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

Galactic field black hole (BH) low-mass X-ray binaries (LMXBs) are believedto form in situ via the evolution of isolated binaries. In the standardformation channel, these systems survived a common envelope phase, after whichthe remaining helium core of the primary star and the subsequently formed BHare not expected to be highly spinning. However, the measured spins of BHs inLMXBs cover the whole range of spin parameters. We propose here that the BHspin in LMXBs is acquired through accretion onto the BH after its formation. Inorder to test this hypothesis, we calculated extensive grids of detailed binarymass-transfer sequences. For each sequence, we examined whether, at any pointin time, the calculated binary properties are in agreement with theirobservationally inferred counterparts of 16 Galactic LMXBs. The "successful"sequences give estimates of the mass that the BH has accreted since the onsetof Roche-Lobe overflow. We find that in all Galactic LMXBs with measured BHspin, the origin of the spin can be accounted for by the accreted matter, andwe make predictions about the maximum BH spin in LMXBs where no measurement isyet available. Furthermore, we derive limits on the maximum spin that any BHcan have depending on current properties of the binary it resides in. Finallywe discuss the implication that our findings have on the BH birth-massdistribution, which is shifted by ~1.5 Msolar towards lower masses, compared tothe currently observed one.

The Origin of Black Hole Spin in Galactic Low-Mass X-ray Binaries