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 Tools annual

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 monthly

Global: Zendy Plus monthly

Presents the access of premium content as premium feature

Premium Content

Global: Zendy Plus annual

Global: Zendy Free Plan

We present a statistical study of the filamentary structure orientation inthe CO emission observations obtained in the Milky Way Imaging Scroll Painting(MWISP) survey in the range $25.8\deg < l < 49.7\deg$, $|b| \leq 1.25\deg$, and$-100 < v_{\rm LSR} < 135$ km/s. We found that most of the filamentarystructures in the $^{12}$CO and $^{13}$CO emission do not show a globalpreferential orientation either parallel or perpendicular to the Galacticplane. However, we found ranges in Galactic longitude and radial velocity wherethe $^{12}$CO and $^{13}$CO filamentary structures are parallel to the Galacticplane. These preferential orientations are different from those found for theHI emission. We consider this an indication that the molecular structures donot simply inherit these properties from parental atomic clouds. Instead, theyare shaped by local physical conditions, such as stellar feedback, magneticfields, and Galactic spiral shocks.

The filamentary structures in the CO emission toward the Milky Way disk