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Masses and Implications for Ages of Low-Mass Pre-Main Sequence Stars in Taurus and Ophiuchus

hal.structure.identifierDepartement of Physics and Astronomy [SUNY]
hal.structure.identifierAmerican Museum of Natural History [New York, USA] = Musée américain d'histoire naturelle [New York, USA] [AMNH]
dc.contributor.authorSIMON, Michal
hal.structure.identifierAMOR 2019
dc.contributor.authorGUILLOTEAU, S.
dc.contributor.authorBECK, Tracy L.
hal.structure.identifierAMOR 2019
dc.contributor.authorCHAPILLON, E.
hal.structure.identifierAMOR 2019
dc.contributor.authorDUTREY, Anne
hal.structure.identifierAMOR 2019
dc.contributor.authorDI FOLCO, E.
dc.contributor.authorFEIDEN, Gregory A.
hal.structure.identifierLaboratoire d'Astrophysique de Marseille [LAM]
dc.contributor.authorGROSSO, N.
dc.contributor.authorPRATO, L.
dc.contributor.authorSCHAEFER, Gail. H.
dc.date.issued2019
dc.identifier.issn0004-637X
dc.description.abstractEnThe accuracy of masses of pre-main sequence (PMS) stars derived from their locations on the Hertzsprung-Russell Diagram (HRD) can be tested by comparison with accurate and precise masses determined independently. We present 29 single stars in the Taurus star-forming region (SFR) and 3 in the Ophiuchus SFR with masses measured dynamically to a precision of at least $10 \%$. Our results include 9 updated mass determinations and 3 that have not had their dynamical masses published before. This list of stars with fundamental, dynamical masses, M$_{dyn}$, is drawn from a larger list of 39 targets in the Taurus SFR and 6 in the Ophiuchus SFR. Placing the stars with accurate and precise dynamical masses on HRDs that do not include internal magnetic fields underestimates the mass compared to M$_{dyn}$ by about $30 \%$. Placing them on an HRD that does include magnetic fields yields mass estimates in much better agreement with M$_{dyn}$, with an average difference between M$_{dyn}$ and the estimated track mass of $0.01\pm0.02$~\msun. The ages of the stars, 3--10 MY on tracks that include magnetic fields, is older than the 1--3 MY indicated by the non-magnetic models. The older ages of T Tauri stars predicted by the magnetic models increase the time available for evolution of their disks and formation of the giant gas exoplanets. The agreement between our M$_{dyn}$ values and the masses on the magnetic field tracks provides indirect support for these older ages.
dc.language.isoen
dc.publisherAmerican Astronomical Society
dc.subject.enAstrophysics - Solar and Stellar Astrophysics
dc.subject.enAstrophysics - Astrophysics of Galaxies
dc.title.enMasses and Implications for Ages of Low-Mass Pre-Main Sequence Stars in Taurus and Ophiuchus
dc.typeArticle de revue
dc.identifier.doi10.3847/1538-4357/ab3e3b
dc.subject.halPlanète et Univers [physics]/Astrophysique [astro-ph]/Cosmologie et astrophysique extra-galactique [astro-ph.CO]
dc.identifier.arxiv1908.10952
bordeaux.journalThe Astrophysical Journal
bordeaux.pageid. 42
bordeaux.volume884
bordeaux.issue1
bordeaux.peerReviewedoui
hal.identifierhal-02282440
hal.version1
hal.popularnon
hal.audienceInternationale
hal.origin.linkhttps://hal.archives-ouvertes.fr//hal-02282440v1
bordeaux.COinSctx_ver=Z39.88-2004&rft_val_fmt=info:ofi/fmt:kev:mtx:journal&rft.jtitle=The%20Astrophysical%20Journal&rft.date=2019&rft.volume=884&rft.issue=1&rft.spage=id.%2042&rft.epage=id.%2042&rft.eissn=0004-637X&rft.issn=0004-637X&rft.au=SIMON,%20Michal&GUILLOTEAU,%20S.&BECK,%20Tracy%20L.&CHAPILLON,%20E.&DUTREY,%20Anne&rft.genre=article


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