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YaPSI: a new database of evolutionary tracks and isochrones

Published online by Cambridge University Press:  02 August 2018

F. Spada Open the ORCID record for F. Spada [Opens in a new window] ,
P. Demarque ,
Y. -C. Kim ,
T. S. Boyajian  and
J. M. Brewer
F. Spada
Affiliation:
Leibniz-Institut für Astrophysik Potsdam (AIP), Germany email: fspada@aip.de
P. Demarque
Affiliation:
Department of Astronomy, Yale University, USA
Y. -C. Kim
Affiliation:
Yonsei University Observatory and Astronomy Department, Korea
T. S. Boyajian
Affiliation:
Department of Astronomy, Yale University, USA Physics and Astronomy, Louisiana State University, USA
J. M. Brewer
Affiliation:
Department of Astronomy, Yale University, USA
Rights & Permissions [Opens in a new window]

Abstract

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The Yale–Potsdam Stellar Isochrones (YaPSI) cover the low and intermediate stellar mass regime (0.15 to 5.0 M⊙) for a wide range of solar-scaled chemical compositions (metallicity from −0.5 to +0.3; helium mass fraction from 0.25 to 0.37, assigned independently of each other). The tracks are finely spaced in mass, to allow for accurate interpolation. The models feature state-of-the-art input physics relevant to low-mass stars modeling (surface boundary conditions, equation of state), thus updating the faint end of the Yonsei-Yale (YY) isochrones. Utility codes, such as an isochrone interpolator in age, metallicity and helium content, are also provided. The YaPSI isochrones are in good agreement with the empirical mass–luminosity and mass–radius relations available to date, and provide satisfactory fitting of the color-magnitude diagrams of well-studied open clusters.

Keywords

HR diagramstars: evolutionstars: fundamental parametersstars: low-mass
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 13 , Symposium S334: Rediscovering our Galaxy , July 2017 , pp. 362 - 363
Copyright
Copyright © International Astronomical Union 2018 

References

Benedict, G. F., Henry, T. J., Franz, O. G., et al. 2016, AJ, 152, 141Google Scholar
Brogaard, K., VandenBerg, D. A., Bruntt, H., et al. 2012, A&A, 543, A106Google Scholar
Feiden, G. A. & Chaboyer, B., 2012, ApJ, 757, 42Google Scholar
Lejeune, T., Cuisinier, F., & Buser, R., 1998, A&AS, 130, 65Google Scholar
Newton, E. R., Irwin, J., Charbonneau, D., et al. 2016, ApJ, 821, 93Google Scholar
Shields, A. L., Ballard, S., & Johnson, J. A., 2016, Physics Reports, 663, 1Google Scholar
Spada, F., Demarque, P., Kim, Y.-C., & Sills, A., 2013, ApJ, 776, 87Google Scholar
Spada, F., Demarque, P., Kim, Y.-C., Boyajian, T. S., & Brewer, J. M. 2017, ApJ, 838, 161Google Scholar
Stetson, P. B., Hesser, J. E., Smith, G. H., Vandenberg, D. A., & Bolte, M., 1989, AJ, 97, 1360Google Scholar
Worthey, G. & Lee, H.-C., 2011, ApJS, 193, 1Google Scholar
Yi, S., Demarque, P., Kim, Y.-C., et al. 2001, ApJS, 136, 417Google Scholar