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

Motivated by the unknown nature of the $2.50-2.67\,M_\odot$ compact object inthe binary merger event GW190814, we study the maximum neutron star mass basedon constraints from low-energy nuclear physics, neutron star tidaldeformabilities from GW170817, and simultaneous mass-radius measurements of PSRJ0030+045 from NICER. Our prior distribution is based on a combination ofnuclear modeling valid in the vicinity of normal nuclear densities togetherwith the assumption of a maximally stiff equation of state at high densities, achoice that enables us to probe the connection between observed heavy neutronstars and the transition density at which conventional nuclear physics modelsmust break down. We demonstrate that a modification of the highly uncertainsupra-saturation density equation of state beyond 2.64 times normal nucleardensity is required in order for chiral effective field theory models to beconsistent with current neutron star observations and the existence of$2.6\,M_\odot$ neutron stars. We also show that the existence of very massiveneutron stars strongly impacts the radii of $\sim 2.0\,M_\odot$ neutron stars(but not necessarily the radii of $1.4\,M_\odot$ neutron stars), which furthermotivates future NICER radius measurements of PSR J1614-2230 and PSRJ0740+6620.

Radius and equation of state constraints from massive neutron stars and GW190814