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

We have performed a pointed survey of N2D+ 2-1 and N2D+ 3-2 emission toward64 N2H+-bright starless and protostellar cores in the Perseus molecular cloudusing the Arizona Radio Observatory Submillimeter Telescope and Kitt Peak 12 mtelescope. We find a mean deuterium fractionation in N2H+, R_D =N(N2D+)/N(N2H+), of 0.08, with a maximum R_D = 0.2. In detected sources, wefind no significant difference in the deuterium fractionation between starlessand protostellar cores, nor between cores in clustered or isolatedenvironments. We compare the deuterium fraction in N2H+ with parameters linkedto advanced core evolution. We only find significant correlations between thedeuterium fraction and increased H_2 column density, as well as with increasedcentral core density, for all cores. Towards protostellar sources, weadditionally find a significant anti-correlation between R_D and bolometrictemperature. We show that the Perseus cores are characterized by low COdepletion values relative to previous studies of star forming cores, similar torecent results in the Ophiuchus molecular cloud. We suggest that the lowaverage CO depletion is the dominant mechanism that constrains the averagedeuterium fractionation in the Perseus cores to small values. While currentequilibrium and dynamic chemical models are able to reproduce the range ofdeuterium fractionation values we find in Perseus, reproducing the scatteracross the cores requires variation in parameters such as the ionizationfraction or the ortho- to para-H_2 ratio across the cloud, or a range in coreevolution timescales.

An analysis of the deuterium fractionation of star-forming cores in the Perseus molecular cloud