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.
%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
}