Modelled parameters of Cepheid and RR Lyrae : J/MNRAS/491/4752

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Authors : Bellinger E.P. orcid , Kanbur S.M., Bhardwaj A. (hide) , Kanbur S.M., Bhardwaj A. et..al

VizieR DOI : 10.26093/cds/vizier.74914752
Bibcode : 2020MNRAS.491.4752B (ADS) (Simbad) (Objects)
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CDS Keywords : Stars, variable; Magellanic Clouds; Models; Stars, masses; Stars, diameters; Effective temperatures; Optical
UAT : Variable stars, Magellanic Clouds, Astronomical models, Stellar masses, Stellar radii, Effective temperature, Optical astronomy

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Inserted into VizieR : 28-Apr-2023
Last modification : 20-Aug-2024

When a period is not a full stop Light-curve structure reveals fundamental parameters of Cepheid and RR Lyrae stars. (2020)

Keywords : stars fundamental parameters - stars: oscillations - stars: variables: Cepheids - stars: variables: RR Lyrae - Magellanic Clouds - distance scale

Abstract:The period of pulsation and the structure of the light curve for Cepheid and RR Lyrae variables depend on the fundamental parameters of the star: mass, radius, luminosity, and effective temperature. Here, we train artificial neural networks on theoretical pulsation models to predict the fundamental parameters of these stars based on their period and light-curve structure. We find significant improvements to estimates of these parameters made using light-curve structure and period over estimates made using only the period. Given that the models are able to reproduce most observables, we find that the fundamental parameters of these stars can be estimated up to 60 per cent more accurately when light-curve structure is taken into ...(more)
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Our interest is in determining global stellar parameters of Cepheids and RR Lyraes, such as M, L, T_eff_, and R and in constraining input stellar physics. The period-mean density relation suggests that the observable period is the most important quantity in constraining the global stellar parameters. However, in this study, using recently published pulsation models for Cepheids and RR Lyraes, we have used modern data analysis methods to demonstrate that light-curve structure plays a statistically significant part in determining these parameters. Using these techniques, we have developed a catalogue of predicted masses, luminosities, radii, and effective temperatures for OGLE Cepheids and RR Lyraes. We have furthermore used the predicted luminosities and hence predicted V- and I-band theoretical magnitudes to construct a Wesenheit function and estimate the distance to the LMC and SMC. Our calculated distances are statistically consistent with the latest estimates from eclipsing binaries. 


                


                

                    

                


                

                    

                


                

                    
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