Molecules with ALMA at Planet-forming Scales (MAPS). VII. Substellar O/H and C/H and Superstellar C/O in Planet-feeding Gas

Simple item page
dc.contributor.authorBosman, Arthur D.
dc.contributor.authorAlarcon, Felipe
dc.contributor.authorBergin, Edwin A.
dc.contributor.authorZhang, Ke
dc.contributor.authorVan't Hoff, Merel L. R.
dc.contributor.authorOberg, Karin I.
dc.contributor.authorGuzman, Viviana V.
dc.contributor.authorWalsh, Catherine
dc.contributor.authorAikawa, Yuri
dc.contributor.authorAndrews, Sean M.
dc.contributor.authorBergner, Jennifer B.
dc.contributor.authorBooth, Alice S.
dc.contributor.authorCataldi, Gianni
dc.contributor.authorCleeves, L. Ilsedore
dc.contributor.authorCzekala, Ian
dc.contributor.authorFuruya, Kenji
dc.contributor.authorHuang, Jane
dc.contributor.authorIlee, John D.
dc.contributor.authorLaw, Charles J.
dc.contributor.authorLe Gal, Romane
dc.contributor.authorLiu, Yao
dc.contributor.authorLong, Feng
dc.contributor.authorLoomis, Ryan A.
dc.contributor.authorMenard, Francois
dc.contributor.authorNomura, Hideko
dc.contributor.authorQi, Chunhua
dc.contributor.authorSchwarz, Kamber R.
dc.contributor.authorTeague, Richard
dc.contributor.authorTsukagoshi, Takashi
dc.contributor.authorYamato, Yoshihide
dc.contributor.authorWilner, David J.
dc.date.accessioned2025-01-20T22:05:36Z
dc.date.available2025-01-20T22:05:36Z
dc.date.issued2021
dc.description.abstractThe elemental composition of the gas and dust in a protoplanetary disk influences the compositions of the planets that form in it. We use the Molecules with ALMA at Planet-forming Scales (MAPS) data to constrain the elemental composition of the gas at the locations of potentially forming planets. The elemental abundances are inferred by comparing source-specific gas-grain thermochemical models with variable C/O ratios and small-grain abundances from the DALI code with CO and C2H column densities derived from the high-resolution observations of the disks of AS 209, HD 163296, and MWC 480. Elevated C/O ratios (similar to 2.0), even within the CO ice line, are necessary to match the inferred C2H column densities over most of the pebble disk. Combined with constraints on the CO abundances in these systems, this implies that both the O/H and C/H ratios in the gas are substellar by a factor of 4-10, with the O/H depleted by a factor of 20-50, resulting in the high C/O ratios. This necessitates that even within the CO ice line, most of the volatile carbon and oxygen is still trapped on grains in the midplane. Planets accreting gas in the gaps of the AS 209, HD 163296, and MWC 480 disks will thus acquire very little carbon and oxygen after reaching the pebble isolation mass. In the absence of atmosphere-enriching events, these planets would thus have a strongly substellar O/H and C/H and superstellar C/O atmospheric composition. This paper is part of the MAPS special issue of the Astrophysical Journal Supplement.
dc.fuente.origenWOS
dc.identifier.doi10.3847/1538-4365/ac1435
dc.identifier.eissn1538-4365
dc.identifier.issn0067-0049
dc.identifier.urihttps://doi.org/10.3847/1538-4365/ac1435
dc.identifier.urihttps://repositorio.uc.cl/handle/11534/94154
dc.identifier.wosidWOS:000714217500001
dc.issue.numero1
dc.language.isoen
dc.revistaAstrophysical journal supplement series
dc.rightsacceso restringido
dc.titleMolecules with ALMA at Planet-forming Scales (MAPS). VII. Substellar O/H and C/H and Superstellar C/O in Planet-feeding Gas
dc.typeartículo
dc.volumen257
sipa.indexWOS
sipa.trazabilidadWOS;2025-01-12
Files
Collections
Artículos de revistas