Central Bureau for Astronomical Telegrams
IAUC 3419: MV Sgr; beta Cyg; SS 433
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Read IAUC 3420
Circular No. 3419
Central Bureau for Astronomical Telegrams
INTERNATIONAL ASTRONOMICAL UNION
Postal Address: Central Bureau for Astronomical Telegrams
Smithsonian Astrophysical Observatory, Cambridge, MA 02138, U.S.A.
TWX 710-320-6842 ASTROGRAM CAM Telephone 617-864-5758
MV SAGITTARII
A. R. Landolt, Louisiana State University, reports that he
observed this R-CrB variable fainter than normal, at V = 15.18,
B-V = +0.87, U-B = +0.17, on Oct. 23.015 UT. Observations were
made with the 1.5-m telescope at Cerro Tololo.
beta CYGNI
C. E. Worley, U.S. Naval Observatory, informs us that his recent
observations of the brighter component of beta Cyg, long known to
exhibit a composite spectrum, now classified as K5II?+B?, confirm
that the component is itself double. Measurements with the 0.66-m
refractor on two nights at 1979.716 show the companion, ~ 1.5 mag
fainter than the primary, separated by 0".40 in p.a. 188o.2. He
confirms McAlister's (1979, Ap. J. 230, 497) reported resolution of
this pair by speckle interferometry with the Kitt Peak 4-m
reflector, in particular supporting the quadrant, which is ambiguous in
speckle observations.
SS 433
A. B. Giles, Astronomy Department, Leicester University, reports
that BVIJHK photometry by several teams at the 1.5-m infrared
flux collector on Tenerife, together with measurernents already
announced or from private communication of unpublished results,
provides a data base of up to 30 points per color over 213 days. The
observations have been folded at periods in the range 2-50 days,
and smooth J, H and K lightcurves result for a period P = 11.80 +/-
0.05 days. Each curve shows a long deep maximum (duration 0.65 P,
depth 1.3 mag at H), and the lowest point of the minimum defines
the ephemeris 1979 Aug. 14.26 (+/- 0.50) UT + 11.80E, in agreement
with the minimum of Kemp and Arbabi (IAUC 3391). A short secondary
minimum is probably also present. The maximum radial velocity
observed by Crampton et al. (IAUC 3388) on July 4.0 +/- 0.2 UT also
occurs at maximum light. The length of the minimum suggests an
eccentric orbit, which possibly accounts for the discrepancy with the
spectroscopic period of 13.0 +/- 0.1 days reported by Crampton et al.
The optical lightcurves appear less smooth than the infrared curves,
probably because of the 160-day period of the emission lines.
1979 October 30 (3419) Brian G. Marsden
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