individual
What campus are you from?
Daytona Beach
Authors' Class Standing
Jacob Becker, Senior
Lead Presenter's Name
Jacob Becker
Faculty Mentor Name
Terry Oswalt
Abstract
Stellar age estimations derived from asteroseismology depend on stellar models that are sensitive to metallicity (Z). Variations in this parameter could alter the agreement between gyrochronological and asteroseismic ages, as well as main sequence lifetimes and observational properties such as effective temperature and luminosity. We test how much typical metallicity differences (±0.2 dex) affect main-sequence models of solar-type stars. Using MESA, evolutionary tracks are created for 1 M☉ stars at three metallicities (Z = 0.009, 0.014, 0.022), and it is measured how these changes shift the positions of the zero-age main sequence and the corresponding main sequence lifetimes. This work aims to establish a quantitative baseline for how model metallicity influences stellar evolution predictions relevant to the main sequence lifetime and subsequent star properties. By finding the magnitude of this effect, we aim to determine whether metallicity-dependent model uncertainties are sufficiently large enough to influence comparisons between the gyrochronological and asteroseismic ages, as well as luminosities and temperatures in solar-type stars and wide-binary systems. Support from NSF grants AST-1910396, AST-2108975 and NASA grants 80NSSC22K0622, 80NSSC21K0245, and NNX16AB76G is gratefully acknowledged.
Did this research project receive funding support from the Office of Undergraduate Research.
No
Quantifying the Effect of Metallicity on Stellar Properties and Evolutionary Timescales
Stellar age estimations derived from asteroseismology depend on stellar models that are sensitive to metallicity (Z). Variations in this parameter could alter the agreement between gyrochronological and asteroseismic ages, as well as main sequence lifetimes and observational properties such as effective temperature and luminosity. We test how much typical metallicity differences (±0.2 dex) affect main-sequence models of solar-type stars. Using MESA, evolutionary tracks are created for 1 M☉ stars at three metallicities (Z = 0.009, 0.014, 0.022), and it is measured how these changes shift the positions of the zero-age main sequence and the corresponding main sequence lifetimes. This work aims to establish a quantitative baseline for how model metallicity influences stellar evolution predictions relevant to the main sequence lifetime and subsequent star properties. By finding the magnitude of this effect, we aim to determine whether metallicity-dependent model uncertainties are sufficiently large enough to influence comparisons between the gyrochronological and asteroseismic ages, as well as luminosities and temperatures in solar-type stars and wide-binary systems. Support from NSF grants AST-1910396, AST-2108975 and NASA grants 80NSSC22K0622, 80NSSC21K0245, and NNX16AB76G is gratefully acknowledged.