Realising efficient computation of individual frequencies for red-giant models
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arXiv
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| Format: | Preprint |
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2024
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| author | Larsen, Jens R. Christensen-Dalsgaard, Jørgen Lundkvist, Mia S. Rørsted, Jakob L. Winther, Mark L. Kjeldsen, Hans |
| author_facet | Larsen, Jens R. Christensen-Dalsgaard, Jørgen Lundkvist, Mia S. Rørsted, Jakob L. Winther, Mark L. Kjeldsen, Hans |
| contents | In order to improve the asteroseismic modelling efforts for red-giant stars, the numerical computation of theoretical individual oscillation modes for evolved red-giant models has to be made feasible. We aim to derive a method for circumventing the computational cost of computing oscillation spectra for models of red-giant stars with an average large frequency separation $Δν<15$ $μ$Hz, thereby allowing for asteroseismic investigations of giants utilising individual frequencies. The proposed Truncated Scanning Method serves as a novel method detailing how the observable individual $l=0,1,2$ frequencies of red giants may be computed on realistic timescales through so-called model truncation. By carefully removing the innermost region of the stellar models, the g-mode influence on the oscillation spectra may be avoided, allowing estimation of the observable regions from the resulting pure p-mode oscillations. The appropriate observable frequency regions are subsequently scanned for the complete and un-truncated stellar model. The observable regions are determined by considering the limitations on observability from the internal mode coupling and damping, yielding consistent frequency spectra obtained at a much reduced computational cost. The Truncated Scanning Method proves the feasibility of obtaining the individual frequencies of red-giant models for a wide range of applications and research, demonstrating an improved computational efficiency by a factor of 10 or better. This means that the inclusion of $l=1,2$ individual frequencies is now a possibility in future asteroseismic modelling efforts of red-giant stars. Further potential avenues for improvements to this method are outlined for future pursuits. |
| format | Preprint |
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arxiv_https___arxiv_org_abs_2408_16382 |
| institution | arXiv |
| publishDate | 2024 |
| record_format | arxiv |
| spellingShingle | Realising efficient computation of individual frequencies for red-giant models Larsen, Jens R. Christensen-Dalsgaard, Jørgen Lundkvist, Mia S. Rørsted, Jakob L. Winther, Mark L. Kjeldsen, Hans Solar and Stellar Astrophysics In order to improve the asteroseismic modelling efforts for red-giant stars, the numerical computation of theoretical individual oscillation modes for evolved red-giant models has to be made feasible. We aim to derive a method for circumventing the computational cost of computing oscillation spectra for models of red-giant stars with an average large frequency separation $Δν<15$ $μ$Hz, thereby allowing for asteroseismic investigations of giants utilising individual frequencies. The proposed Truncated Scanning Method serves as a novel method detailing how the observable individual $l=0,1,2$ frequencies of red giants may be computed on realistic timescales through so-called model truncation. By carefully removing the innermost region of the stellar models, the g-mode influence on the oscillation spectra may be avoided, allowing estimation of the observable regions from the resulting pure p-mode oscillations. The appropriate observable frequency regions are subsequently scanned for the complete and un-truncated stellar model. The observable regions are determined by considering the limitations on observability from the internal mode coupling and damping, yielding consistent frequency spectra obtained at a much reduced computational cost. The Truncated Scanning Method proves the feasibility of obtaining the individual frequencies of red-giant models for a wide range of applications and research, demonstrating an improved computational efficiency by a factor of 10 or better. This means that the inclusion of $l=1,2$ individual frequencies is now a possibility in future asteroseismic modelling efforts of red-giant stars. Further potential avenues for improvements to this method are outlined for future pursuits. |
| title | Realising efficient computation of individual frequencies for red-giant models |
| topic | Solar and Stellar Astrophysics |
| url | https://arxiv.org/abs/2408.16382 |