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Four new BY Draconis variables found in the NSVS data
by Ivan Adamin, Alexandr Ditkovsky, Andrey Prokopovich, Valery Tsehmeystrenko in November-December 2013 (#3)
Abstract: As a part of VS-COMPAS data-mining program, in the paper four new rotating BY Draconis variables are presented. The research result on these objects is submitted to the VSX catalog for the first time by the VS-COMPAS team members. Photometric data from publicly available surveys (primarily, from the NSVS and CRTS) was used as a source for light curves.
The BY Draconis variables are rotating K and M dwarfs which exhibit low-amplitude photometric variability with typical periods of a few days. These variable stars have been of exceptional importance in the development of stellar surface activity under-standing and provided the important source of data to connect theory of spotted star's surface with rotation.
Resultant brightness fluctuations are generally less than 0.5 magnitudes. The first discovered BY Draconis variable is Ross 248 (HH Andromedae). Its variability was discovered by Gerald E. Kron in 1950. The variability of BY Draconis itself was discovered in 1966 and studied in detail by Chugainov in 1966 (Hall, 1994). The spectra of BY Dra variables are similar to RS CVn stars - another class of variable stars with active chromospheres. BY Draconis is a close binary consisting of a K6V dwarf and a M0V dwarf with an orbital period of 5.975 days and a mean separation of 0.05 AU.
Some of BY Draconis variables show flares, and are therefore UV Ceti stars (flare stars).
A model characterized by cooler, darker regions (starspots) on the surface of a rotating star appears to explain BY Draconis photometric variations (Kron, 1952; Torres and Ferraz Mello, 1973; Bopp and Evans, 1973; Vogt, 1975).
II. Candidates pre-selection and analysis
Candidates for analysis were selected by a custom piece of software created by I.Adamin. The software used the publicly available photometric databases, such as the Northern Sky Variability Survey (Woniak et al., 2004), zThe Catalina Real-time Transient Survey (Drake et al., 2012), as a source of photometric measurements.
Then, the whole set of candidates was distributed among the VS-COMPAS Project team members for further analysis. During this phase of research there was a custom period search and data analysis software used, created by combined efforts of A.Prokopovich and I.Adamin.
For high-precision periodogram calculation the Lafler-Kinman (Lafler, Kinman, 1965) statistical algorithm implementation was used. The VizieR web services were broadly used for obtaining data on the objects.
III. The list of discovered objects
We report the discovery of 4 new variables of BY Draconis type. These are: VSX J095115.5+220811, NSVS 352541, NSVS 6762026, NSVS 18711283. Below the results of this research are presented: a light curve for each object along with the name of its discoverer and light curve elements (cf. Table 1).
For NSVS 352541 (J-K = 0.79) magnitudes are contaminated by two neighbors: 2MASS J01353005+6910236 (J-K = 0.93, V = 14.35) 2MASS J01352603+6909398 (J-K = 0.36, V = 14.0). Thus, the range has been corrected for this object, taking into account photometric properties of its neighbors..
VSX J095115.5+220811 is particularly interesting for its short period, which is 0.636742 of a day. There are only 149 BY Draconis variables with period less than a day (out of 2633) in the VSX catalog at the moment of publication.
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- Samus, N. N.; Durlevich, O. V.; Kazarovets, E. V.; Kireeva, N. N.; Pastukhova, E. N.; Zharova, A. V. et al., 2007-2013, General Catalogue of Variable Stars, VizieR On-line Data Catalog, B/gcvs
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