Nova Ophiuchus 2017 as a Probe of 13C Nucleosynthesis and Carbon Monoxide Formation and Destruction in Classical Novae

Joshi, Vishal; Banerjee, D. P. K.; Srivastava, Mudit

doi:10.3847/2041-8213/aa9d86

Cited by 9 publications

(7 citation statements)

References 24 publications

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“…We have estimated the CO mass in SN 2020oi using the LTE model developed by Das et al (2009), which assumes optically thin emission and a pure 12 C 16 O composition. Earlier applications of the model include SN 2017eaw (Rho et al 2018a), SN 2016adj (Banerjee et al 2018), and several novae (Banerjee et al 2016;Joshi et al 2017). We adopted a straight continuum (for the dust emission) passing through the two minima (2.01-2.08 μm and 2.155-2.17 μm) in the spectrum between 2.00 and 2.23 μm.…”

Section: Co and Dust Formation In Type Ic Sn 2020oimentioning

confidence: 99%

Near-infrared and Optical Observations of Type Ic SN 2020oi and Broad-lined Type Ic SN 2020bvc: Carbon Monoxide, Dust, and High-velocity Supernova Ejecta

Rho

Evans

Geballe

et al. 2021

ApJ

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We present near-IR (NIR) and optical observations of the Type Ic supernova (SN Ic) SN 2020oi in the galaxy M100 and the broad-lined SN Ic SN 2020bvc in UGC 9379, using Gemini, Las Cumbres Observatory, Southern Astrophysical Telescope, and other ground-based telescopes. The NIR spectrum of SN 2020oi at day 63 since the explosion shows strong CO emissions and a rising K-band continuum, which is the first unambiguous dust detection from an SN Ic. Non-LTE CO modeling shows that CO is still optically thick and that the lower limit to the CO mass is 10 −3 M e. The dust temperature is 810 K, and the dust mass is ∼10 −5 M e. We explore the possibilities that the dust is freshly formed in the ejecta, heated dust in the preexisting circumstellar medium, and an infrared echo. The light curves of SN 2020oi are consistent with a STELLA model with canonical explosion energy, 0.07 M e Ni mass, and 0.7 M e ejecta mass. A model of high explosion energy of 10 52 erg, 0.4 M e Ni mass, and 6.5 M e ejecta mass with the circumstellar matter reproduces the double-peaked light curves of SN 2020bvc. We observe temporal changes of absorption features of the IR Ca II triplet, S I at 1.043 μm, and Fe II at 5169 Å. The blueshifted lines indicate high velocities, up to 60,000 km s −1 for SN 2020bvc and 20,000 km s −1 for SN 2020oi, and the expansion velocity rapidly declines before the optical maximum. We present modeled spectral signatures and diagnostics of CO and SiO molecular bands between 1.4 and 10 μm.

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Section: Co and Dust Formation In Type Ic Sn 2020oimentioning

confidence: 99%

Near-infrared and Optical Observations of Type Ic SN 2020oi and Broad-lined Type Ic SN 2020bvc: Carbon Monoxide, Dust, and High-velocity Supernova Ejecta

Rho

Evans

Geballe

et al. 2021

ApJ

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“…We have estimated the CO mass in SN2020oi using the LTE model developed by Das et al (2009), which assumes optically thin emission and a pure 12 C 16 O composition. Earlier applications of the model include SN2017eaw (Rho et al 2018a), SN2016adj (Banerjee et al 2018) and several novae (Banerjee et al 2016;Joshi et al 2017). The best fit model, shown in Figure 8, was determined by varying the CO mass, temperature, and velocity dispersion using chi-square minimization over the region 2.27 to 2.44 µm.…”

Section: Optical and Near-ir Spectroscopy Of Sn Ic And Ic-blmentioning

confidence: 99%

Near-Infrared and Optical Observations of Type Ic SN2020oi and broad-lined Ic SN2020bvc: Carbon Monoxide, Dust and High-Velocity Supernova Ejecta

