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Activity and Rotation in the Young Cluster h Per

Published online by Cambridge University Press:  07 August 2014

C. Argiroffi ,
M. Caramazza ,
G. Micela ,
E. Moraux  and
J. Bouvier
C. Argiroffi
Affiliation:
Dip. di Fisica e Chimica, Università di Palermo, Piazza del Parlamento 1, 90134 Palermo, Italy, email: argi@astropa.unipa.it 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.

Keywords

DynamoStars: activityStars: pre-main sequenceX-rays: stars

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