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dc.contributor.authorVeyette, Mark J.en_US
dc.contributor.authorMuirhead, Philip S.en_US
dc.contributor.authorMann, Andrew W.en_US
dc.contributor.authorAllard, Franceen_US
dc.date.accessioned2017-06-01T20:14:41Z
dc.date.available2017-06-01T20:14:41Z
dc.date.issued2016-09-07
dc.identifier.citationMJ Veyette, PS Muirhead, AW Mann, F Allard. 2016. "The physical mechanism behind M dwarf metallicity indicators and the role of C and O abundances." The Astrophysical Journal, Volume 828, Issue 2, pp. 95 - ?.
dc.identifier.issn0004-637X
dc.identifier.urihttps://hdl.handle.net/2144/22290
dc.description.abstractWe present near-infrared (NIR) synthetic spectra based on PHOENIX stellar atmosphere models of typical early and mid-M dwarfs with varied C and O abundances. We apply multiple recently published methods for determining M dwarf metallicity to our models to determine the effects of C and O abundances on metallicity indicators. We find that the pseudo-continuum level is very sensitive to C/O and that all metallicity indicators show a dependence on C and O abundances, especially in lower T eff models. In some cases, the inferred metallicity ranges over a full order of magnitude (>1 dex) when [C/Fe] and [O/Fe] are varied independently by ±0.2. We also find that [(O−C)/Fe], the difference in O and C abundances, is a better tracer of the pseudo-continuum level than C/O. Models of mid-M dwarfs with [C/Fe], [O/Fe], and [M/H] that are realistic in the context of galactic chemical evolution suggest that variation in [(O−C)/Fe] is the primary physical mechanism behind the M dwarf metallicity tracers investigated here. Empirically calibrated metallicity indicators are still valid for most nearby M dwarfs due to the tight correlation between [(O−C)/Fe] and [Fe/H] evident in spectroscopic surveys of solar neighborhood FGK stars. Variations in C and O abundances also affect the spectral energy distribution of M dwarfs. Allowing [O/Fe] to be a free parameter provides better agreement between the synthetic spectra and observed spectra of metal-rich M dwarfs. We suggest that flux-calibrated, low-resolution, NIR spectra can provide a path toward measuring C and O abundances in M dwarfs and breaking the degeneracy between C/O and [Fe/H] present in M dwarf metallicity indicators.en_US
dc.format.extent95 - ?en_US
dc.publisherIOP Publishingen_US
dc.relation.ispartofThe Astrophysical Journal
dc.rights© 2016 American Astronomical Societyen_US
dc.subjectAstronomical and space sciencesen_US
dc.subjectOrganic chemistryen_US
dc.subjectSolar and stellar astrophysicsen_US
dc.subjectAstronomy & astrophysicsen_US
dc.subjectBrown dwarf starsen_US
dc.titleThe physical mechanism behind M dwarf metallicity indicators and the role of C and O abundancesen_US
dc.typeArticleen_US
dc.identifier.doi10.3847/0004-637X/828/2/95
pubs.elements-sourcemanual-entryen_US
pubs.notesEmbargo: No embargoen_US
pubs.organisational-groupBoston Universityen_US
pubs.organisational-groupBoston University, College of Arts & Sciencesen_US
pubs.organisational-groupBoston University, College of Arts & Sciences, Department of Astronomyen_US
dc.identifier.orcid0000-0002-0638-8822 (Muirhead, PS)


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