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

Recently, the black hole X-ray binary (BHXB) Nova Muscae 1991 has beenreported to be experiencing an extremely rapid orbital decay. So far, threeBHXBs have anomalously high orbital period derivatives, which can not beinterpreted by the standard stellar evolution theory. In this work, weinvestigate whether the resonant interaction between the binary and asurrounding circumbinary (CB) disk could produce the observed orbital periodderivatives. Analytical calculations indicate that the observed orbital periodderivatives of XTE J1118+480 and A0620-00 can originate from the tidal torquebetween the binary and a CB disk with a mass of $10^{-9}~\rm M_{\odot}$, whichis approximately in agreement with the dust disk mass detected in these twosources. However, Nova Muscae 1991 was probably surrounded by a heavy CB diskwith a mass of $10^{-7}~\rm M_{\odot}$. Based on the CB disk model and theanomalous magnetic braking theory, we simulate the evolution of the three BHXBswith intermediate-mass donor stars by using the MESA code. Our simulatedresults are approximately consistent with the observed donor star masses,orbital periods, and orbital-period derivatives. However, the calculatedeffective temperatures of the donor stars are higher than indicated by theobserved spectral types of two sources.

Fast orbital shrinkage of black hole X-ray binaries driven by circumbinary disks