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

In the numerical modeling of the GRB afterglow, some approximations have beenmade for simplicity, and different groups developed their codes. A robust testof these models/approaches is challenging because of the lack of directlymeasured physical parameters. Fortunately, the viewing angle inferred from theafterglow modeling is widely anticipated to be the same as the inclinationangle of the binary neutron star (BNS) mergers that can be evaluated with thegravitational wave (GW) data. Therefore in the future, it is possible tocalibrate the afterglow modeling with the GW inclination angle measurements. Wetake three methods, including both analytical estimations and directsimulations, to project the uncertainties of the inclination anglemeasurements. For some BNS mergers accompanied with electromagneticcounterparts detected in the O4/O5 runs of LIGO/Virgo/KAGRA/LIGO-Indiadetectors, we show that the inclination angle can be determined within anuncertainty of $\leq 0.1$ rad, supposing that the Hubble constant is known withan accuracy of $\leq 3\%$ and the uncertainty of Hubble flow velocity is within$\sim 1 \%$. The off-axis GRB outflow will give rise to afterglow emission, andthe most energetic ones may be detectable at the distance of $\sim$ 100-200 Mpceven for a viewing angle of $\geq 0.3$ rad. Such events can thus serve as arobust test of the afterglow modeling approach. We have also evaluated theprospect of resolving the so-called Hubble tension with a single GW/GRBassociation event. We find out that a $\sim 3\%$ precision Hubble constant isobtainable if the uncertainty of the viewing angle can be constrained to bewithin $\sim 0.1$ rad, which is expected to be the case for some nearby ($\leq250$ Mpc) bright/on-axis GRBs with a well-behaved afterglow light curvedisplaying a clear achromatic break at early times.

physical review. d/physical review. d.

Prospects of calibrating afterglow modeling of short GRBs with  gravitational wave inclination angle measurements and resolving the Hubble  tension with a GW-GRB association event