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dc.contributor.author
Messina, S.
dc.contributor.author
Lanzafame, A. C.
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Malo, L.
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Desidera, S.
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Buccino, Andrea Paola
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Zhang, L.
dc.contributor.author
Artemenko, S.
dc.contributor.author
Millward, M.
dc.contributor.author
Hambsch, F.-J.
dc.date.available
2018-10-31T17:20:18Z
dc.date.issued
2017-11
dc.identifier.citation
Messina, S.; Lanzafame, A. C.; Malo, L.; Desidera, S.; Buccino, Andrea Paola; et al.; The β Pictoris association low-mass members: Membership assessment, rotation period distribution, and dependence on multiplicity; EDP Sciences; Astronomy and Astrophysics; 607; A3; 11-2017; 1-17
dc.identifier.issn
0004-6361
dc.identifier.uri
http://hdl.handle.net/11336/63388
dc.description.abstract
Context. Low-mass members of young loose stellar associations and open clusters exhibit a wide spread of rotation periods. Such a spread originates from the distributions of masses and initial rotation periods. However, multiplicity can also play a significant role. Aims. We aim to investigate the role played by physical companions in multiple systems in shortening the primordial disk lifetime, anticipating the rotation spin up with respect to single stars. Methods. We have compiled the most extensive list to date of low-mass bona fide and candidate members of the young 25-Myr β Pictoris association. We have measured from our own photometric time series or from archival time series the rotation periods of almost all members. In a few cases the rotation periods were retrieved from the literature. We used updated UVWXYZ components to assess the membership of the whole stellar sample. Thanks to the known basic properties of most members we built the rotation period distribution distinguishing between bona fide members and candidate members and according to their multiplicity status. Results. We find that single stars and components of multiple systems in wide orbits (>80 AU) have rotation periods that exhibit a well defined sequence arising from mass distribution with some level of spread likely arising from initial rotation period distribution. All components of multiple systems in close orbits (<80 AU) have rotation periods that are significantly shorter than their equal-mass single counterparts. For these close components of multiple systems a linear dependence of rotation rate on separation is only barely detected. A comparison with the younger 13 Myr h Per cluster and with the older 40-Myr open clusters and stellar associations NGC 2547, IC 2391, Argus, and IC 2602 and the 130-Myr Pleiades shows that whereas the evolution of F-G stars is well reproduced by angular momentum evolution models, this is not the case for the slow K and early-M stars. Finally, we find that the amplitude of their light curves is correlated neither with rotation nor with mass. Conclusions. Once single stars and wide components of multiple systems are separated from close components of multiple systems, the rotation period distributions exhibit a well defined dependence on mass that allows us to make a meaningful comparison with similar distributions of either younger or older associations and clusters. Such cleaned distributions allow us to use the stellar rotation period meaningfully as an age indicator for F and G type stars.
dc.format
application/pdf
dc.language.iso
eng
dc.publisher
EDP Sciences
dc.rights
info:eu-repo/semantics/openAccess
dc.rights.uri
https://creativecommons.org/licenses/by-nc-sa/2.5/ar/
dc.subject
Binaries: Close
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Open Clusters And Associations: Individual: ΒPictoris
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Stars: Activity
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Stars: Late-Type
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Stars: Rotation
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Starspots
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Astronomía
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Ciencias Físicas
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CIENCIAS NATURALES Y EXACTAS
dc.title
The β Pictoris association low-mass members: Membership assessment, rotation period distribution, and dependence on multiplicity
dc.type
info:eu-repo/semantics/article
dc.type
info:ar-repo/semantics/artículo
dc.type
info:eu-repo/semantics/publishedVersion
dc.date.updated
2018-10-23T18:11:22Z
dc.journal.volume
607
dc.journal.number
A3
dc.journal.pagination
1-17
dc.journal.pais
Francia
dc.journal.ciudad
Paris
dc.description.fil
Fil: Messina, S.. Osservatorio Astrofisico Di Catania; Italia
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Fil: Lanzafame, A. C.. Universita Degli Studi Di Catania; Italia
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Fil: Malo, L.. Canada France Hawaii Telescope Corporation; Canadá
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Fil: Desidera, S.. Osservatorio Astronomico Di Padova; Italia
dc.description.fil
Fil: Buccino, Andrea Paola. Universidad de Buenos Aires; Argentina. Consejo Nacional de Investigaciónes Científicas y Técnicas. Oficina de Coordinación Administrativa Ciudad Universitaria. Instituto de Astronomía y Física del Espacio. - Universidad de Buenos Aires. Facultad de Ciencias Exactas y Naturales. Instituto de Astronomía y Física del Espacio; Argentina
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Fil: Zhang, L.. Guizhou University; China
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Fil: Artemenko, S.. Crimean Astrophysical Observatory; Australia
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Fil: Millward, M.. York Creek Observatory Georgetown; Australia
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Fil: Hambsch, F.-J.. American Association Of Variable Star Observers; Estados Unidos
dc.journal.title
Astronomy and Astrophysics
dc.relation.alternativeid
info:eu-repo/semantics/altIdentifier/doi/http://dx.doi.org/10.1051/0004-6361/201730444
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