Life after eruption – VI. Recovery of the old novae EL Aql, V606 Aql, V908 Oph, V1149 Sgr, V1583 Sgr and V3964 Sgr

Tappert, C.; Barría, Daniela; Morales, Irma Fuentes; Vogt, N.; Ederoclite, A.; Schmidtobreick, L.

doi:10.1093/mnras/stw1748

Cited by 12 publications

(13 citation statements)

References 41 publications

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“…

We found that the 1899 nova V606 Aql currently shows dwarf nova outbursts with a typical cycle length of 270 d and amplitudes of ∼1.5 mag using Public Data Release of Zwicky Transient Facility observations. The low mass-transfer rate in quiescence has been suggested to explain the large eruption amplitude (Tappert et al, 2016), and the present detection of dwarf nova outbursts supports this interpretation. The transition to the dwarf nova state more than 100 yr after the nova eruption gives credence to the hibernation scenario.

…”

supporting

confidence: 83%

V606 Aql (Nova Aquilae 1899) is now a dwarf nova

Kato,

Kojiguchi

2021

Preprint

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We found that the 1899 nova V606 Aql currently shows dwarf nova outbursts with a typical cycle length of 270 d and amplitudes of ∼1.5 mag using Public Data Release of Zwicky Transient Facility observations. The low mass-transfer rate in quiescence has been suggested to explain the large eruption amplitude (Tappert et al., 2016), and the present detection of dwarf nova outbursts supports this interpretation. The transition to the dwarf nova state more than 100 yr after the nova eruption gives credence to the hibernation scenario. The absolute magnitude estimated from dwarf nova outbursts suggests that V606 Aql should have been a fast nova and the presence of high excitation lines in quiescence would be explained by the presence of a massive white dwarf.

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“…

…”

supporting

confidence: 83%

V606 Aql (Nova Aquilae 1899) is now a dwarf nova

Kato,

Kojiguchi

2021

Preprint

View full text Add to dashboard Cite

We found that the 1899 nova V606 Aql currently shows dwarf nova outbursts with a typical cycle length of 270 d and amplitudes of ∼1.5 mag using Public Data Release of Zwicky Transient Facility observations. The low mass-transfer rate in quiescence has been suggested to explain the large eruption amplitude (Tappert et al., 2016), and the present detection of dwarf nova outbursts supports this interpretation. The transition to the dwarf nova state more than 100 yr after the nova eruption gives credence to the hibernation scenario. The absolute magnitude estimated from dwarf nova outbursts suggests that V606 Aql should have been a fast nova and the presence of high excitation lines in quiescence would be explained by the presence of a massive white dwarf.

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“…2. Spectroscopic confirmation of the CV: Identified candidates are confirmed as CVs by optical spectroscopy [21], [24], [25], [26] 3. Determination of the orbital period: Time resolved photometry or spectroscopy is performed on the brightest confirmed candidates with the aim to measure the orbital period [22], [23] For the most recent results, see the proceedings by Ederoclite et al in this conference.…”

Section: The Search For Old Novaementioning

confidence: 98%

The hunt for ancient novae

Schmidtobreick¹,

Tappert²,

Shara³

et al. 2018

Proceedings of the Golden Age of Cataclysmic Variables and Related Objects IV — PoS(GOLDEN 2017)

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“…Another question arises: Is the distribution of amplitudes in Figure real or biased by many unrecovered novae with amplitudes much larger than 13 mag? The total number of reported nova eruptions pre‐1986 amounts to 219 events (Downes et al ), while the histogram in Figure is based on the sample of the 93 confirmed postnovae (Tappert et al , and references therein). Thus, about 58% of the pre‐1986 novae are still unidentified.…”

Section: Are the Modern Counterparts Of Ancient Classical Novae Too Fmentioning

confidence: 99%

On the possibilities of classical nova identifications among historical Far Eastern guest star observations

2019

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More than 100 guest star observations have been obtained by Chinese, Korean, Japanese, and Vietnamese astronomers between ∼600 BCE and ∼1690 CE. Comparing the coordinates from the information given in old texts for eight supernova recoveries with modern supernova remnant positions, we estimate the typical positional accuracy of the order of 0.3–7° for these supernovae. These values could also be a start for the expected deviation angle between a classical nova observed as a guest star and its modern counterpart among known cataclysmic variables (CVs). However, there are considerable disagreements among modern authors regarding the interpretation of ancient Far Eastern texts, emphasizing the need to consult the original historic sources again in order to improve the positioning reliability. We also discuss the typical amplitudes of well‐observed classical novae and find that modern counterparts of nova guest stars should be V = 18 mag and thus easily observable. In this context, we also consider the “hibernation scenario” and conclude that it is impossible to decide from currently available observations whether hibernation is common. In addition to the limiting magnitude of around 2 mag for ancient guest star detections mentioned in the literature, we consider the possibility that fainter guest stars (4–5 mag) could also have been detected by ancient observers and provide arguments in favor of this possibility. For these limits, we compare the expected nova detection rate of ancient naked‐eye observers with that during modern times and conclude that they coincide in order of magnitude, which implies that, indeed, a considerable number of classical nova remnants should be hidden among the Far Eastern guest star reports. Finally, we present a statistical analysis of the probability of casual misidentifications based on frequency and Galactic distribution of CVs in the AAVSO‐Variable Star indeX catalog.

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Life after eruption – VI. Recovery of the old novae EL Aql, V606 Aql, V908 Oph, V1149 Sgr, V1583 Sgr and V3964 Sgr

Cited by 12 publications

References 41 publications

V606 Aql (Nova Aquilae 1899) is now a dwarf nova

V606 Aql (Nova Aquilae 1899) is now a dwarf nova

The hunt for ancient novae

On the possibilities of classical nova identifications among historical Far Eastern guest star observations

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