Central Bureau for Astronomical Telegrams
IAUC 2245: N Ser 1970
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Circular No. 2245
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 SERPENTIS 1970
Dr. P. Tempesti, Collurania Observatory, Teramo, communicates
the following photoelectric observations, obtained with the 40-cm
refractor. Comparison stars were BD +3 3737 and +2 3604, with
assumed V magnitudes of 6.40 and 10.14, respectively. Mean
internal error + 0.01.
1970 UT V 1970 UT V 1970 UT V
Feb. 20.15 4.60 Mar. 20.16 6.02 Apr. 26.05 9.40
Mar. 7.16 5.44 Apr. 3.11 6.67 30.00 10.02
8.18 5.47 12.05 6.75 May 1.04 10.18
13.14 5.78 17.01 7.24 4.06 10.58
Dr. L. Rosino, Asiago Astrophysical Observatory, writes:
"Spectra of Nova Ser 1970 have been secured at Asiago Astrophysical
Observatory in the region 3600-11000 A by Drs. F. Ciatti and A.
Mammano since the maximum. In addition to the lines reported in
previous IAU Circulars, the following infrared emissions have been
detected using a Carnegie 51 intensifier, at 0.2 magnitude below
maximum: P6-P12, Ca II 8662-8542-8498 A, O I 7774 A, 8446 A, equally
intense and flanked by absorption components; some O I, N I and
possibly C I lines are also recorded. On April 29-30, when the
nova had undergone a faster decline, a spectrum obtained with the
prism-spectrograph at the Cassegrain focus of the 122-cm reflector
with a Carnegie S20 tube (dispersion 60 A/mm) shows saddle-shaped
emission lines split into two components whose separation gives a
velocity of about +/- 400 km/s. The strongest double lines, in order
of decreasing intensity, are: H-alpha, [0 I] 6300 A, [N II] 5755 A, H-beta,
[0 I] 6364 A, H-gamma, Fe II 4924 A, 5018 A, 5169 A, 5317 A, [O I] 5577 A,
Fe II 4584 A, [Fe II] 4410 A. Although in general the blue component is
much stronger than the red for most of the lines, some exceptions
are observed for H-beta and H-gamma and Na I 5893 A, which present components
of equal strength. It is apparent, from these preliminary observations,
that the emission shell approaching us somewhat veils the
receding shell (which gives rise to the redward components). The
Balmer decrement is very steep, and the lines in the blue region of
the spectrum are fainter than normal in comparison with the red-infrared
region. The infrared spectrum at about the same epoch is
dominated by O I 8446 A, while O I 7774 A has weakened. Paschen
lines from P6 to P9 are still present. [N I] 10395 A is growing."
1970 May 20 (2245) Brian G. Marsden
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