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| Format: | Preprint |
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2024
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| Online-Zugang: | https://arxiv.org/abs/2411.10256 |
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| _version_ | 1866916482504458240 |
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| author | Herrera, Yago Vela, Daniel Muñoz Sala, Glòria José, Jordi Cavecchi, Yuri |
| author_facet | Herrera, Yago Vela, Daniel Muñoz Sala, Glòria José, Jordi Cavecchi, Yuri |
| contents | X-Ray bursts (XRBs) are powerful thermonuclear events on the surface of accreting neutron stars (NSs), which can synthesize intermediate-mass elements. Although the high surface gravity prevents an explosive ejection, a small fraction of the envelope may be ejected by radiation-driven winds. In our previous works, we have developed a non-relativistic radiative wind model and coupled it to an XRB hydrodynamic simulation. We now apply this technique to another model featuring consecutive bursts. We determine the mass-loss and chemical composition of the wind ejecta. Results show that, for a representative XRB, about $0.1\%$ of the envelope mass is ejected per burst, at an average rate of $3.9 \times 10^{-12}\,M_\odot \texttt{yr}^{-1}$. Between $66\%$ and $76\%$ of the ejecta composition is $^{60}$Ni, $^{64}$Zn, $^{68}$Ge, $^{4}$He and $^{58}$Ni. We also report on the evolution of observational quantities during the wind phase and simulate NICER observations that resemble those of 4U 1820-40. |
| format | Preprint |
| id |
arxiv_https___arxiv_org_abs_2411_10256 |
| institution | arXiv |
| publishDate | 2024 |
| record_format | arxiv |
| spellingShingle | Mass-loss, composition and observational signatures of stellar winds from X-ray bursts Herrera, Yago Vela, Daniel Muñoz Sala, Glòria José, Jordi Cavecchi, Yuri High Energy Astrophysical Phenomena Solar and Stellar Astrophysics X-Ray bursts (XRBs) are powerful thermonuclear events on the surface of accreting neutron stars (NSs), which can synthesize intermediate-mass elements. Although the high surface gravity prevents an explosive ejection, a small fraction of the envelope may be ejected by radiation-driven winds. In our previous works, we have developed a non-relativistic radiative wind model and coupled it to an XRB hydrodynamic simulation. We now apply this technique to another model featuring consecutive bursts. We determine the mass-loss and chemical composition of the wind ejecta. Results show that, for a representative XRB, about $0.1\%$ of the envelope mass is ejected per burst, at an average rate of $3.9 \times 10^{-12}\,M_\odot \texttt{yr}^{-1}$. Between $66\%$ and $76\%$ of the ejecta composition is $^{60}$Ni, $^{64}$Zn, $^{68}$Ge, $^{4}$He and $^{58}$Ni. We also report on the evolution of observational quantities during the wind phase and simulate NICER observations that resemble those of 4U 1820-40. |
| title | Mass-loss, composition and observational signatures of stellar winds from X-ray bursts |
| topic | High Energy Astrophysical Phenomena Solar and Stellar Astrophysics |
| url | https://arxiv.org/abs/2411.10256 |