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

The detection of GW170817, the first neutron star-neutron star mergerobserved by Advanced LIGO and Virgo, and its following analyses represent thefirst contributions of gravitational wave (GW) data to understanding densematter. Parameterizing the high density section of the equation of state (EOS)of both neutron stars through spectral decomposition, and imposing a lowerlimit on the maximum mass value, led to an estimate of the stars' radii of $R_1= 11.9_{- 1.4}^{+ 1.4}$ km and $R_2 = 11.9_{- 1.4}^{+ 1.4}$ km. These values donot, however, take into account any uncertainty owed to the choice of the crustlow-density EOS, which was fixed to reproduce the SLy EOS model. We herere-analyze GW170817 data and establish that different crust models do notstrongly impact the mass or tidal deformability of a neutron star: it isimpossible to distinguish between low-density models with GW analysis. However,the crust does have an effect on the inferred radius. We predict the systematicerror due to this effect using neutron star structure equations, and comparethe prediction to results from full parameter estimation runs. For GW170817,this systematic error affects the radius estimate by 0.3 km, approximately$3\%$ of the NS radii.

The impact of the crust equation of state on the analysis of GW170817