Hostname: page-component-78c5997874-lj6df Total loading time: 0 Render date: 2024-11-05T21:15:50.191Z Has data issue: false hasContentIssue false
  • English
  • Français

The Effects of Magnetic Activity on Lithium-Inferred Ages of Stars

Published online by Cambridge University Press:  07 August 2014

Aaron J. Juarez ,
Phillip A. Cargile ,
David J. James  and
Keivan G. Stassun
Aaron J. Juarez
Affiliation:
Dept. of Physics, Fisk University, Nashville, TN 37208, USA Dept. of Physics and Astronomy, Vanderbilt University, Nashville, TN 37235, USA email: [email protected]
Phillip A. Cargile
Affiliation:
Dept. of Physics and Astronomy, Vanderbilt University, Nashville, TN 37235, USA email: [email protected]
David J. James
Affiliation:
Cerro Tololo Inter-American Observatory, Casilla 603, La Serena, Chile
Keivan G. Stassun
Affiliation:
Dept. of Physics, Fisk University, Nashville, TN 37208, USA Dept. of Physics and Astronomy, Vanderbilt University, Nashville, TN 37235, USA email: [email protected]
Rights & Permissions [Opens in a new window]

Abstract

Core share and HTML view are not available for this content. However, as you have access to this content, a full PDF is available via the ‘Save PDF’ action button.

In this project, we investigate the effects of magnetic activity on the Lithium Depletion Boundary (LDB) to recalibrate the measured ages for star clusters, using the open cluster Blanco 1 as a pilot study. We apply the LDB technique on low-mass Pre-Main-Sequence (PMS) stars to derive an accurate age for Blanco 1, and we consider the effect of magnetic activity on this inferred age. Although observations have shown that magnetic activity directly affects stellar radius and temperature, most PMS models do not include the effects of magnetic activity on stellar properties. Since the lithium abundance of a star depends on its radius and temperature, we expect that LDB ages are affected by magnetic activity. After empirically accounting for the effects of magnetic activity, we find the age of Blanco 1 to be ~100 Myr, which is ~30 Myr younger than the standard LDB age of ~130 Myr.

Keywords

Magnetic activityfundamental parameterspre-main sequence starsopen clusters
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 9 , Symposium S302: Magnetic Fields throughout Stellar Evolution , August 2013 , pp. 100 - 101
Copyright
Copyright © International Astronomical Union 2014 

References

Allard, F., Homeier, D., & Freytag, B. 2012, Phil. Trans. R. Soc. A 370 2765Google Scholar
Baraffe, I., Chabrier, G., Allard, F., & Hauschildt, P. H. 1998, A&A, 337, 403Google Scholar
Cargile, P. A., James, D. J., & Jeffries, R. D. 2010, ApJ (Letters), 725, 111Google Scholar
Jeffries, R. D. & Naylor, T. 2011, ASPC, 243, 633Google Scholar
Morales, J. C., Ribas, I., & Jordi, C. 2008, A&A, 478, 507Google Scholar
Platais, I., Girard, T. M. and Vieira, K., Lopez, C. E., Loomis, C., McLean, B. J., Pourbaix, D., Moraux, E., Mermilliod, J.-C., James, D. J., Cargile, P. A., Barnes, S. A., & Castillo, D. J. 2011, MNRAS, 413, 1024Google Scholar
Stassun, K. G., Kratter, K. M., Scholz, A., & Dupuy, T. J. 2012, ApJ, 756, 47Google Scholar
Zapatero Osorio, M. R., Bejar, V. J. S., Pavlenko, Ya., Rebolo, R., Allende Prieto, C., Martin, E. L., & Garcia Lopez, R. J. 2002, A&A, 384, 937Google Scholar