UBVRI photometry of Nova Cygni 1975

Marcocci, M.; Messi, R.; Natali, G.; Rossi, L.

doi:10.1038/259186a0

Cited by 3 publications

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“…The 0 -C computed for the times of Table 3 with the elements derived by SEMENIUK et al (1977) fit fairly well their 0 -C curve conveniently extrapolated. The error in the period caused by the uncertainty in the data of the light extrema of Table 3 The perequated lightcurve, reported in Figure 2, shows, besides the 3.3-hour oscillation, fluctuations on a time scale of half an hour having the amplitude of about 0.10 mag; the presence of spikes and hollowness in the 3.3-hour light variation had already been observed in some cycles (MARCOCCI et al 1976;PROKOFIEVA and ABRAMENKO 1976;SEMENIUK 1975;YOUNG et al 1977), nevertheless the reality of the modulation appearing in Figure 2 may be questioned, especially considering that the brightness of the nova was rather close to the limit of the telescope power. Unfortunately no suitable check star could be used thoroughly along the night run; however a plot of the measures on the comparison star (see Figure 2) shows no fluctuations greater than 0.02 mag and there appears only the steady decline caused by the increasing of the zenithal distance; the constancy of this star has been moreover tested by WILLIAMON (1977).…”

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confidence: 90%

“…The period appears anyhow to have progressively shortened from od141o to od138o & 0.0002 in the first 15 months after the nova outburst. The presence of secondary waves gives little significance to the different shape of the two maxima observed on Decembre 13, 1976, as regards the (MARCOCCI et al 1976;PROKOFIEVA and ABRAMENKO 1976;SEMENIUK 1975;YOUNG et al 1977), nevertheless the reality of the modulation appearing in Figure 2 may be questioned, especially considering that the brightness of the nova was rather close to the limit of the telescope power. Unfortunately no suitable check star could be used thoroughly along the night run; however a plot of the measures on the comparison star (see Figure 2) shows no fluctuations greater than 0.02 mag and there appears only the steady decline caused by the increasing of the zenithal distance; the constancy of this star has been moreover tested by WILLIAMON (1977).…”

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confidence: 98%

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The lightcurve of nova cygni 1975 (V 1500 Cyg) from the outburst to July 1977

Tempesti

1979

Astron Nachr

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On the basis of photoelectric observations performed at the Teramo Observatory, the V lightcurve of Nova Cygni 1975 from August 1975 to July 1977 is given. Since three days after maximum thereafter, the decline pursued smoothly according the law V = 2.5 + 3.9 lg t, and 680 days after maximum the star had weakened by 12.5 mag. The well-known shortperiod light variation, which at the time of the early decline showed an amplitude smaller than 0.2 mag in V light, on December 13, 1976, displayed an amplitude as high as 0.5 mag. Table I, have been utilized; owing to the well known strong discordance generally found between the magnitudes obtained for a nova in the nebular stage by means of equipments differing even slightly in colour response, from September 5, 1975, thereafter only the Teramo observations have been considered. The equipment, an E M 1 9502 photomultiplier with 2-mm Schott GG14 + GG13 filter combination, is the same employed for the already published observations of the nova (ROSINO and TEMPESTI 1977) and the same comparison star, BD +48"3340 with assumed V magnitude 84143, was used throughout for the new observations here presented in Tables I and 2 .

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confidence: 90%

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confidence: 98%

The lightcurve of nova cygni 1975 (V 1500 Cyg) from the outburst to July 1977

Tempesti

1979

Astron Nachr

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“…In 8 < (t-t 0 ) < 16 the mean period was P = 0.2820 ± 0^0001 followed by a decrease, the precise nature of which is dependent upon the phasing of the Marcocci et al, 1975Marcocci et al, . 1975 October 27, November 9, 10 points.…”

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confidence: 99%

Periodicities and rapid line variability in nova V1500 Cygni 1975

Young¹,

Robinson²,

Africano³

et al. 1977

PASP

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We analyze photoelectric Johnson V and Strömgren y observations of nova Cygni over the interval 1975 September 8 to November 10 for evidence of periodicities in the observed light maxima and minima. The periods deduced are P = 0.2820 ± 0^0001 for 1975 September 8-15 followed by a change to ? -0.2792 ± 0^0001 over the interval 1975 September 25-November 10. The light curve is double humped with distinguishable minima which change in form over the time covered by the observations. In addition we use spectroscopic observations of the Hß and [O in] lines to investigate the possibility of rap id-line variability. We conclude that these variations were due to fluctuations in the continuum rather than the line fluxes.

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Observations de Nova Cygni 1975 (V 1500 Cyg)

Andrillat

1977

Novae and Related Stars

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UBVRI photometry of Nova Cygni 1975

Cited by 3 publications

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The lightcurve of nova cygni 1975 (V 1500 Cyg) from the outburst to July 1977

The lightcurve of nova cygni 1975 (V 1500 Cyg) from the outburst to July 1977

Periodicities and rapid line variability in nova V1500 Cygni 1975

Observations de Nova Cygni 1975 (V 1500 Cyg)

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