Central Bureau for Astronomical Telegrams
IAUC 3382: CP Pup; HR 8752 = HD 217476; alpha Mus AND chi Car
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Read IAUC 3383
Circular No. 3382
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
CP PUPPIS
K. Jensen, California Institute of Technology, reports that
soft x-ray emission in the region of the 1942 nova CP Pup has been
observed by the HEAO A-2 group. The observed flux in the 0.15-0.5
keV band is 8.9 +/- 1.8 x 10**-12 erg cm**-2 s**-1. There is no detectable
emission in the 0.5-2.0 keV band, but the group has determined a 2-signa
upper limit to the flux in this band to be 4.4 x 10**-12 erg cm**-2 s**-1.
CP Pup (R.A. = 8h09m.0, Decl. = -35o12', equinox 1950.0) is located in the
90-percent confidence region, which is centered at R.A. = 8h08m.1, Decl. =
-35o13'. A search of this region has revealed no other compelling
candidate for the source of emission. If CP Pup is the source, the
softness of the observed x-ray spectrum, combined with the large
expected interstellar absorption of soft x-rays, suggests a very
steep spectrum in the 0.15-2.0 keV band.
HR 8752 = HD 217476
J. Smolinski, J. L. Climenhaga and H. Funakawa, University of
Victoria; and M. Fletcher, Dominion Astrophysical Observatory,
communicate: "The spectrum of the very luminous supergiant HR 8752 is
undergoing considerable change. Inverse P-Cyg profiles were
observed in Fe I, Fe II and Ti II lines on spectra obtained at the
Dominion Astrophysical Observatory on May 24, June 29 and July 13.
The intensities of the emission lines appear to have increased
continuously during this time. Measurements give radial velocities
for these lines of ~ -85 km/s, almost the same as for the H-alpha
absorption line. Apparently these lines are formed in a shell which
is expanding at ~ 40 km/s relative to the photosphere."
alpha MUSCAE AND chi CARINAE
E. W. Elst, Royal Observatory at Uccie, writes: "Several early
B-type stars were observed in 1979 Feb. with the 61-cm photometric
telescope at the European Southern Observatory. From the observations
of alpha Mus and chi Car, the observed UBV short-period variations
appear to be caused by beta CMa-type variability. The color and spectral
type of alpha Mus and chi Car are typical for beta CMa-type stars, and
the observed light variation and calculated periods fit the normal
beta CMa variability ranges. The standstill phenomenon (Sareyan et al.
1975, Astron. Astrophys. 44, 215) is observed, and beat phenomena
are present in both stars."
1979 July 23 (3382) Daniel W. E. Green
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