A Stringent Test of Magnetic Models of Stellar Evolution
Main-sequence stars with convective envelopes often appear larger and cooler than predicted by standard models of stellar evolution for their measured masses. This is believed to be caused by stellar activity. In a recent study, accurate measurements were published for the K-type components of the 1...
| Main Authors: | , , , |
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| Format: | Article |
| Language: | English |
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MDPI AG
2021-12-01
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| Series: | Galaxies |
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| Online Access: | https://www.mdpi.com/2075-4434/10/1/3 |
| _version_ | 1827654839819042816 |
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| author | Guillermo Torres Gregory A. Feiden Andrew Vanderburg Jason L. Curtis |
| author_facet | Guillermo Torres Gregory A. Feiden Andrew Vanderburg Jason L. Curtis |
| author_sort | Guillermo Torres |
| collection | DOAJ |
| description | Main-sequence stars with convective envelopes often appear larger and cooler than predicted by standard models of stellar evolution for their measured masses. This is believed to be caused by stellar activity. In a recent study, accurate measurements were published for the K-type components of the 1.62-day detached eclipsing binary EPIC 219511354, showing the radii and temperatures for both stars to be affected by these discrepancies. This is a rare example of a system in which the age and chemical composition are known, by virtue of being a member of the well-studied open cluster Ruprecht 147 (age~3 Gyr, [Fe/H] = +0.10). Here, we report a detailed study of this system with nonstandard models incorporating magnetic inhibition of convection. We show that these calculations are able to reproduce the observations largely within their uncertainties, providing robust estimates of the strength of the magnetic fields on both stars: 1600 ± 130 G and 1830 ± 150 G for the primary and secondary, respectively. Empirical estimates of the magnetic field strengths based on the measured X-ray luminosity of the system are roughly consistent with these predictions, supporting this mechanism as a possible explanation for the radius and temperature discrepancies. |
| first_indexed | 2024-03-09T21:54:28Z |
| format | Article |
| id | doaj.art-24ca04fee19b47679087f6b81f7159e9 |
| institution | Directory Open Access Journal |
| issn | 2075-4434 |
| language | English |
| last_indexed | 2024-03-09T21:54:28Z |
| publishDate | 2021-12-01 |
| publisher | MDPI AG |
| record_format | Article |
| series | Galaxies |
| spelling | doaj.art-24ca04fee19b47679087f6b81f7159e92023-11-23T20:00:13ZengMDPI AGGalaxies2075-44342021-12-01101310.3390/galaxies10010003A Stringent Test of Magnetic Models of Stellar EvolutionGuillermo Torres0Gregory A. Feiden1Andrew Vanderburg2Jason L. Curtis3Center for Astrophysics Harvard & Smithsonian, 60 Garden Street, Cambridge, MA 02138, USADepartment of Physics & Astronomy, University of North Georgia, Dahlonega, GA 30597, USADepartment of Physics and Kavli Institute for Astrophysics and Space Research, Massachusetts Institute of Technology, Cambridge, MA 02139, USADepartment of Astronomy, Columbia University, 550 West 120th Street, New York, NY 10027, USAMain-sequence stars with convective envelopes often appear larger and cooler than predicted by standard models of stellar evolution for their measured masses. This is believed to be caused by stellar activity. In a recent study, accurate measurements were published for the K-type components of the 1.62-day detached eclipsing binary EPIC 219511354, showing the radii and temperatures for both stars to be affected by these discrepancies. This is a rare example of a system in which the age and chemical composition are known, by virtue of being a member of the well-studied open cluster Ruprecht 147 (age~3 Gyr, [Fe/H] = +0.10). Here, we report a detailed study of this system with nonstandard models incorporating magnetic inhibition of convection. We show that these calculations are able to reproduce the observations largely within their uncertainties, providing robust estimates of the strength of the magnetic fields on both stars: 1600 ± 130 G and 1830 ± 150 G for the primary and secondary, respectively. Empirical estimates of the magnetic field strengths based on the measured X-ray luminosity of the system are roughly consistent with these predictions, supporting this mechanism as a possible explanation for the radius and temperature discrepancies.https://www.mdpi.com/2075-4434/10/1/3stellar evolutioneclipsing binariesfundamental stellar parametersstellar activitymagnetic fieldsopen clusters |
| spellingShingle | Guillermo Torres Gregory A. Feiden Andrew Vanderburg Jason L. Curtis A Stringent Test of Magnetic Models of Stellar Evolution Galaxies stellar evolution eclipsing binaries fundamental stellar parameters stellar activity magnetic fields open clusters |
| title | A Stringent Test of Magnetic Models of Stellar Evolution |
| title_full | A Stringent Test of Magnetic Models of Stellar Evolution |
| title_fullStr | A Stringent Test of Magnetic Models of Stellar Evolution |
| title_full_unstemmed | A Stringent Test of Magnetic Models of Stellar Evolution |
| title_short | A Stringent Test of Magnetic Models of Stellar Evolution |
| title_sort | stringent test of magnetic models of stellar evolution |
| topic | stellar evolution eclipsing binaries fundamental stellar parameters stellar activity magnetic fields open clusters |
| url | https://www.mdpi.com/2075-4434/10/1/3 |
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