We present photometric results for four new variable stars discovered in the vicinity of the ZZ Ceti-type pulsating white dwarf BR Cam. Observations were performed on 5 nights in November 2003 using the 1.8m telescope at Bohyunsan Optical Astronomy Observatory with no filter, on 3 nights in December 2003 using the 0.61m telescope at Sobaeksan Optical Astronomy Observatory with V, I filters, and on 3 nights in October 2004 using the 1.0m telescope at Mt. Lemmon Optical Astronomy Observatory with V, I filters. We estimated their periods from the phase-match technique for one eclipsing binary and the multiple frequency analysis for three pulsating stars. By considering the light curve shape, period and amplitude difference between two passbands, we classified the objects by their variability types as follows: V1 (USNO-A2.0 1425-05691757) is a W UMa-type eclipsing binary with an orbital period of 0d.4641; V2 (USNO-A2.0 1425-05703335) is a multi-periodic δ Sct-type pulsating star with a dominant period of 0d.0649; V3 (USNO-A2.0 1425-05699659) is also a δ Sct-type pulsating star with a period of 0d.1408; and V4 (USNO-A2.0 1425-05707705) is a RR Lyr-type pulsating star with a period of 0d.2643.

• S.-L. KIM(Korea Astronomy Observatory)
• C.-D. LEE(Korea Astronomy Observatory)
• J. W. LEE(Dept. of Astronomy and Space Science, Chungbuk National University)
• J. A. LEE(Korea Astronomy Observatory)
• Y.B. KANG(Korea Astronomy Observatory)
• J.-R. KOO(Korea Astronomy Observatory)
• G. VAUCLAIR(Universite Paul Sabatier, Observatoire Midi-Pyrenees)