On nova Scorpii 2007 N.1 (V1280 Sco)

Kuncarayakti, H.; Kristyowati, Desima; Kunjaya, Chatief

doi:10.1007/s10509-008-9756-0

Cited by 4 publications

(5 citation statements)

References 12 publications

(6 reference statements)

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“…Large post maximum oscillations have been previously observed in the novae V2540 Oph (Kato et al 2002), V1178 Sco (Kato and Mitsugu 2001), V4361 Sgr (Kato and Mitsugu 2001), V2214 Oph (Lynch et al 1989), V868 Cen (Williams et al 2003). This behavior is markedly different from the dips and returning to decline curve shown by dust forming novae, such as V1280 Sco (Kuncarayakti et al 2008).…”

Section: Photometrycontrasting

confidence: 62%

The early spectroscopic evolution of nova V458 Vul (Nova Vulpeculae 2007)

Poggiani

2008

Astrophys Space Sci

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The early spectral evolution of the nova V458 Vul has been monitored at the Loiano Observatory, Italy. The nova exhibited a couple of oscillations during the decline from initial maximum. We have performed spectroscopic observations to study the physical properties of the ejected material. The photometric light curve has been used to derive the nova distance and its absolute magnitude at maximum. V458 Vul is a fast nova, with decline rates by two or three magnitudes of 7 and 15 days respectively. The magnitude at maximum is M V = −8.8. The nova distance is in the range 6.7-10.3 kpc. The spectra secured a few days after initial maximum showed emission lines of H I and Fe II, making V458 Vul a Fe II nova at this stage. After the oscillations V458 Vul came back to a standard decline curve, but evolved towards the He/N class. Thus V458 Vul is a hybrid nova.

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Section: Photometrycontrasting

confidence: 62%

The early spectroscopic evolution of nova V458 Vul (Nova Vulpeculae 2007)

Poggiani

2008

Astrophys Space Sci

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“…There are very few novae for which the spectral evolution before the maximum brightness has been documented, e.g. V1280 Sco (Kuncarayakti, Kristyowati & Kunjaya ; Naito et al ) and V2615 Oph (Munari et al ). The spectral evolution of V496 Sct during the pre‐maximum, maximum and optically thick branch of the decline phase is presented in Fig.…”

Section: Resultsmentioning

confidence: 99%

“…The optical spectra presented here cover the pre-maximum rise, the optical maximum brightness, the early decline and the nebular phase. There are very few novae for which the spectral evolution before the maximum brightness has been documented: V1280 Sco (Naito et al 2012, Kuncarayakti et al 2008) and V2615 Oph (Munari et al 2008). The spectral evolution of V496 Sct during the pre-maximum, maximum and optically thick branch of the decline phase is presented in Fig.…”

Section: Line Identification Evolution and General Characteristics Of...mentioning

confidence: 99%

V496 Scuti: an Fe ii nova with dust shell accompanied by CO emission

Raj

Ashok

Banerjee

et al. 2012

Monthly Notices of the Royal Astronomical Society

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We present near‐infrared (near‐IR) and optical observations of the nova Scuti 2009 (V496 Sct) covering various phases – pre‐maximum, early decline and nebular – during the first 10 months of its discovery followed by limited observations in the early part of 2011 April. The spectra follow the evolution of the nova when the lines had strong P Cygni profiles to a phase dominated by prominent emission lines. The notable feature of the near‐IR spectra in the early decline phase is the rare presence of first overtone bands of carbon monoxide in emission. Later about 150 days after the peak brightness, the IR spectra show clear dust formation in the expanding ejecta. Dust formation in V496 Sct is consistent with the presence of lines of elements with low ionization potentials like Na and Mg in the early spectra and the detection of CO bands in emission. The light curve shows a slow rise to the maximum and a slow decline indicating a prolonged mass loss. This is corroborated by the strengthening of P Cygni profiles during the first 30 days. In the spectra taken close to the optical maximum brightness, the broad and single absorption components seen at the time of discovery are replaced by two sharper components. During the early decline phase, two sharp dips that show increasing outflow velocities are seen in the P Cygni absorption components of Fe ii and H i lines. The spectra in 2010 March showed the onset of the nebular phase. Several emission lines display saddle‐like profiles during the nebular phase. In the nebular stage, the observed fluxes of [O iii] and Hβ lines are used to estimate the electron number densities and the mass of the ejecta. The optical spectra show that the nova is evolved in the PfeAo spectral sequence. The physical conditions in the ejecta are estimated. The absolute magnitude and the distance to the nova are estimated to be MV = −7.0 ± 0.2 and d = 2.9 ± 0.3 kpc, respectively.

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“…Its early spectra were taken by some observers (e.g. Naito & Narusawa 2007, Kuncarayakti et al 2008) and it was classified as an Fe ii type nova ). Yamaoka et al (2007c) reported that the spectrum at the pre-maximum stage looked like that of an F-type supergiant dominated by absorption lines of hydrogen, Fe ii and other metals.…”

Section: Introductionmentioning

confidence: 99%

Five-year optical and near-infrared observations of the extremely slow nova V1280 Scorpii

Naito

Mizoguchi

Arai

et al. 2012

A&A

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We present optical (B, V, R c , I c and y) and near-infrared (J, H, and K s ) photometric and spectroscopic observations of a classical nova V1280 Scorpii for five years from 2007 to 2011. Our photometric observations show a declining event in optical bands shortly after the maximum light, which took about 250 days to recover. This event was most probably caused by dust formation. The event was accompanied by a short (∼30 days) re-brightening episode (∼2.5 mag in V), which suggests that there had been some re-ignition of the surface nuclear burning. After 2008, the y band observations show a very long plateau at around y = 10.5 for more than 1000 days until April 2011 (∼1500 days after the maximum light). The nova had taken a very long time (∼50 months) to enter the nebular phase, according to a clear detection of both [O iii] 4959 and 5007 and is still continuing to generate the wind caused by H-burning.This finding suggests that historically V1280 Sco is evolving at its slowest ever measured rate. The interval from the maximum light (2007 February 16) to the beginning of the nebular phase is longer than any previously known slow novae: V723 Cas (18 months), RR Pic (10 months), or HR Del (8 months). It suggests that the mass of a white dwarf in the V1280 Sco system might be 0.6 M or lower. The distance, based on our measurements of the expansion velocity combined with the directly measured size of the dust shell, is estimated to be 1.1 ± 0.5 kpc.

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On nova Scorpii 2007 N.1 (V1280 Sco)

Cited by 4 publications

References 12 publications

The early spectroscopic evolution of nova V458 Vul (Nova Vulpeculae 2007)

The early spectroscopic evolution of nova V458 Vul (Nova Vulpeculae 2007)

V496 Scuti: an Fe ii nova with dust shell accompanied by CO emission

Five-year optical and near-infrared observations of the extremely slow nova V1280 Scorpii

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