COMMISSION 27 OF THE I. A. U. INFORMATION BULLETIN ON VARIABLE STARS Number 2606 Konkoly Observatory Budapest 16 October 1984 HU ISSN 0374 - 0676 H_alpha EMISSION IN RS CVn STARS: HD 8357, HD 175 742 AND HR 7428 Recently Hall et al.(1984) edited the "Hall Catalogue of RS CVn Binary Systems", in which twenty stars with H_alpha emission were reported. We observed 33 RS CVn stars i.n the H_alpha region using the coude Reticon system of the McDonald Observatory 2.1 m telescope. The dispersion is 9.5 A/mm and the resolution is 0.29 A. Three of these stars (HD 8357, HD 175742 and HR7428) showed conspicuous H_alpha emission. Physical data and observational details are listed in Table I. The individual systems are reported separately below. Table I ----------------------------------------------------------------- star sp mag. period obs. J.D.(H) phase ----------------------------------------------------------------- HD 8357 G5 7.28 - 2445957.8848 - composite 57.9428 - 58.8243 - 58.9799 - 59.8129 - 60.9638 - HD 175742 K0V 8.4 - 2445958.6146 - K5- M2V 58.6764 - 59.6153 - 60.5845 - HR 7428 A? 6.36 108.6 2445957.6288 0.4835 K2III-II 58.5794 0.4922 59.5774 0.5014 59.6711 0.5023 60.5669 0.5106 ------------------------------------------------------------------- HD 8357: The H_alpha profile changed significantly in both emission and absorption components as shown in Figure 1. The peak of emission fluctuated somewhat but was systematically shifted to the blue from the expected photospheric velocity by 0.6 A. The intensity of the strongest emission is 1.29 times of that of the continuum. The profile is similar to that of UX Ari. (Nations and Ramsey, 1980). [FIGURE 1] Figure 1. Variation of the Halpha emission feature of HD8357 [FIGURE 2] Figure 2. Variation of the Halpha emission of HD175742 HD 175 742: These H_alpha profiles are bizarre, and show extreme changes over three nights (Figure 2). The interval between the two observations on Sep. 15 was only 1.5 hours, but the two profiles are radically different, and the emission peak shifted from red to blue. The period of variation will be very short if the change is periodic. HR 7428 : HR7428 shows double emission, the red element being stronger than the blue one as shown in Figure 3, in which we only drew one plot since the profiles show little change in blue emission. This star was observed by Bopp et al. (1978), but they did not find H_alpha emission from two plates. Our observations were near phase 0.5. The H_alpha emission may be related to the phase, so more observations are needed. [FIGURE 3] Figure 3. H_alpha emission feature of HR7428 We are especially grateful to Dr. H. Smith for scheduling the telescope time. LIU XUEFU and TAN HUISONG McDonald Observatory The University of Texas (two visiting scholars from China) References: Bopp, B.W., and Talcott, J.C., 1978: A.J., 83, 1517. [BIBCODE 1978AJ.....83.1517B ] Hall, D.S., Zeilik, M., and Nelson, E.R., 1984: IBVS, No. 2458. Nations, H.L., and Ramsey, L.W., 1980: A.J., 85, 1086. [BIBCODE 1980AJ.....85.1086N ]