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J/other/NewA/41.17 Time of minima of BX Peg (Li+, 2015)
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Beginning of ReadMe :J/other/NewA/41.17 Time of minima of BX Peg (Li+, 2015)
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Four color light curves and period changes investigation of the
contact binary BX Peg.
Li K., Hu S., Guo D., Jiang Y., Gao D., Chen X.
<New Astron., 41, 17-21 (2015)>
=2015NewA...41...17L (SIMBAD/NED BibCode)
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ADC_Keywords: Binaries, eclipsing
Keywords: stars: binaries: close - stars: binaries: eclipsing -
stars: individual (BX Peg)
Abstract:
We presented BVRcIc light curves of BX Peg obtained by the Weihai
Observatory 1.0m telescope of Shandong University. The W-D code was
used to analyze the four color light curves, it is shown that BX Peg
is a W-subtype shallow contact binary with a fill-out factor of
f=14.6%. The asymmetric light curves were explained by a dark spot on
the less massive hot component. A total of 328 times of minimum light
were used to study the orbital period variation of BX Peg. We found
that the orbital period of BX Peg was continuous decrease with a rate
of dp/dt=-2.07x10^-7^d/yr superimposed on a cyclic oscillation
with a period of 57.8yr. The secular period decrease should be caused
by the angular momentum loss via magnetic stellar wind. The cyclic
modulation is very likely to be produced by the light travel time
effect due to a tertiary companion.
Description:
We monitored BX Peg using the Weihai Observatory 1.0-m telescope
(WHOT) of Shandong University on August 29th and September 9th, 2014.
WHOT is a classical Cassegrain telescope.
It has been about six years since the detailed study of the period
variation of BX Peg by Lee et al. (2009, Cat. J/PASP/121/1366). A lot
of times of minimum light have been obtained during these years. This
allows us to reanalyze the period change of BX Peg. By our new
determined times of minimum light and those collected from
literatures, a total of 328 times of minimum light which span about
88yr were used to analyze the period variation of BX Peg.
Objects:
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RA (2000) DE Designation(s)
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21 38 49.39 +26 41 34.2 BX Peg V* BX Peg
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