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

Observations of pulsars in globular clusters (GCs) give evidence that more>10-20% of neutron stars (NSs) ever formed in GCs were retained there. However,the velocity distribution of field pulsars peaks at 5-10 times the escapevelocities of GCs. Consequently, only a small fraction of GC-NSs should havebeen retained, even accounting for low-velocity NSs formed throughelectron-capture supernovae. Thus, too few low-velocity NSs should have beenretained in GCs, giving rise to the NS retention problem in GCs. Here wesuggest a novel solution, in which the progenitors of most GC-NSs were ONewhite-dwarfs (WDs) that accreted ambient intra-cluster gas and formedlow-velocity NSs through accretion induced collapse (AIC). The existence of anearly gas-enriched environment in GCs is supported by observations of GCmultiple stellar populations. It is thought that 10s-100s of Myrs after theformation of the first generation of stars, and after ONe-WDs were alreadyformed, GCs were replenished with gas which formed a second generation ofstars. Accretion of such replenished gas onto the ONe-WDs catalyzed the AICprocesses. The number of AIC-formed NSs is then sufficient to explain the largenumber of NSs retained in GCs. Similar processes might also drive CO-WDs toproduce type-Ia SNe or to merge and form NSs, and similarly drive NSs to AICand mergers producing BHs. Moreover, the wide variety of gas-catalyzed binarymergers and explosive transients suggest to occur in the gas-rich environmentsof AGN disk could similarly, and even more efficiently, occur insecond-generation gas in GCs.

Compact objects formation, retention, and growth through accretion onto gas-embedded white-dwarfs/neutron-stars in gas-enriched globular-clusters