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| Natura: | Preprint |
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2024
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| Accesso online: | https://arxiv.org/abs/2407.09634 |
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| _version_ | 1866916322267365376 |
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| author | Pandey, Ruchi Srivastava, Mudit K. Shaw, Gargi |
| author_facet | Pandey, Ruchi Srivastava, Mudit K. Shaw, Gargi |
| contents | The eruption of Nova V2891 Cygni in 2019 offers a rare opportunity to explore the shock-induced processes in novae ejecta. The spectral evolution shows noticeable differences in the evolution of various oxygen emission lines such as O I 7773 Å, O I 8446 Å, O I 1.1286 $μ$m, O I 1.3164 $μ$m, etc. Here, we use spectral synthesis code CLOUDY to study the temporal evolution of these oxygen emission lines. Our photoionization model requires the introduction of a component with a very high density ($n ~ 10^{11}$ cm$^{-3}$) and an enhanced oxygen abundance (O/H $\sim$ 28) to produce the O I 7773 Å emission line, suggesting a stratification of material with high oxygen abundance within the ejecta. An important outcome is the behaviour of the O I 1.3164 $μ$m line, which could only be generated by invoking the collisional ionization models in CLOUDY. Our phenomenological analysis suggests that O I 1.3164 $μ$m emission originates from a thin, dense shell characterized by a high density of about $10^{12.5} - 10^{12.8}$ cm$^{-3}$, which is most likely formed due to the strong internal collisions. If such is the case, the O I 1.3164 $μ$m emission presents itself as a tracer of shock-induced dust formation in V2891 Cyg. The collisional ionization models have also been successful in creating the high-temperature conditions ($~ 7.07 - 7.49 \times 10^5$ K) required to reproduce the observed high ionization potential coronal lines, which coincide with the epoch of dust formation and evolution of the O I 1.3164 $μ$m emission line. |
| format | Preprint |
| id |
arxiv_https___arxiv_org_abs_2407_09634 |
| institution | arXiv |
| publishDate | 2024 |
| record_format | arxiv |
| spellingShingle | A phenomenological study of the evolution of shock-induced O I emission lines in the spectrum of nova V2891 Cygni Pandey, Ruchi Srivastava, Mudit K. Shaw, Gargi Solar and Stellar Astrophysics The eruption of Nova V2891 Cygni in 2019 offers a rare opportunity to explore the shock-induced processes in novae ejecta. The spectral evolution shows noticeable differences in the evolution of various oxygen emission lines such as O I 7773 Å, O I 8446 Å, O I 1.1286 $μ$m, O I 1.3164 $μ$m, etc. Here, we use spectral synthesis code CLOUDY to study the temporal evolution of these oxygen emission lines. Our photoionization model requires the introduction of a component with a very high density ($n ~ 10^{11}$ cm$^{-3}$) and an enhanced oxygen abundance (O/H $\sim$ 28) to produce the O I 7773 Å emission line, suggesting a stratification of material with high oxygen abundance within the ejecta. An important outcome is the behaviour of the O I 1.3164 $μ$m line, which could only be generated by invoking the collisional ionization models in CLOUDY. Our phenomenological analysis suggests that O I 1.3164 $μ$m emission originates from a thin, dense shell characterized by a high density of about $10^{12.5} - 10^{12.8}$ cm$^{-3}$, which is most likely formed due to the strong internal collisions. If such is the case, the O I 1.3164 $μ$m emission presents itself as a tracer of shock-induced dust formation in V2891 Cyg. The collisional ionization models have also been successful in creating the high-temperature conditions ($~ 7.07 - 7.49 \times 10^5$ K) required to reproduce the observed high ionization potential coronal lines, which coincide with the epoch of dust formation and evolution of the O I 1.3164 $μ$m emission line. |
| title | A phenomenological study of the evolution of shock-induced O I emission lines in the spectrum of nova V2891 Cygni |
| topic | Solar and Stellar Astrophysics |
| url | https://arxiv.org/abs/2407.09634 |