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 studied the star formation history and the initial mass function(IMF) using the age and mass derived from spectral energy distribution (SED)fitting and from color-magnitude diagrams. We also examined the physical andstructural parameters of more than 1,000 pre-main sequence stars in NGC 2264using the on-line SED fitting tool (SED fitter) of Robitaille et al.  The cumulative distribution of stellar ages showed a distinct differenceamong SFRs. The results indicate that star formation in NGC 2264 started at thesurface region (Halo and Field regions) about 6 - 7 Myr ago, propagated intothe molecular cloud and finally triggered the recent star formation in theSpokes cluster. The kind of sequential star formation that started in thelow-density surface region (Halo and Field regions) implies that star formationin NGC 2264 was triggered by an external source.  The IMF of NGC 2264 was determined in two different ways. The slope of theIMF of NGC 2264 for massive stars (log m >= 0.5) is -1.7 \pm 0.1, which issomewhat steeper than the so-called standard "Salpeter-Kroupa" IMF. We alsopresent data for 79 young brown dwarf candidates.

The Initial Mass Function and Young Brown Dwarf Candidates in NGC 2264. IV. The Initial Mass Function and Star Formation History