Nova Vulpeculae 1984 N 2 in 1985

Bergner, Yu. K.; Мирошниченко, А. С.; Yudin, R. V.; Yutanov, N. Yu.; Dzakusheva, K. G.; Ilyin, V. V.; Kuratov, K. S.; Mukanov, D. B.

doi:10.1007/bf00640466

Cited by 9 publications

(10 citation statements)

References 9 publications

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“…The optical data are taken from IAU Circular No. 4033, Kolotilov & Shenavrin (1988), Bergner et al (1988), Rosino et al (1992), and the AAVSO archive. The UV1455 Å data are compiled from the IUE Newly Extracted Spectra (INES) archive data sever 4 (see Cassatella et al 2002, for the UV1455 Å band).…”

Section: Quvul 1984#2mentioning

confidence: 99%

“…Figure 46 Figure 45. The data for QUVul are taken from Bergner et al (1988), Kolotilov & Shenavrin (1988), and Rosino et al (1992). The B−V colors of Rosino et al (1992) are systematically ∼0.2 mag bluer than those of Bergner et al (1988), so that we shifted them rightward (redward) by 0.2 mag.…”

Section: Wd Masses Of Neon Novaementioning

confidence: 99%

“…The data for QUVul are taken from Bergner et al (1988), Kolotilov & Shenavrin (1988), and Rosino et al (1992). The B−V colors of Rosino et al (1992) are systematically ∼0.2 mag bluer than those of Bergner et al (1988), so that we shifted them rightward (redward) by 0.2 mag. Although the color data of QUVul are scattered between the two groups, i.e., Bergner et al (1988) and Rosino et al (1992), the track of QUVul is close to those of V1500Cyg and V1974Cyg.…”

Section: Wd Masses Of Neon Novaementioning

confidence: 99%

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Light-Curve Analysis of Neon Novae

Hachisu

Kato

2015

ApJ

145

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We analyzed light curves of five neon novae, QUVul, V351Pup, V382Vel, V693CrA, and V1974Cyg, and determined their white dwarf (WD) masses and distance moduli on the basis of theoretical light curves composed of free-free and photospheric emission. For QUVul, we obtained a distance of d∼2.4 kpc, reddening of E (B−V)∼0. -M 1.1  . In QUVul, photospheric emission contributes 0.4-0.8 mag at most to the optical light curve compared with freefree emission only. In V351Pup and V1974Cyg, photospheric emission contributes very little (0.2-0.4 mag at most) to the optical light curve. In V382Vel and V693CrA, free-free emission dominates the continuum spectra, and photospheric emission does not contribute to the optical magnitudes. We also discuss the maximum magnitude versus rate of decline relation for these novae based on the universal decline law.

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Section: Quvul 1984#2mentioning

confidence: 99%

Section: Wd Masses Of Neon Novaementioning

confidence: 99%

Section: Wd Masses Of Neon Novaementioning

confidence: 99%

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Light-Curve Analysis of Neon Novae

Hachisu

Kato

2015

ApJ

145

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“…The UM/UW data taken through 28 August 1986 UT, previously reported piecemeal in Papers I and II, and by Greenhouse et al (1988), are collected in Table 1 for completeness of the photometric record. We have also included in Table 1 several very early IR measurements reported by British (Burton et al 1984) and Russian (Bergner et al 1984) observers in LAU Circulars No. 4024 and 4033.…”

Section: Observationsmentioning

confidence: 99%

The Neon Nova. III. The Infrared Light Curves of Nova QU Vulpeculae (Nova VUL 1984#2)

Gehrz¹,

Jones²,

Matthews³

et al. 1995

The Astronomical Journal

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We report 1.25 to 19.5 /¿m broadband infrared (IR) photometric measurements acquired during an eight year period on the prototypical ONeMg "neon nova" QU Vulpeculae (Nova Vul 1984 #2). The energy distribution of the ejecta evolved through several phases. An early free-free emission phase was followed by an IR coronal phase characterized by the appearance of strong emission lines from forbidden atomic transitions. The lines of [Ne Vi] at 7.6 /xm, and [Ne il] at 12.8 /¿m were especially strong during the coronal phase. A small amount of silicate dust condensed in the ejecta after about a year. The evidence provided by our IR observations for high abundances of metals in the ejecta of QU Vul is reviewed. We present the IR light curves of QU Vul, and show that the temporal development of its persistent IR coronal emission phase was evident in the broadband K (2.3 //m) andL (3.6 /¿m) photometry. Using data from our previous studies of classical novae, we suggest that K and L photometry can distinguish between the slower ONeMg novae with persistent IR coronal activity and CO novae that produce copious quantities of circumstellar dust. The most striking signature is produced in the L band, which contains emission from [Mg Vlll] at 3.02 /xm, [A1 Vi] at 3.66 /xm, and [Si ix] at 3.92 /xm. We comment on the peculiar tendency of the IR light curves of novae to decay exponentially.

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“…Here, we focus on VLBI observations towards V627 Cas, which emits both relatively strong H 2 O and SiO maser lines. V627 Cas is classified as a suspected D-type (dust-rich) symbiotic star (Belczyński et al 2000) characterized by thick dusty envelopes (Bergner et al 1988;Kolotilov et al 1991). The nature of the binary system including the companion separation and orbital period etc.…”

Section: Introductionmentioning

confidence: 99%

Asymmetric distributions of H2O and SiO masers towards V627 Cas

Yang,

Cho,

Yun

et al. 2020

Preprint

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We performed simultaneous observations of the H 2 O 6 1,6 − 5 2,3 (22.235080 GHz) and SiO v=1, 2, J=1→0, SiO v=1, J=2→1, 3→2 (43.122080, 42.820587, 86.243442, and 129.363359 GHz) masers toward the suspected D-type symbiotic star, V627 Cas, using the Korean VLBI Network (KVN). Here, we present astrometrically registered maps of the H 2 O and SiO v=1, 2, J=1→0, SiO v=1, J=2→1 masers for five epochs from Jan. 2016 to Jun. 2018. Distributions of the SiO maser spots do not show clear ringlike structures, and those of the H 2 O maser are biased towards the north-northwest to west with respect to the SiO maser features according to observational epochs. These asymmetric distributions of H 2 O and SiO masers are discussed based on two scenarios of a bipolar outflow and the presence of the hot companion, a white dwarf, in V627 Cas. We carried out ring fitting of SiO v=1, and v=2 masers and estimated the expected position of the cool red giant. The ring radii of the SiO v=1 maser are slightly larger than those of the SiO v=2 maser, as previously known. Our assumption for the physical size of the SiO maser ring of V627 Cas to be the typical size of a SiO maser ring radius (∼ 4 AU) of red giants yields the distance of V627 Cas to be ∼ 1 kpc.

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Nova Vulpeculae 1984 N 2 in 1985

Cited by 9 publications

References 9 publications

Light-Curve Analysis of Neon Novae

Light-Curve Analysis of Neon Novae

The Neon Nova. III. The Infrared Light Curves of Nova QU Vulpeculae (Nova VUL 1984#2)

Asymmetric distributions of H2O and SiO masers towards V627 Cas

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