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

We comment on a recent study reporting evidence for the general relativisticLense-Thirring secular precession of the inclination $I$ of the orbital planeto the plane of the sky of the tight binary system PSR J1141-6545 made of awhite dwarf and an emitting radiopulsar of comparable masses. The quadrupolemass moment $Q_2^\mathrm{c}$ and the angular momentum ${\boldsymbolS}^\mathrm{c}$ of the white dwarf cause the detectable effects on $I$ withrespect to the present-day accuracy in the pulsar's timing. Thehistory-dependent and model-dependent assumptions to be made on$Q_2^\mathrm{c}$ and ${\boldsymbol S}^\mathrm{c}$, required even just tocalculate the analytical expressions for the resulting post-Keplerianprecessions, may be deemed as too wide in order to claim a successful test ofthe Einsteinian gravitomagnetic effect. Moreover, depending on how$Q_2^\mathrm{c}$ is calculated, the competing quadrupole-induced rate ofchange, which is a major source of systematic uncertainty, may be up to$\lesssim 30-50\%$ of the Lense-Thirring effect for most of the allowed valuesin the 3D parameter space spanned by the white dwarf's spin period$P_\mathrm{s}$, and the polar angles $i_\mathrm{c},\,\zeta_\mathrm{c}$ of itsspin axis. The possible use of the longitude of periastron $\dot\varpi$ isinvestigated as well. It turns out that a measurement of its secularprecession, caused, among other things, also by$Q_2^\mathrm{c},\,{\boldsymbol{S}}^\mathrm{c}$, could help in furtherrestricting the permitted regions in the white dwarf's parameter space.

A comment on "Lense-Thirring frame dragging induced by a fast-rotating white dwarf in a binary pulsar system" by V. Venkatraman Krishnan et al