MRI-active inner regions of protoplanetary discs – II. Dependence on dust, disc, and stellar parameters

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dc.citation.issue4
dc.citation.rankM21
dc.citation.spage5974-5991
dc.citation.volume509
dc.contributor.authorJankovic, Marija R.
dc.contributor.authorMohanty, Subhanjoy
dc.contributor.authorOwen, James E.
dc.contributor.authorTan, Jonathan C.
dc.date.accessioned2023-06-12T11:59:07Z
dc.date.available2023-06-12T11:59:07Z
dc.date.issued2021-11-24
dc.description.abstractClose-in super-Earths are the most abundant exoplanets known. It has been hypothesized that they form in the inner regions of protoplanetary discs, out of the dust that may accumulate at the boundary between the inner region susceptible to the magneto-rotational instability (MRI) and an MRI-dead zone further out. In Paper I, we presented a model for the viscous inner disc which includes heating due to both irradiation and MRI-driven accretion; thermal and non-thermal ionization; dust opacities; and dust effects on ionization. Here, we examine how the inner disc structure varies with stellar, disc, and dust parameters. For high accretion rates and small dust grains, we find that: (1) the main sources of ionization are thermal ionization and thermionic and ion emission; (2) the disc features a hot, high-viscosity inner region, and a local gas pressure maximum at the outer edge of this region (in line with previous studies); and (3) an increase in the dust-to-gas ratio pushes the pressure maximum outwards. Consequently, dust can accumulate in such inner discs without suppressing the MRI, with the amount of accumulation depending on the viscosity in the MRI-dead regions. Conversely, for low accretion rates and large dust grains, there appears to be an additional steady-state solution in which: (1) stellar X-rays become the main source of ionization; (2) MRI-viscosity is high throughout the disc; and (3) the pressure maximum ceases to exist. Hence, if planets form in the inner disc, larger accretion rates (and thus younger discs) are favoured.
dc.identifier.doi10.1093/mnras/stab3370
dc.identifier.issn0035-8711
dc.identifier.issn1365-2966
dc.identifier.scopus2-s2.0-85125130535
dc.identifier.urihttps://pub.ipb.ac.rs/handle/123456789/44
dc.identifier.wos000780137000091
dc.language.isoen
dc.publisherOxford University Press (OUP)
dc.relation.ispartofMonthly Notices of the Royal Astronomical Society
dc.rightsopenAccess
dc.titleMRI-active inner regions of protoplanetary discs – II. Dependence on dust, disc, and stellar parameters
dc.typejournal-article
dc.type.versionpublishedVersion
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