Rho,

Evans,

Geballe

et al. 2020

Preprint

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We present near-infrared and optical observations of the Type Ic Supernova (SN) 2020oi in the galaxy M100 and the broad-lined Type Ic SN2020bvc in UGC 9379, using Gemini, LCO, SOAR, and other ground-based telescopes. The near-IR spectrum of SN2020oi at day 63 since the explosion shows strong CO emissions and a rising K-band continuum, which is the first unambiguous dust detection from a Type Ic SN. Non-LTE CO modeling shows that CO is still optically thick, and that the lower limit to the CO mass is 10 −3 M . The dust temperature is 810 K, and the dust mass is ∼10 −5 M . We explore the possibilities that the dust is freshly formed in the ejecta, heated dust in the pre-existing circumstellar medium, and an infrared echo. The light curves of SN2020oi are consistent with a STELLA model with canonical explosion energy, 0.07 M Ni mass, and 0.7 M ejecta mass. A model of high explosion energy of 10 52 erg, 0.4 M Ni mass, 6.5 M ejecta mass with the circumstellar matter, reproduces the double-peaked light curves of SN2020bvc. We observe temporal changes of absorption features of the IR Ca ii triplet, S i at 1.043 µm, and Fe ii at 5169 Å. The blue-shifted lines indicate high velocities, up to 60,000 km s −1 for SN2020bvc and 20,000 km s −1 for SN2020oi, and the expansion velocity rapidly declines before the optical maximum. We present spectral signatures and diagnostics of CO and SiO molecular bands between 1.4 and 10 µm.

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“…For the observational data from Joshi et al (2017), our models show that CO WDs with a mass 1.0-1.1 M or a 1.1 M ONe WDs can approach the narrow 12 C/ 13 C mass ratio observed in this nova. The results are consistent with the spectrographic data in the UV band which also suggested that the observed WD has a mass of 1.0-1.1 M (Miko lajewska & Shara 2017).…”

Section: Production Of Stable Isotopesmentioning

confidence: 77%

“…Their ratio represents how the proton capture competes with the CNO cycle. Another tight measurement from Nova Oph 2017 is given in Joshi et al (2017) which also shows a very low 12 C/ 13 C ratio of 1.6±0.3. In Figure 9 we show the three ratios of our models as a function of WD progenitor mass in comparison to these measurements.…”

Section: Production Of Stable Isotopesmentioning

confidence: 94%

Gamma-ray light curves and spectra of classical novae

Leung

Siegert

2022

Monthly Notices of the Royal Astronomical Society

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The nucleosynthesis in classical novae, in particular that of radioactive isotopes, is directly measurable by its γ-ray signature. Despite decades of observations, MeV γ-rays from novae have never been detected – neither individually at the time of the explosion, nor as a result of radioactive decay, nor the diffuse Galactic emission from the nova population. Thanks to recent developments in modeling of instrumental background for MeV telescopes such as INTEGRAL/SPI and Fermi/GBM, the prospects to finally detect these elusive transients are greatly enhanced. This demands for updated and refined models of γ-ray spectra and light curves of classical novae. In this work, we develop numerical models of nova explosions using sub- and near-Chandrasekhar CO white dwarfs as the progenitor. We study the parameter dependence of the explosions, their thermodynamics and energetics, as well as their chemical abundance patterns. We use a Monte Carlo radiative transfer code to compute γ-ray light curves and spectra, with a focus on the early time evolution. We compare our results to previous studies and find that the expected 511-keV-line flash at the time of the explosion is heavily suppressed, showing a maximum flux of only 10−9 ph cm−2 s−1 and thus making it at least one million times fainter than estimated before. This finding would render it impossible for current MeV instruments to detect novae within the first day after the outburst. Nevertheless, our time-resolved spectra can be used for retrospective analyses of archival data, thereby improving the sensitivity of the instruments.

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Nova Ophiuchus 2017 as a Probe of 13C Nucleosynthesis and Carbon Monoxide Formation and Destruction in Classical Novae

Cited by 9 publications

References 24 publications

Near-infrared and Optical Observations of Type Ic SN 2020oi and Broad-lined Type Ic SN 2020bvc: Carbon Monoxide, Dust, and High-velocity Supernova Ejecta

Near-infrared and Optical Observations of Type Ic SN 2020oi and Broad-lined Type Ic SN 2020bvc: Carbon Monoxide, Dust, and High-velocity Supernova Ejecta

Near-Infrared and Optical Observations of Type Ic SN2020oi and broad-lined Ic SN2020bvc: Carbon Monoxide, Dust and High-Velocity Supernova Ejecta

Gamma-ray light curves and spectra of classical novae

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