J/A+A/661/A101ivo://CDS.VizieR/J/A+A/661/A101doi:10.26093/cds/vizier.36610101CDSRodriguez-Mozos J.M.Moya A.2023-07-03T13:25:52Z2022-09-30T14:32:07ZCDS support team

CDS, Observatoire de Strasbourg, 11 rue de l'Universite, F-67000 Strasbourg, France

cds-question@unistra.frmultiple-starsexoplanetsmagnetic-fieldsFor a planet to be considered habitable on its surface, it is an important advantage for it to have a magnetic field that protects its atmosphere from stellar winds as well as cosmic rays. The magnetic protection of potentially habitable planets plays a key role in determining the chances of detecting atmospheric biosignatures. In making an estimate of a planet's magnetic field, its internal structure must first be known. This study proposes to use the Preliminary Reference Earth Model (PREM) internal structure as the base of a numerical model, as it is considered the best available option for estimating the internal structure of rocky exoplanets. With this model, we estimate the magnetic properties of dry and water-rich Earth-like and Super-Earth-like planets and we apply it to the first 176 planets of this kind confirmed by the Transiting Exoplanet Survey Satellite exoplanet mission (TESS). Using PREM as a reference, we estimated the internal structure of dry and water-rich rocky planets. This model provides an estimation of the average density and core size of the planet, which are the key ingredients for estimating its magnetic moment, depending on whether it is tidally locked or not. Our model estimates the thermodynamic variables as a function of pressure and including saltwater as a component of water-rich exoplanets. In addition, we did not use the perfect layer differentiation approximation. We validated our model based on the selection of planets and satellites in the Solar System with similar characteristics. Using our model, we estimated the internal structure and magnetic moment of selected dry and water-rich rocky planets and satellites in the Solar system. The differences with the observed values in the internal structure characteristics, mass, average density, moment of inertia factor, and local Rossby number are remarkably low or even negligible. The estimated magnetic moments are also very similar to the observed ones. We applied the model to the first dry and water-rich rocky planets confirmed by TESS, 176 in total, and we find, from an astrobiological perspective, that TOI-700 d and TOI-2257 b are the most interesting examples, as they are located in the habitable zone. However, we note that their magnetic moments are only about 0.01 of the Earth's magnetic moment.2022A&A...661A.101Rhttps://cdsarc.cds.unistra.fr/viz-bin/cat/J/A+A/661/A101CatalogResearchIsServedByTAP VizieR generic serviceIsServedByConesearch servicehttps://cds.unistra.fr/vizier-org/licences_vizier.htmlhttps://vizier.cds.unistra.fr/viz-bin/VizieR-2?-source=J/A+A/661/A101https://vizier.iucaa.in/viz-bin/VizieR-2?-source=J/A+A/661/A101http://vizieridia.saao.ac.za/viz-bin/VizieR-2?-source=J/A+A/661/A101https://vizier.cds.unistra.fr/viz-bin/votable?-source=J/A+A/661/A101https://vizier.iucaa.in/viz-bin/votable?-source=J/A+A/661/A101http://vizieridia.saao.ac.za/viz-bin/votable?-source=J/A+A/661/A101GETtext/xml+votablehttps://tapvizier.cds.unistra.fr/TAPVizieR/tapCone search capability for table J/A+A/661/A101/tableb3 (Results for dry rocky planets observed by TESS after 30,000 runs (Monte Carlo method))https://vizier.cds.unistra.fr/viz-bin/conesearch/J/A+A/661/A101/tableb3?https://vizier.iucaa.in/viz-bin/conesearch/J/A+A/661/A101/tableb3?http://vizieridia.saao.ac.za/viz-bin/conesearch/J/A+A/661/A101/tableb3?GETtext/xml+votable180.050000true306.9253392-56.45698810.005555555555555556Cone search capability for table J/A+A/661/A101/tableb4 (Results for water-rich rocky planets observed by TESS after 30,000 runs (Monte Carlo method))https://vizier.cds.unistra.fr/viz-bin/conesearch/J/A+A/661/A101/tableb4?https://vizier.iucaa.in/viz-bin/conesearch/J/A+A/661/A101/tableb4?http://vizieridia.saao.ac.za/viz-bin/conesearch/J/A+A/661/A101/tableb4?GETtext/xml+votable180.050000true51.7467619-63.49910060.0055555555555555566/1585 1793 3900 6217 7487 7605 10491 11923 12195 15629 16014 16162 16258 16347 16472 16551 20667 21986 24587 25312 26768 27358 32848 32918 33210 33212 33972 34005 34423 34561 35696 35985 36015 36614 37453 37548 38456 39080 40220 40250 41786 43525 43580 43631 45372 45527 45964 46128https://cdsarc.cds.unistra.fr/viz-bin/moc/J/A+A/661/A101?format=asciidefaultJ/A+A/661/A101/tableb3Results for dry rocky planets observed by TESS after 30,000 runs (Monte Carlo method)SimbadNameSimbad column added by the CDSmeta.idcharnullablerecnoRecord number assigned by the VizieR team. 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Ice mass fraction error (only in tableb4.dat)stat.errorfloatnullableRollocal Rossby numberstat.paramfloate_Rollocal Rossby number errorstat.errorfloatRegimeRegime (Dipolar or Multiple)meta.codecharMMagnetic moment (in Earth magnetic moment unit)Earthphys.magFieldfloate_MMagnetic moment error (in Earth magnetic moment unit)Earthstat.errorfloat_RARight Ascension (J2000) from SIMBAD (not part of the original data)degpos.eq.ra;meta.main_DEDeclination (J2000) from SIMBAD (not part of the original data)degpos.eq.dec;meta.mainNameExoplanet designationmeta.id;meta.maincharS:OSpin:Orbit resonancesrc.orbitalchar