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Iue Observations of the Two Peculiar Binary Systems Beta Lyrae and Upsilon Sagittarii+

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Iue Observations of the Two Peculiar Binary Systems Beta Lyrae and Upsilon Sagittarii+ IUE OBSERVATIONS OF THE TWO PECULIAR BINARY SYSTEMS BETA LYRAE AND UPSILON SAGITTARII+ Margherita Hack, Umberto Flora, Paolo Santin Astronomical Observatory, Trieste, Italy The common peculiarities of these two systems are: a) the companion is a massive object (probably m2>10 ) whose spectrum is not observable; b) both systems show evidence, though in different degrees, of mass-transfer and mass-loss; c) both present, in different degrees, hydrogen deficiency; d) ultraviolet observations have shown, in both cases, the presence of lines of highly ionized elements like N V, C IV, Si IV, probably formed in an extended envelope because they do not show orbital radial velocity shifts, and cannot be explained by the effective temperature of the star whose spectrum we observe. The latter property seems to be common to several close binaries, as shown by the ultra­ violet observations with IUE by Plavec and Koch (1979); e) both systems present infrared excess, suggesting the presence of an extended envelope (Gehrz et al. 1974; Lee and Nariai, 1967; Humphreys and Ney, 1974; Treffers et al. 1976) . The main characteristics of the two systems are summarized in Table 1. The IUE observations and their purpose. Although Beta Lyrae had been observed very extensively with Copernicus (Hack et al. 1975, 1976, 1977) a few problems were left, because the spectral region 1500-2000 A, where the sensitivity of the spectrometer was extremely low, had not been observed. In this region are located two lines,X 1640 He II and \ 1908 C IIIJ , which are impor­ tant for deriving the physical conditions of the envelope. During the first run of observations of Beta Lyrae with Copernicus, it was a sur­ prise to observe the strong emission of the resonance lines of N V and + Based on observations by the International Ultraviolet Observer (IUE) collected at the Villafranca Satellite Tracking Station of the European Space Agency. 271 M. J. Plavec, D. M. Popper and R. K. Ulrich (eds.), Close Binary Stars: Observations and Interpretation, 271-286. Copyright © 1980 by the IAU. Downloaded from https://www.cambridge.org/core. IP address: 43.130.79.121, on 06 Oct 2021 at 14:55:33, subject to the Cambridge Core terms of use, available at https://www.cambridge.org/core/terms. https://doi.org/10.1017/S0074180900065001 272 M. HACK ET AL. the apparent absence of ^1085 He II (blended with the resonance lines of N II). A confirmation of the weakness or absence of He II was given by low resolution spectra obtained with an objective prism spectrograph on Skylab by Kondo et al. (1976), and its complete absence was confirmed by IUE observations. This result suggested that the far UV emission lines are not radiatively but collisionally excited. Table 1 - Properties of the systems P Lyr ^ Sgr p (d) 12.9349 137.9567 f(m) (•) 8.73 1.677 K (Km s"1) 184.0 49.12 (Km s-1) -17.8 -13.29 r 6 7 a sin:L(Km ) 32.7xl0 9.3X10 i (°) £75° 47° Sp .Prim. B8-B9 B8,F0 la H/He 1/2 1/40 m m l/ 2 (i=90°) 1/1., 6 11^ = 14 m2 ==21 .. 4 M M 1/6 1.6 11,. 8 m^/m^ (i=47°) 1/2 m1=4.8 m2=9,.6 4 H ti 1 17.1 17,. 1 tl t» 2 38.6 19,. 3 Probabl. e type sec. B0-B5 Ill--IV or 09 V Black Hole The existence of strong emission in the region 1900-2100 A was shown by the low resolution observations obtained by Hack (1974) with experiment S2/68 on TD-1 and by Kondo et al. (1976) with Skylab. Hack attributed these emissions mainly to the strong Fe III lines present in this region. However, a possible contribution could be due to \l908 C III] whose emission is strong in several Wolf-Rayet stars, symbiotic stars, and chromospheric spectra of late-type stars. This line requires a gas density of 1010 cm"3 or less (Osterbrok, 1970). Now the IUE obser­ vations have excluded its presence, putting the lower limit for the density of the envelope above 1010 cm~3. Upsilon Sgr was also observed with Copernicus, but only in two limited spectral regions (Duvignau et al. 1979) and with very low S/N. The present observations cover the epochs of the two minima and the two quadratures in the spectral range 1170-3200 A. Table 2 gives the list of the observations. All the exposures were obtained with the 3" aperture. Downloaded from https://www.cambridge.org/core. IP address: 43.130.79.121, on 06 Oct 2021 at 14:55:33, subject to the Cambridge Core terms of use, available at https://www.cambridge.org/core/terms. https://doi.org/10.1017/S0074180900065001 IUE OBSERVATIONS OF (3 LYRAE AND v SAGITTARII 273 1384.00 1386.00 1388.00 1390.00 1392.00 1394.00 1396.00 139R.00 niOO.OO 1402.00 1404.00 1406.00 m08.01 14 LAMBDA (ANGSTROM) Figure 1. The profiles of the Si IV resonance lines. Top: Beta Lyr (phase 0.51); bottom: Upsilon Sgr (phase-0.02). Downloaded from https://www.cambridge.org/core. 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