Abstract
The process of building seismic models of observed stars that match the observed pulsation frequencies often proves to be a difficult one. The outputs of computational codes used to perform these calculations match observational data fairly well for the sun, but fail to do so as well for larger-mass stars. This suggests that the codes are neglecting potentially significant processes that occur more strongly in larger stars. We examine some hydrodynamically motivated modifications to the standard stellar models that might help to bring theoretical calculations into agreement with observational data. The analysis of Press (1981) and Press & Rybicki (1981) is applied to the case of the δ Scuti star FG Vir, and presented.
Talk to us
Join us for a 30 min session where you can share your feedback and ask us any queries you have
Schedule a callDisclaimer: All third-party content on this website/platform is and will remain the property of their respective owners and is provided on "as is" basis without any warranties, express or implied. Use of third-party content does not indicate any affiliation, sponsorship with or endorsement by them. Any references to third-party content is to identify the corresponding services and shall be considered fair use under The CopyrightLaw.
