Is the $\beta$ Pictoris member GJ3039AB a physical binary? What the rotation periods tell us

Abstract

We have carried out a multi-band photometric monitoring of the close visual binary GJ3039, consisting of a M4 primary and a fainter secondary component, and likely member of the young stellar association $\beta$ Pictoris (24-Myr old). From our analysis we found that both components are photometric variables and, for the first time, we detected two micro-flare events. We measured from periodogram analysis of the photometric time series two rotation periods P = 3.355d and P = 0.925d, that we could attribute to the brighter GJ3039A and the fainter GJ3039B components, respectively. A comparison of these rotation periods with the period distribution of other $\beta$ Pictoris members further supports that GJ3039A is a member of this association. We find that also GJ3039B could be a member, but the infrared magnitude differences between the two components taken from the literature and the photometric variability, which is found to be comparable in both stars, suggest that GJ3039B could be a foreground star physically unbound to the primary A component.

Accepted by New Astronomy; 17 pages, 5 figures

References in corpus (2)

• Evidence from stellar rotation of enhanced disc dispersal: (I) The case of the triple visual system BD-21 1074 in the $\beta$ Pictoris association
• The visual binary AG Tri in $\beta$ Pictoris Association: can a debris disc cause very different rotation periods of its components?

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• Exploring the short-term variability of H$\alpha$ and H$\beta$ emissions in a sample of M dwarfs