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A likely magnetic activity cycle for the Exoplanet Host M Dwarf GJ 3512

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dc.affiliation.dptoUC3M. Departamento de Teoría de la Señal y Comunicacioneses
dc.affiliation.grupoinvUC3M. Grupo de Investigación: Tratamiento de la Señal y Aprendizaje (GTSA)es
dc.contributor.authorLópez Santiago, Javier
dc.contributor.authorMartino, Luca
dc.contributor.authorMíguez Arenas, Joaquín
dc.contributor.authorVázquez López, Manuel Alberto
dc.contributor.funderComunidad de Madrides
dc.contributor.funderMinisterio de Ciencia e Innovación (España)es
dc.date.accessioned2022-03-18T13:21:51Z
dc.date.available2022-03-18T13:21:51Z
dc.date.issued2020-12-01
dc.description.abstractCurrent radial velocity data from specialized instruments contain a large amount of information that may pass unnoticed if their analysis is not accurate. The joint use of Bayesian inference tools and frequency analysis has been shown as effective in revealing exoplanets but they have been used less frequently to investigate stellar activity. We intend to use radial velocity data of the exoplanet host star GJ 3512 to investigate its magnetic activity. Our study includes the analysis of the photometric data available. The main objectives of our work are to constrain the orbital parameters of the exoplanets in the system, to determine the current level of activity of the star and to derive an activity cycle length for it. An adaptive importance sampling method was used to determine the parameters of the exoplanets orbit. Generalized Lomb–Scargle periodograms were constructed with both radial velocity curve and photometric data. A careful analysis of the harmonic frequencies was conducted in each periodogram. Our fit to multiple Keplerian orbits constrained the orbital parameters of two giant gas planets orbiting the star GJ 3512. The host star showed an increase of its magnetic activity during the last observing campaign. The accurate fit of the radial velocity curve data to the multi-Keplerian orbit permitted to reveal the star rotation in the residuals of the best fit and estimate an activity cycle length of ∼14 yr.en
dc.description.sponsorshipThe authors acknowledges the referee of this work for useful comments and suggestions that helped to improve the manuscript. This work was supported by the Office of Naval Research Global (N00014-19-1-2226), Spanish Ministry of Science, Innovation and Universities (RTI2018-099655-BI00), and Regional Ministry of Education and Research for the Community of Madrid (Y2018/TCS-4705).en
dc.description.statusPublicadoes
dc.format.extent11
dc.identifier.bibliographicCitationThe Astronomical Journal, (2020), 160(6): 273.en
dc.identifier.doihttps://doi.org/10.3847/1538-3881/abc171
dc.identifier.issn0004-6256
dc.identifier.publicationfirstpage273
dc.identifier.publicationissue6
dc.identifier.publicationtitleASTRONOMICAL JOURNALen
dc.identifier.publicationvolume160
dc.identifier.urihttps://hdl.handle.net/10016/34421
dc.identifier.uxxiAR/0000027334
dc.language.isoengen
dc.publisherIOP Publishingen
dc.relation.projectIDComunidad de Madrid. Y2018/TCS-4705es
dc.relation.projectIDGobierno de España. RTI2018-099655-B-I00es
dc.rights© 2020. The American Astronomical Society. All rights reserved.en
dc.rights.accessRightsopen accessen
dc.subject.ecienciaTelecomunicacioneses
dc.subject.otherStellar activityen
dc.subject.otherM dwarf starsen
dc.subject.otherExoplanet systemsen
dc.subject.otherStarspotsen
dc.subject.otherComputational methodsen
dc.subject.otherLate-type dwarf starsen
dc.subject.otherBayesian statisticsen
dc.subject.otherImportance samplingen
dc.titleA likely magnetic activity cycle for the Exoplanet Host M Dwarf GJ 3512en
dc.typeresearch article*
dc.type.hasVersionAM*
dspace.entity.typePublication
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