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 Tools annual

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 monthly

Global: Zendy Plus monthly

Presents the access of premium content as premium feature

Premium Content

Global: Zendy Plus annual

Global: Zendy Free Plan

Although gravitational waves only interact weakly with matter, theirpropagation is affected by a gravitational potential. If a gravitational wavesource is eclipsed by a star, measuring these perturbations provides a way todirectly measure the distribution of mass throughout the stellar interior. Wecompute the expected Shapiro time delay, amplification and deflection during aneclipse, and show how this can be used to infer the mass distribution of theeclipsing body. We identify continuous gravitational waves from neutron starsas the best candidates to detect this effect. When the Sun eclipses a far-awaysource, depending on the depth of the eclipse the time-delay can change by upto $\sim 0.034$ ms, the gravitational-wave strain amplitude can increase by$\sim 4$%, and the apparent position of the source in the sky can vary by$4''$. Accreting neutron stars with Roche-lobe filling companion stars have ahigh probability of exhibiting eclipses, producing similar time delays butundetectable changes in amplitude and sky location. Even for the most rapidlyrotating neutron stars, this time delay only corresponds to a few percent ofthe phase of the gravitational wave, making it an extremely challengingmeasurement. However, if sources of continuous gravitational waves exist justbelow the limit of detection of current observatories, next-generationinstruments will be able to observe them with enough precision to measure thesignal of an eclipsing star. Detecting this effect would provide a new directprobe to the interior of stars, complementing asteroseismology and thedetection of solar neutrinos.

Eclipses of continuous gravitational waves as a probe of stellar structure