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

Despite its importance to our understanding of physics at supranucleardensities, the equation of state (EoS) of matter deep within neutron starsremains poorly understood. Millisecond pulsars (MSPs) are among the most usefulastrophysical objects in the Universe for testing fundamental physics, andplace some of the most stringent constraints on this high-density EoS. Pulsartiming - the process of accounting for every rotation of a pulsar over longtime periods - can precisely measure a wide variety of physical phenomena,including those that allow the measurement of the masses of the components of apulsar binary system (Lorimer & Kramer 2005). One of these, called relativisticShapiro delay (Shapiro 1964), can yield precise masses for both an MSP and itscompanion; however, it is only easily observed in a small subset ofhigh-precision, highly inclined (nearly edge-on) binary pulsar systems. Bycombining data from the North American Nanohertz Observatory for GravitationalWaves (NANOGrav) 12.5-year data set with recent orbital-phase-specificobservations using the Green Bank Telescope, we have measured the mass of theMSP J0740+6620 to be $\mathbf{2.14^{+0.10}_{-0.09}}$ solar masses (68.3%credibility interval; 95.4% credibility interval is$\mathbf{2.14^{+0.20}_{-0.18}}$ solar masses). It is highly likely to be themost massive neutron star yet observed, and serves as a strong constraint onthe neutron star interior EoS.

Relativistic Shapiro delay measurements of an extremely massive millisecond pulsar