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

In a previous work we analysed the white-light coronal brightness as afunction of elongation and time from Wide-Field Imager (WISPR) observations onboard the Parker Solar Probe (PSP) mission when PSP reached a minimumheliocentric distance of ~ 28 Rs. We found 4-5 transient outflows per day overa narrow wedge in the PSP orbital plane, which is close to the solar equatorialplane. However, the elongation versus time map (J-map) analysis supplied onlylower limits on the number of released density structures due to the smallspatial-scales of the transient outflows and line-of-sight integration effects.In this work we place constraints on the properties of slow solar windtransient mass release from the entire solar equatorial plane. We simulated therelease and propagation of transient density structures in the solar equatorialplane for four scenarios: (1) periodic release in time and longitude withrandom speeds; (2) corotating release in longitude, periodic release in timewith random speeds; (3) random release in longitude, periodic release in timeand speed; and (4) random release in longitude, time, and speed. Thesimulations were used in the construction of synthetic J-maps, which aresimilar to the observed J-map. The four considered scenarios have similarranges (35-45 for the minimum values and 96-127 for the maximum values) ofreleased density structures per day from the solar equatorial plane andconsequently from the streamer belt, given its proximity to the solarequatorial plane during the WISPR observation. Our results also predict thatdensity structures with sizes in the range 2-8 Rs, covering 1-20 % of theperihelion could have been detectable by PSP in situ observations during thatinterval.

Constraints on the variable nature of the slow solar wind with the Wide-Field Imager on board the Parker Solar Probe