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[JCF 0.8Ka$,, 3lO, h 1f60M0Hh 2f60M0H,&87F$k+iG"kHra5lF$k.+7*ZdB AS1N~|f, 0.758HJCF$k,, 3N3HO}@*C-~|N&fkL+iO}rOq7$. 3N1N~|fO 0.713 G"kH$&Q,kLb"j, 3AiNMrQ$?&f@8b"k (19). 3N~|fO, p\M0Hh 1f60M0HN~|fH7FdjOJ$.3N=Khje2ilF$J$,, GaN@8Ghje2ilF$ksE~|1U'$IH7FO, 5|B Y1, 5|B EY1, 5|BGZ1,GSC 8691-1294 1, GSC 8607-0608 1JI,"k. 3liN1N~|fO 0.702 +i 0.708 NVG"k (20).dOObNsE~|1U'$IO, Q,,JaP, "k$O9GKy(ilF$kQ,kLNrO,JaP, bCHt,}(kKc$J$. =7F, Q,kL,}(kKDlF, 1N=$d, 1NbtG/-F$kaxN}r, =XH.JIKD$F, 77$N+r?(F/lkdj,+D+kG"m&HWolk. +7*ZdB TU1N, [o+HbWol?T,'J}wN/++iO^C?sE~|1U'$INdjO, #eb&f,31ilk3HG"m&.2M8%[1℄ Sanford, R. F., 1928: On the Variation of the Radial Veloity ofTU Cassiopeiae. Astrophys. J ., Vol. 68, p. 169[2℄ Worley, C. E., Eggen, O. J., 1957: The Peuliar Light Variation ofTU Cas. Astron. J ., Vol. 62, p. 104[3℄ Oosterho�, P. Th., 1957: The Light-Variation and the Radial-Veloity Curve of TU Cas Explained in Term of a Primary Periodand a Beat Period. Bull. Astron. Inst. Netherl., Vol. 13, p. 320[4℄ Oosterho�, P. Th., 1957: U Trianguli Australis, a Classial Cepheid14

with Seondary Period. Bull. Astron. Inst. Netherl., Vol. 13, p.317[5℄ Epstein, I., 1950: Pulsation Properties of Giant-Star Models.Astrophys. J ., Vol. 112, p. 6[6℄ Cox, J. P., King, D. S., Stellingwerf, R. F., 1972: Theoretial Pul-sation Constants and Cepheid Masses. Astrophys. J ., Vol. 171, p.93[7℄ Takeuti, M., 1958: The Masses of Pulsating Stars. Si. Rep. T ôhokuUniv., Ser. I, Vol. 42, p. 72[8℄ Rodgers, A. W., 1970: The Masses of Pulsating Stars. Mon. Not.Roy. Astron. So., Vol. 151, p. 133[9℄ Takeuti, M., 1973: On the Pulsation Masses of the ClassialCepheids. Publ. Astron. So. Japan, Vol. 25, p. 567[10℄ Cox, A. N., Hodson, S. W., Henden, A. A., King, D. S., 1977: TheMasse of AC Andromedae, U Triangli Australis, and BC Draonis.Astrophys. J ., Vol. 212, p. 451[11℄ Petersen, J. O., 1973: Masses of Double Mode Cepheid VariablesDetermined by Analysis of Period Ratios. Astron. Astrophys., Vol.27, p. 89[12℄ Efremov, Yu. N., Kholopov, P. N., 1975: Double Mode CepheidV367 St in Open Cluster NGC 6649. Inf . Bull. V ar. Stars, No.1073, p. 1[13℄ Kobayashi. E., Saio, H., Takeuti, M., 1976: The Mass of the Double-mode Cepheid V367 Suti. Si. Rep. T ôhoku Univ., Ser. I, Vol. 59,p. 67 15

[14℄ Petersen, J. O., Takeuti, M., 2001: A Historial Sketh of the BeatCepheids Studies. in Stellar Pulsation { Nonlinear Studies, eds.M. Takeuti, D. D. Sasselov, Astrophys. Spae Si. Library, Vol.257, p. 1[15℄ Simon, N. R., 1982: A Plea for Reexamining Heavy Element Opa-ities in Stars. Astrophys. J . (Letters), Vol. 260, L. 87[16℄ Moskalik, P., Buhler, J. R., Marom, A., 1992: Toward a Resolutionof the Bump and Beat Cepheid Mass Disrepany. Astrophys. J .,Vol. 385, p. 685[17℄ Alok, C., Allsman, R. A., Axelrod, T. S., et al., 1995: The MA-CHO Projet LMC Variable Star Inventory. I: Beat Cepheids - Con-lusive Evidene for the Exitation of the Seond Overtone in Clas-sial Cepheids. Astron. J ., Vol. 109, p. 1654[18℄ Soszynski, I., Udalski, A., Szymanski, M., et al., 2000: The Opti-al Gravitational Lensing Experiment. Cepheids in the MagellaniClouds. VI. Double-Mode Cepheids in the Large Magellani Cloud.Ata Astron., Vol. 50, p. 451[19℄ Pardo, I., Poretti, E., 1997: The Galati Double-mode Cepheids.I. Frequeny Analysis of the Light Curves and Comparison withSingle-mode Cepheids. Astron. Astrophys., Vol. 324, p. 121[20℄ Szil�adi, K., Vink�o, J., Poretti, E. et al., 2007: New HomogeneousIron Abundanes of Double-mode Cepheids from High-resolutionEhells Spetrosopy. Astron. Astrophys., Vol. 473, p. 57916

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