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IAUC 2811: N Sgr 1975; N Sct 1975; N Aql 1975; VV Cep

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IAUC number 

                                                  Circular No. 2811
Central Bureau for Astronomical Telegrams
INTERNATIONAL ASTRONOMICAL UNION
Postal Address: Central Bureau for Astronomical Telegrams
Smithsonian Astrophysical Observatory, Cambridge, MA 02138, U.S.A.
Cable Address: SATELLITES, NEWYORK
Western Union: RAPID SATELLITE CAMBMASS


NOVA SAGITTARII 1975
     The following magnitude estimates have been reported: July
23.17 UT, mpv = 10.5 (C. Scovil, Stamford Museum); 26.38, mv = 11.2
(K. Locher, Grut-Wetzikon, Switzerland; comparisons USNO 15244 V =
9.28 and USNO 15194 V = 11.07); 27.38, 11.4 (Locher); 28.90, 11.6
(Locher); 30.91, 12.2 (Locher); Aug. 2.09, m_pg = 13.2 (C. Y. Shao,
Harvard College Observatory).  Mr. Shao adds that there may be an
extremely faint image at the position of the nova on the blue print
of the Palomar Sky Survey.


NOVA SCUTI 1975
     Further selected visual magnitude estimates have been reported
as follows: July 19.20 UT, 9.7 (K. Simmons, Switzerland, Florida);
22.11, 9.4 (D. di Cicco, Waltham, Massachusetts); 23.16, 9.4 (di
Cicco); 25.18, 9.2 (C. Sherrod, North Little Rock, Arkansas); 27.16,
9.0 (Sherrod); 29.23, 9.5 (Sherrod); 31.25, 9.7 (Sherrod); Aug.
2.17, 10.1 (Sherrod); 3.09, 10.4 (Sherrod).


NOVA AQUILAE 1975
     J. E. Bortle, Brooks Observatory, provides the following visual
magnitude estimate of the "eruptive variable in Aquila": July
14.13 UT, 13.3.


VV CEPHEI
     Dr. K. O. Wright, Dominion Astrophysical Observatory, writes:
"Several high-dispersion (5 A/mm) plates of VV Cep taken at the 122-cm
coude spectrograph in the region 3250-4250 A in June and July
show important changes since 1974 in the strength and structure of
numerous lines.  In the 3600 A region the Sc II lines are now quite
strong, whereas in 1974 they were barely visible; the low-excitation
Ti II lines are also much stronger.  In addition there are now
sharp cores at the center of the strong Fe I lines, Ca I 4227 A and
Sr 4078 and 4216 A.  These observations indicate that the light from
the early-type secondary component is already being absorbed by the
outermost atmosphere of the supergiant M-type primary star even
though first contact is not predicted until Nov. 1976.  Similar
effects were observed during 1958 following the 1956-57 eclipse."


1975 August 5                  (2811)              Brian G. Marsden

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