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Forward modelling and the quest for mode identification in rapidly rotating stars
dc.contributor.author | Mirouh, Giovanni Marcello | |
dc.date.accessioned | 2022-11-18T10:28:52Z | |
dc.date.available | 2022-11-18T10:28:52Z | |
dc.date.issued | 2022-10-07 | |
dc.identifier.citation | Mirouh GM (2022), Forward modelling and the quest for mode identification in rapidly rotating stars. Front. Astron. Space Sci. 9:952296. doi: [10.3389/fspas.2022.952296] | es_ES |
dc.identifier.uri | https://hdl.handle.net/10481/78033 | |
dc.description.abstract | Asteroseismology has opened a window on the internal physics of thousands of stars, by relating oscillation spectra properties to the internal physics of stars. Mode identification, namely the process of associating a measured oscillation frequency to the corresponding mode geometry and properties, is the cornerstone of this analysis of seismic spectra. In rapidly rotating stars this identification is a challenging task that remains incomplete, as modes assume complex geometries and regular patterns in frequencies get scrambled under the influence of the Coriolis force and centrifugal flattening. In this article, I will first discuss the various classes of mode geometries that emerge in rapidly rotating stars and the related frequency and period patterns, as predicted by ray dynamics, complete (non-)adiabatic calculations, or using the traditional approximation of rotation. These patterns scale with structural quantities and help us derive crucial constraints on the structure and evolution of these stars. I will summarize the amazing progress accomplished over the last few years for the deciphering of gravity-mode pulsator oscillation spectra, and recent developments based on machine-learning classification techniques to distinguish oscillation modes and pattern analysis strategies that let us access the underlying physics of pressure-mode pulsators. These approaches pave the way to ensemble asteroseismology of classical pulsators. Finally, I will highlight how these recent progress can be combined to improve forward seismic modelling. I will focus on the example of Rasalhague, a well-known rapid rotator, to illustrate the process and the needed advances to obtain à-la-carte modelling of such stars. | es_ES |
dc.language.iso | eng | es_ES |
dc.publisher | Frontiers | es_ES |
dc.rights | Atribución 4.0 Internacional | * |
dc.rights.uri | http://creativecommons.org/licenses/by/4.0/ | * |
dc.subject | Stars: oscillations | es_ES |
dc.subject | Stars: rotation | es_ES |
dc.subject | Stars: interiors | es_ES |
dc.subject | Stars:individual α Ophiuchi | es_ES |
dc.subject | Stars: evolution | es_ES |
dc.title | Forward modelling and the quest for mode identification in rapidly rotating stars | es_ES |
dc.type | info:eu-repo/semantics/article | es_ES |
dc.rights.accessRights | info:eu-repo/semantics/openAccess | es_ES |
dc.identifier.doi | 10.3389/fspas.2022.952296 | |
dc.type.hasVersion | info:eu-repo/semantics/publishedVersion | es_ES |