = {13944083}, citeulike-linkout-0 = {http://arxiv.org/abs/1602.07972}, citeulike-linkout-1 = {http://arxiv.org/pdf/1602.07972}, day = 25, eprint = {1602.07972}, interhash = {9bb7998caa5aea347db6aa3f2e68c6b4}, intrahash = {96063c1fb33fcf80b023149bfe81c6ea}, keywords = {imported}, month = feb, posted-at = {2016-02-29 06:20:40}, priority = {2}, timestamp = {2019-03-25T08:20:55.000+0100}, title = {{White-Light Flares on Close Binaries Observed with Kepler}}, url = {http://arxiv.org/abs/1602.07972}, year = 2016 }