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 Tools annual

Global: Zendy Free Plan

Global: Zendy Tools monthly

Global: Zendy Plus monthly

The deuterium enrichment of molecules is sensitive to their formationenvironment. Constraining patterns of deuterium chemistry in protoplanetarydisks is therefore useful for probing how material is inherited or reprocessedthroughout the stages of star and planet formation. We present ALMAobservations at $\sim0.6"$ resolution of DCO$^+$, H$^{13}$CO$^+$, DCN, andH$^{13}$CN in the full disks around T Tauri stars AS 209 and IM Lup, thetransition disks around T Tauri stars V4046 Sgr and LkCa 15, and the full disksaround Herbig Ae stars MWC 480 and HD 163296. We also present ALMA observationsof HCN in the IM Lup disk. DCN, DCO$^+$, and H$^{13}$CO$^+$ are detected in alldisks, and H$^{13}$CN in all but the IM Lup disk. We find efficient deuteriumfractionation for the sample, with estimates of disk-averaged DCO$^+$/HCO$^+$and DCN/HCN abundance ratios ranging from $\sim0.02-0.06$ and $\sim0.005-0.08$,respectively, which is comparable to values reported for other ISMenvironments. The relative distributions of DCN and DCO$^+$ vary between disks,suggesting that multiple formation pathways may be needed to explain thediverse emission morphologies. In addition, gaps and rings observed in bothH$^{13}$CO$^+$ and DCO$^+$ emission provide new evidence that DCO$^+$ bears acomplex relationship with the location of the midplane CO snowline.

An ALMA survey of DCN/H$^{13}$CN and DCO$^+$/H$^{13}$CO$^+$ in protoplanetary disks