We report on 25 new variable stars (9 new eclipsing binary systems, 1 RR Lyrae star, 1 semi-regular variable and 14 miscellaneous long term variables), discovered during 4 months-long BVR monitoring of selected fields. The new variable stars are listed in Table below.

New variables
SAVS ID	Vmax	Amp	B-V	V-R	Period	Type
083716+412222 083726+424023 083828+414520 083958+413258 084002+274332 084041+423633 084136+371322 084146+390530 084416+250433 084612+365443 084626+343636 084828+414312 085055+305604 085444+415515 085609+345207 090002+273928 090144+421931 090552+441934 121315+301307 122025+415629 125417+282700 130753+233728 131008+243602 131314+271523 131845+254731	10.01 10.94 10.56 11.94 12.08 12.81 8.69 11.36 10.23 10.23 11.72 10.51 10.63 11.02 11.69 11.83 12.46 11.30 10.59 10.19 9.28 9.92 9.66 10.10 10.04	0.75 0.46 0.64 0.26 0.69 0.76 0.53 0.33 0.49 0.63 0.34 0.25 0.46 0.35 0.52 0.54 0.44 0.34 0.25 0.70 0.21 0.63 0.52 0.22 0.52	0.53 0.54 1.72 1.07 0.36 - 1.79 0.86 0.58 2.10 0.32 1.75 1.70 0.62 1.75 0.44 - 1.74 0.51 1.62 1.41 1.62 0.67 1.28 1.42	0.43 0.46 1.49 0.81 0.46 1.24 1.54 0.71 0.51 1.81 0.42 1.32 1.27 0.47 1.74 0.38 0.58 1.50 0.50 1.25 1.47 1.95 2.17 1.00 1.47	1.81 0.63 - - 0.50 - - 0.36 3.40 - 0.57 - - 0.54 - 0.67 0.39 - 0.31 - - - 69.4 - -	EA EW MISC MISC RRAB MISC MISC EW EA MISC EW MISC MISC EB MISC EW EW MISC EB MISC MISC MISC SR MISC MISC
SAVS ID - identifier consisted of Right Ascension and Declination of a star calculated for J2000.0. Other ID - cross-identification with other catalogs. Vmax - max brightness in V band. Amp - amplitude of variation in V. B-V and V-R - mean color indexes. Period - period of variability in days. Type - type of variability in GCVS convention.

In search for color variation in new variables we studied correlation between V and color indexes B-V and V-R for every new variable. We selected those stars for which the correlation coefficient |r|>0.5 in at least one color index as stars showing color variations. Due to large scatter in B no detectable variability of B-V was found for any star. In the next step the V-R color curves of such preselected variables were inspected visually. 7 of them, that passed that inspection, are displayed in Figure below. All but one stars are late spectral type, red semi-regular or irregular variables.

To illustrate the shape and amplitude of V-R variations we fitted either first or second order polynomials and sinusoid for red variables and the EW system, respectively. As expected the color variations of red variables are correlated with brightness, what indicates pulsating nature of the variability. The only eclipsing system in our sample revealing color variation, SAVS 090002+273928, becomes more red during eclipses.

The light curves of 18 variables revealing no detectable color changes are shown in figure below, where only V data are plotted.

The original photometric data and individual light curve graphs are available in the New Variables section.