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Activity and Rotation in the Young Cluster h Per

Published online by Cambridge University Press:  07 August 2014

C. Argiroffi
Affiliation:
Dip. di Fisica e Chimica, Università di Palermo, Piazza del Parlamento 1, 90134 Palermo, Italy, email: [email protected] INAF - Osservatorio Astronomico di Palermo, Piazza del Parlamento 1, 90134 Palermo, Italy
M. Caramazza
Affiliation:
INAF - Osservatorio Astronomico di Palermo, Piazza del Parlamento 1, 90134 Palermo, Italy
G. Micela
Affiliation:
INAF - Osservatorio Astronomico di Palermo, Piazza del Parlamento 1, 90134 Palermo, Italy
E. Moraux
Affiliation:
UJF-Grenoble 1/CNRS-INSU, Institut de Plantologie et d'Astrophysique de Grenoble (IPAG) UMR 5274, Grenoble, F-38041, France
J. Bouvier
Affiliation:
UJF-Grenoble 1/CNRS-INSU, Institut de Plantologie et d'Astrophysique de Grenoble (IPAG) UMR 5274, Grenoble, F-38041, France
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Abstract

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We study the rotation-activity relationship for low-mass members of the young cluster h Persei, a ~13 Myr old cluster. h Per, thanks to its age, allows us to link the rotation-activity relation observed for main-sequence stars to the still unexplained activity levels of very young clusters.

We constrained the activity levels of h Per members by analyzing a deep Chandra/ACIS-I observation pointed to the central field of h Per. We combined this X-ray catalog with the catalog of h Per members with measured rotational period, presented by Moraux et al. (2013). We obtained a final catalog of 202 h Per members with measured X-ray luminosity and rotational period. We investigate the rotation-activity relation of h Per members considering different mass ranges. We find that stars with 1.3 M > M 1.4 M show significant evidence of supersaturation for short periods. This phenomenon is instead not observed for lower mass stars.

Type
Contributed Papers
Copyright
Copyright © International Astronomical Union 2014 

References

Currie, T., Hernandez, J., Irwin, J., et al. 2010, ApJS, 186, 191Google Scholar
Moraux, E., Artemenko, S., Bouvier, J., et al. 2013, A&A, in pressGoogle Scholar
Noyes, R. W., Hartmann, L. W., Baliunas, S. L., Duncan, D. K., & Vaughan, A. H. 1984, ApJ, 279, 763Google Scholar
Pallavicini, R., Golub, L., Rosner, R., et al. 1981, ApJ, 248, 279Google Scholar
Pizzolato, N., Maggio, A., Micela, G., Sciortino, S., & Ventura, P. 2003, A&A, 397, 147Google Scholar
Preibisch, T., Kim, Y.-C., Favata, F., et al. 2005, ApJS, 160, 401Google Scholar
Randich, S., Schmitt, J. H. M. M., Prosser, C. F., & Stauffer, J. R. 1996, A&A, 305, 785Google Scholar
Siess, L., Dufour, E., & Forestini, M. 2000, A&A, 358, 593Google Scholar
Wright, N. J., Drake, J. J., Mamajek, E. E., & Henry, G. W. 2011, ApJ, 743, 48Google Scholar