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IAUC 3565: HD 58050; HONDA'S Var IN Cyg; 1980g

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                                                  Circular No. 3565
Central Bureau for Astronomical Telegrams
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

HD 58050
     D. Ballereau and A. M. Hubert, Observatoire de Paris, write:
"The Be star HO 58050, of spectral type B2V with stellar low-rotational
velocity v sin i = 140 km/s, is known to present strong Balmer
emission lines of variable intensity.  Spectra taken with the
Haute Provence 1.93- and 1.52-m telescopes (dispersions 0.967 and
1.244 x 10**-6) reveal a double Balmer emission centered on a wide
photospheric absorption.  Emission was visible up to H-12 from 1961
to 1966, with a maximum intensity in 1961.  During 1967-1968, there
was a minimum of emission, being visible only as far as H-epsilon.  The
emission was again strengthened and visible to H-11 in 1971 Jan.,
falling short of the 1961 intensity level.  From late 1971 to 1976,
emission was weaker but still visible to H-9 and fluctuating in intensity.
We have noted a new emission minimum, more significant
than that in 1968, on a plate taken on 1980 Nov. 24.  A faint
double emission feature was visible at H-beta on the wide photospheric
absorption, and H-gamma had a diffuse absorption.  Independently, J.
Busquets, J. Fabregat, L. Rivas, J. C. Misson and A. Figer, Groupe
Europeen d'Astronomes Amateurs, observed this star to brighten by
0.5 magnitude, from a mean value of 6.44 during 1979-1980 to 6.00
in 1980 Nov.-Dec.  The Balmer emission intensity decrease observed
in HD 58050 at the end of 1980 should be strongly correlated with
the increase in brightness."

     W. Wenzel, Sonneberg Observatory, telexes that H. Gessner
found this object on several hundred Sonneberg plates which indicate
it as a long-period variable with period just under 300 days.

     L. Rosino, Asiago Astrophysical Observatory, communicates:
"Spectra of Honda's variable in Cygnus were obtained on Jan. 11
with the Mount Ekar 1.82-m telescope by G. Massone.  They show that
the star is not a nova but very likely a Mira-type variable with
TiO absorption and sharp H emission."

     C. S. Morris, Harvard, MA, provides the following total visual
magnitude estimates and coma diameters from observations with a
0.25-m reflector: 1981 Jan. 6.10, 9.2, 2'; 9.07, 9.2, 1'.3.

1981 January 21                (3565)              Daniel W. E. Green

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