Non-Thermal Ionization of Kilonova Ejecta: Observable Impacts
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arXiv
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| Autori principali: | , , , |
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| Natura: | Preprint |
| Pubblicazione: |
2025
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| _version_ | 1866918131514998784 |
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| author | Brethauer, Daniel Kasen, Daniel Margutti, Raffaella Chornock, Ryan |
| author_facet | Brethauer, Daniel Kasen, Daniel Margutti, Raffaella Chornock, Ryan |
| contents | The characteristic rapid rise and decline at optical wavelengths of a kilonova is the product of the low ejecta mass ($\lesssim 0.05 M_\odot$) and high ejecta velocity ($\gtrsim 0.1$c). We show that, even at very early times ($\lesssim 2$ days), regions of ejecta fall below critical density and temperature thresholds at which non-local thermodynamic equilibrium (NLTE) effects become important. Here, we present an approximate method for calculating the ionization state of the ejecta that accounts for the NLTE impact of high-energy electrons produced in the beta decay of freshly synthesized $r$-process elements. We find that incorporating ionization from high-energy electrons produces an ``inverted" and ``blended" ionization structure, where the most highly ionized species are located in the fastest moving homologous ejecta and multiple ionization states coexist. In radiation transport calculations, the higher degree of ionization reduces line blanketing in optical bands, leading to improved agreement with the light curve properties of AT\,2017gfo such as the duration, decay rates, brightness, and colors. Our quasi-NLTE implementation helps to alleviate tensions in kilonova modeling: for high-velocity ($\sim 0.3c$) ejecta components our models require less mass for a given peak brightness in optical bands, by as much as a factor of 3; our models can explain the presence of observed features associated to Sr II, W III, Se III, and Te III under conditions where LTE models would predict only neutral species; and we naturally predict the coexistence of species like Sr II and Ce III without the need for fine-tuning of the ejecta properties. |
| format | Preprint |
| id |
arxiv_https___arxiv_org_abs_2508_18364 |
| institution | arXiv |
| publishDate | 2025 |
| record_format | arxiv |
| spellingShingle | Non-Thermal Ionization of Kilonova Ejecta: Observable Impacts Brethauer, Daniel Kasen, Daniel Margutti, Raffaella Chornock, Ryan High Energy Astrophysical Phenomena Solar and Stellar Astrophysics The characteristic rapid rise and decline at optical wavelengths of a kilonova is the product of the low ejecta mass ($\lesssim 0.05 M_\odot$) and high ejecta velocity ($\gtrsim 0.1$c). We show that, even at very early times ($\lesssim 2$ days), regions of ejecta fall below critical density and temperature thresholds at which non-local thermodynamic equilibrium (NLTE) effects become important. Here, we present an approximate method for calculating the ionization state of the ejecta that accounts for the NLTE impact of high-energy electrons produced in the beta decay of freshly synthesized $r$-process elements. We find that incorporating ionization from high-energy electrons produces an ``inverted" and ``blended" ionization structure, where the most highly ionized species are located in the fastest moving homologous ejecta and multiple ionization states coexist. In radiation transport calculations, the higher degree of ionization reduces line blanketing in optical bands, leading to improved agreement with the light curve properties of AT\,2017gfo such as the duration, decay rates, brightness, and colors. Our quasi-NLTE implementation helps to alleviate tensions in kilonova modeling: for high-velocity ($\sim 0.3c$) ejecta components our models require less mass for a given peak brightness in optical bands, by as much as a factor of 3; our models can explain the presence of observed features associated to Sr II, W III, Se III, and Te III under conditions where LTE models would predict only neutral species; and we naturally predict the coexistence of species like Sr II and Ce III without the need for fine-tuning of the ejecta properties. |
| title | Non-Thermal Ionization of Kilonova Ejecta: Observable Impacts |
| topic | High Energy Astrophysical Phenomena Solar and Stellar Astrophysics |
| url | https://arxiv.org/abs/2508.18364 |