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

(abridged) The star formation rate (SFR) linearly correlates with the amountof dense gas mass (Mdg) involved in the formation of stars both for distantgalaxies and clouds in our Galaxy. Similarly, the mass accretion rate (Macc)and the disk mass (Mdisk) of young, Class II stars are also linearlycorrelated. We plotted the corresponding observational data together, finding astatistically significant correlation that spans ~ 16 orders of magnitude. Thisprobably represents one of the widest ranges of any empirical correlationknown, encompassing galaxies that are several kpc in size, pc-size star-formingclouds within our Galaxy, down to young, pre-main sequence stars with au-sizeprotoplanetary disks. We propose a bottom-up hypothesis suggesting that arelation between Macc and the total circumstellar mass surrounding Class 0/Isources (Mcs; disk+envelope) drives the correlation in protostellar-hostingclouds and cloud-hosting galaxies. This is consistent with the fact that theSFRs derived for clouds over a timescale of 2 Myr can be roughly recovered fromthe sum of instantaneous Macc values of the protostars embedded within them,implying that galactic SFRs averaged over ~ 10-100 Myr should be constant overthis period too. Moreover, the sum of the Mcs values directly participating inthe formation of the protostellar population in a cloud likely represents anon-negligible fraction of the Mdg within the cloud. If such fraction is ~1-35% of the Mdg associated with star-forming clouds and galaxies, then theglobal correlation for all scales has a near unity slope and an interceptconsistent with the (proto-)stellar accretion timescale, Mcs/Macc. Therefore,an additional critical test of our hypothesis is that the Macc-Mdiskcorrelation for Class II stars should also be observed between Macc and Mcs forClass 0/I sources with similar slope and intercept.

A global correlation linking young stars, clouds, and galaxies. Towards a unified view of star formation