Numerical and Physical Challenges to Nebular Spectroscopy in Thermonuclear Supernovae
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| Auteurs principaux: | , , , , , , , , , , |
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| Format: | Preprint |
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2025
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| _version_ | 1866913647651979264 |
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| author | Hoeflich, P. Fereidouni, E. Fisher, A. Mera, T. Ashall, C. Brown, P. Baron, E. DerKacy, J. Diamond, T. Shabandeh, M. Stritzinger, M. |
| author_facet | Hoeflich, P. Fereidouni, E. Fisher, A. Mera, T. Ashall, C. Brown, P. Baron, E. DerKacy, J. Diamond, T. Shabandeh, M. Stritzinger, M. |
| contents | Thermodynamical explosions of White Dwarfs (WD)are one of the keys to high precision cosmology. Nebular spectra, namely mid-infrared (MIR) with JWST are an effective tool to probe for the multi-dimensional imprints of the explosion physics of WDs and their progenitor systems but also pose a challenge for simulations. What we observe as SNe Ia are low-energy photons, namely light curves, and spectra detected some days to years after the explosion. The light is emitted from a rapidly expanding envelope consisting of a low-density and low-temperature plasma with atomic population numbers far from thermodynamical equilibrium. SNe Ia are powered radioactive decays which produce hard X- and gamma-rays and MeV leptons which are converted within the ejecta to low-energy photons. We find that the optical and IR nebular spectra depend sensitively on the proper treatment of the physical conversion of high to low energies. The low-energy photons produced by forbidden line transitions originate from a mostly optically thin envelope. However, the UV is optically thick because of a quasi-continuum formed by allowed lines and bound-free transitions even several years after the explosion. We find that stimulated recombination limits the over-ionization of high ions with populations governed by the far UV. The requirements to simulate nebular spectra are well beyond both classical stellar atmospheres and nebulae. Using our full non-LTE HYDrodynamical RAdiation code (HYDRA) as a test-bed, the sensitivity on the physics on synthetic spectra are demonstrated using observations as a benchmark. At some examples, we establish the power of high-precision nebular spectroscopy as quantitative tool. Centrally ignited, off-center delayed-detonation near Chandrasekhar-mass models can reproduce line-ratios and line profiles of Branch-normal and underluminous SNe Ia observed with JWST. |
| format | Preprint |
| id |
arxiv_https___arxiv_org_abs_2501_07654 |
| institution | arXiv |
| publishDate | 2025 |
| record_format | arxiv |
| spellingShingle | Numerical and Physical Challenges to Nebular Spectroscopy in Thermonuclear Supernovae Hoeflich, P. Fereidouni, E. Fisher, A. Mera, T. Ashall, C. Brown, P. Baron, E. DerKacy, J. Diamond, T. Shabandeh, M. Stritzinger, M. Solar and Stellar Astrophysics High Energy Astrophysical Phenomena Space Physics Thermodynamical explosions of White Dwarfs (WD)are one of the keys to high precision cosmology. Nebular spectra, namely mid-infrared (MIR) with JWST are an effective tool to probe for the multi-dimensional imprints of the explosion physics of WDs and their progenitor systems but also pose a challenge for simulations. What we observe as SNe Ia are low-energy photons, namely light curves, and spectra detected some days to years after the explosion. The light is emitted from a rapidly expanding envelope consisting of a low-density and low-temperature plasma with atomic population numbers far from thermodynamical equilibrium. SNe Ia are powered radioactive decays which produce hard X- and gamma-rays and MeV leptons which are converted within the ejecta to low-energy photons. We find that the optical and IR nebular spectra depend sensitively on the proper treatment of the physical conversion of high to low energies. The low-energy photons produced by forbidden line transitions originate from a mostly optically thin envelope. However, the UV is optically thick because of a quasi-continuum formed by allowed lines and bound-free transitions even several years after the explosion. We find that stimulated recombination limits the over-ionization of high ions with populations governed by the far UV. The requirements to simulate nebular spectra are well beyond both classical stellar atmospheres and nebulae. Using our full non-LTE HYDrodynamical RAdiation code (HYDRA) as a test-bed, the sensitivity on the physics on synthetic spectra are demonstrated using observations as a benchmark. At some examples, we establish the power of high-precision nebular spectroscopy as quantitative tool. Centrally ignited, off-center delayed-detonation near Chandrasekhar-mass models can reproduce line-ratios and line profiles of Branch-normal and underluminous SNe Ia observed with JWST. |
| title | Numerical and Physical Challenges to Nebular Spectroscopy in Thermonuclear Supernovae |
| topic | Solar and Stellar Astrophysics High Energy Astrophysical Phenomena Space Physics |
| url | https://arxiv.org/abs/2501.07654 |