A search for cool molecular gas in GK Persei and other classical novae

Kamiński, T.; Mazurek, H.; Menten, K. M.; Tylenda, R.

doi:10.1051/0004-6361/202142737

Cited by 4 publications

(2 citation statements)

References 65 publications

(79 reference statements)

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“…In addition, CK Vul, along with V4332 Sgr, V838 Mon, and V1309 Sco, all lie at the centers of cool, compact molecular nebulae, which are prominent at millimeter wavelengths (Kamiński et al 2018(Kamiński et al , 2021a. Kamiński et al (2022) attempted to detect CO emission from V1148 Sgr with the Atacama Pathfinder Experiment (APEX) 12-m submillimeter telescope, with unsuccessful results. Unfortunately, they pointed at the Duerbeck position discussed in §2.…”

Section: Was V1148 Sgr a Luminous Red Nova?mentioning

confidence: 99%

Nova Sagittarii 1943 (V1148 Sgr): A Luminous Red Nova?

Bond,

Mink,

Doane

et al. 2022

Preprint

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Nova Sagittarii 1943 (V1148 Sgr) was an 8th-mag optical transient that was unusual in having a late-type spectrum during its outburst, in striking contrast to the normal high-excitation spectra seen in classical novae. Unfortunately, only an approximate position was given in the discovery announcement, hampering follow-up attempts to observe its remnant. We have identified the nova on two photographic plates in the Harvard archive, allowing us to determine a precise astrometric position. Apart from these two plates, obtained in 1943 and 1944, none of the photographs in the Harvard collection, from 1897 to 1950, show V1148 Sgr to limits as faint as g 18.3. Modern deep images show a candidate remnant at i 19.2, lying only 0. 26 from the site of the nova. V1148 Sgr may have been a luminous red nova (LRN), only the sixth one known in the Milky Way. However, it lacks the near-and mid-infrared excesses, and millimeter-wave emission, seen in other LRNe, leaving its nature uncertain. We urge spectroscopy of the candidate remnant.

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Section: Was V1148 Sgr a Luminous Red Nova?mentioning

confidence: 99%

Nova Sagittarii 1943 (V1148 Sgr): A Luminous Red Nova?

Bond,

Mink,

Doane

et al. 2022

Preprint

View full text Add to dashboard Cite

show abstract

“…In addition, CK Vul, along with V4332 Sgr, V838 Mon, and V1309 Sco, all lie at the centers of cool, compact molecular nebulae, which are prominent at millimeter wavelengths (Kamiński et al 2018(Kamiński et al , 2021a(Kamiński et al , 2021b. Kamiński et al (2022) attempted to detect CO emission from V1148 Sgr with the Atacama Pathfinder Experiment (APEX) 12 m submillimeter telescope, with unsuccessful results. Unfortunately, they pointed at the Duerbeck position discussed in Section 2.…”

Section: Was V1148 Sgr a Luminous Red Nova?mentioning

confidence: 99%

Nova Sagittarii 1943 (V1148 Sgr): A Luminous Red Nova?

Bond

Mink

Doane

et al. 2022

View full text Add to dashboard Cite

Nova Sagittarii 1943 (V1148 Sgr) was an eighth magnitude optical transient that was unusual in having a late-type spectrum during its outburst, in striking contrast to the normal high-excitation spectra seen in classical novae. Unfortunately, only an approximate position was given in the discovery announcement, hampering follow-up attempts to observe its remnant. We have identified the nova on two photographic plates in the Harvard archive, allowing us to determine a precise astrometric position. Apart from these two plates, obtained in 1943 and 1944, none of the photographs in the Harvard collection, from 1897 to 1950, show V1148 Sgr to limits as faint as g ≃ 18.3. Modern deep images show a candidate remnant at i ≃ 19.2, lying only 0.″26 from the site of the nova. V1148 Sgr may have been a luminous red nova (LRN), only the sixth one known in the Milky Way. However, it lacks the near- and mid-infrared excesses, and millimeter-wave emission, seen in other LRNe, leaving its nature uncertain. We urge spectroscopy of the candidate remnant.

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Lithium in red novae and their remnants

Kamiński¹,

Schmidt²,

Hajduk³

et al. 2023

A&A

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Context. Galactic red novae are thought to be produced in stellar mergers between non-compact stars, such as main-sequence stars and cool giants. It is hoped that they will help explain the physical processes involved in common-envelope evolution and stellar binary collisions. Aims. We investigate the presence of lithium in the three best observed Galactic red nova remnants. Explaining the origin of lithium may point to a mixing mechanism present before, during, or after the merger. Methods. We compared the lithium line at 6707.81 Å to a feature of Ca I] at 6572.78 Å to derive relative abundances in circumstellar gas. We next calculated absolute abundances, assuming the solar calcium-to-lithium abundance ratio. Results. Our analysis yields the following lithium abundances: A(Li) = 2.3 for V838 Mon, A(Li) = 2.5 for CK Vul, and A(Li) = 1.8 for V1309 Sco. Conclusions. The super-solar lithium abundances in red novae may suggest that at least some merger products activate mixing mechanisms capable of producing lithium, but other interpretations are possible. In particular, the merger product of V838 Mon may be enhanced in lithium by the matter of one of the progenitor stars. Early observations of lithium in V838 Mon and V1309 Sco hint that Li-producing mechanisms, if present, activate early, perhaps already in the common-envelope phase. Determining the origin of lithium in red novae requires further investigation and a larger sample of measured stars.

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A search for cool molecular gas in GK Persei and other classical novae

Cited by 4 publications

References 65 publications

Nova Sagittarii 1943 (V1148 Sgr): A Luminous Red Nova?

Nova Sagittarii 1943 (V1148 Sgr): A Luminous Red Nova?

Nova Sagittarii 1943 (V1148 Sgr): A Luminous Red Nova?

Lithium in red novae and their remnants

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