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Theoretical mass estimates for the Mira-type variable R Hydrae
Solar and Stellar Astrophysics · Submitted 31 May 2023
abstract compiled · 2026-09-23 · no language-model review
The authors' main claim Theoretical mass estimates of R Hya are in the range $4.44M_\odot\le M\le 4.63M_\odot$, whereas the mean stellar radius ($421R_\odot\le \bar R \le 445R_\odot$) corresponding to the pulsation period $\Pi\approx 380$ agrees well with measurements of the angular diameter by methods of the optical interferometric imaging.
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The abstract, sentence by sentence
Calculations of stellar evolution at initial abundances of helium $Y=0.28$ and heavier elements $Z=0.014$ were done for stars with masses on the main sequence $1.7M_\odot\le M_\textrm{ZAMS}\le 5.2M_\odot$. Evolutionary sequences corresponding to the AGB stage were used for modelling the pulsation period decrease observed for almost two centuries in the Mira--type variable R Hya. Diminution of the period from $\Pi\approx$ 495 d in the second half of the eighteenth century to $\Pi\approx 380$ d in the 1950s is due stellar radius decrease accompanying dissipation of the radiation--diffusion wave generated by the helium flash. For all the history of its observations R Hya was the fundamental mode pulsator. The best agreement with observations is obtained for eight evolutionary models with initial mass $M_\textrm{ZAMS}=4.8M_\odot$ and the mass loss rate parameter of the Bl\"ocker formula $0.03\le\eta_\mathrm{B}\le 0.07$. Theoretical mass estimates of R Hya are in the range $4.44M_\odot\le M\le 4.63M_\odot$, whereas the mean stellar radius ($421R_\odot\le \bar R \le 445R_\odot$) corresponding to the pulsation period $\Pi\approx 380$ agrees well with measurements of the angular diameter by methods of the optical interferometric imaging.
background contribution method result interpretation main claim
| # | sentence | role | the authors' own work | states the main conclusion | strength |
|---|---|---|---|---|---|
| s0 | Calculations of stellar evolution at initial abundances of helium $Y=0.28$ and heavier elements $Z=0.014$ were done for stars with masses on the main sequence $1.7M_\odot\le M_\textrm{ZAMS}\le 5.2M_\odot$. | method 0.98 | 0.90 | 0.03 | asserted 0.98 |
| s1 | Evolutionary sequences corresponding to the AGB stage were used for modelling the pulsation period decrease observed for almost two centuries in the Mira--type variable R Hya. | method 0.95 | 0.66 | 0.06 | asserted 0.98 |
| s2 | Diminution of the period from $\Pi\approx$ 495 d in the second half of the eighteenth century to $\Pi\approx 380$ d in the 1950s is due stellar radius decrease accompanying dissipation of the radiation--diffusion wave generated by the helium flash. | interpretation 0.83 | 0.64 | 0.24 | asserted 1.00 |
| s3 | For all the history of its observations R Hya was the fundamental mode pulsator. | background 0.59 | 0.19 | 0.04 | asserted 1.00 |
| s4 | The best agreement with observations is obtained for eight evolutionary models with initial mass $M_\textrm{ZAMS}=4.8M_\odot$ and the mass loss rate parameter of the Bl\"ocker formula $0.03\le\eta_\mathrm{B}\le 0.07$. | result 0.99 | 0.92 | 0.34 | asserted 0.99 |
| s5 | Theoretical mass estimates of R Hya are in the range $4.44M_\odot\le M\le 4.63M_\odot$, whereas the mean stellar radius ($421R_\odot\le \bar R \le 445R_\odot$) corresponding to the pulsation period $\Pi\approx 380$ agrees well with measurements of the angular diameter by methods of the optical interferometric imaging. | result 1.00 | 0.89 | 0.80 | asserted 0.98 |
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Original abstract
Calculations of stellar evolution at initial abundances of helium $Y=0.28$ and heavier elements $Z=0.014$ were done for stars with masses on the main sequence $1.7M_\odot\le M_\textrm{ZAMS}\le 5.2M_\odot$. Evolutionary sequences corresponding to the AGB stage were used for modelling the pulsation period decrease observed for almost two centuries in the Mira--type variable R Hya. Diminution of the period from $\Pi\approx$ 495 d in the second half of the eighteenth century to $\Pi\approx 380$ d in the 1950s is due stellar radius decrease accompanying dissipation of the radiation--diffusion wave generated by the helium flash. For all the history of its observations R Hya was the fundamental mode pulsator. The best agreement with observations is obtained for eight evolutionary models with initial mass $M_\textrm{ZAMS}=4.8M_\odot$ and the mass loss rate parameter of the Bl\"ocker formula $0.03\le\eta_\mathrm{B}\le 0.07$. Theoretical mass estimates of R Hya are in the range $4.44M_\odot\le M\le 4.63M_\odot$, whereas the mean stellar radius ($421R_\odot\le \bar R \le 445R_\odot$) corresponding to the pulsation period $\Pi\approx 380$ agrees well with measurements of the angular diameter by methods of the optical interferometric imaging.
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