English (United Kingdom)

https://curated-unify.zendy.io/wp-json/zendy-region/v1/featured_content/oa?rat=en

https://curated-unify.zendy.io/wp-json/zendy-region/v1/highlighted_journal/

Global: Zendy Plus annual

Presents the access of premium content as premium feature

Premium Content

Presents the keyphrase highlighting as premium feature

Keyphrase Highlighting

Presents the summarisation as premium feature

Summarisation

Insights

Presents the pdf analysis as premium feature

PDF Analysis

Presents the zaia usage as premium feature

ZAIA

Global: Zendy Plus monthly

Global: Zendy Tools annual

Global: Zendy Tools monthly

Global: Zendy Free Plan

It has been suggested that $\beta$ Pic b has a supersolar metallicity andsubsolar C/O ratio. Assuming solar carbon and oxygen abundances for the star$\beta$ Pic and therefore the planet's parent protoplanetary disk, $\beta$ Picb's C/O ratio suggests that it formed via core accretion between its parentprotoplanteary disk's H$_{2}$O and CO$_{2}$ ice lines. $\beta$ Pic b's highmetallicity is difficult to reconcile with its mass$M_{\text{p}}~=~11.7~M_{\text{Jup}}$ though. Massive stars can present peculiarphotospheric abundances that are unlikely to record the abundances of theirformer protoplanetary disks. This issue can be overcome for early-type stars inmoving groups by infering the elemental abundances of the FGK stars in the samemoving group that formed in the same molecular cloud and presumably share thesame composition. We infer the photospheric abundances of the F dwarf HD181327, a $\beta$ Pic moving group member that is the best available proxy forthe composition of $\beta$ Pic b's parent protoplanetary disk. In parallel, weinfer updated atmospheric abundances for $\beta$ Pic b. As expected for aplanet of its mass formed via core-accretion beyond its parent protoplanetarydisk's H$_{2}$O ice line, we find that $\beta$ Pic b's atmosphere is consistentwith stellar metallicity and confirm that is has superstellar carbon and oxygenabundances with a substellar C/O ratio. We propose that the elementalabundances of FGK dwarfs in moving groups can be used as proxies for theotherwise difficult-to-infer elemental abundances of early-type and late-typemembers of the same moving groups.

Insight into the Formation of $\beta$ Pic b through the Composition of  Its Parent Protoplanetary Disk as Revealed by the $\beta$ Pic Moving Group  Member HD 181327