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 Plus monthly

Global: Zendy Tools annual

Global: Zendy Tools monthly

Global: Zendy Free Plan

GW190814 was reported during LIGO's and Virgo's third observing run with themost asymmetric component masses (a $\sim 23$ $M_{\odot}$ black hole and a$\sim2.6$ $M_{\odot}$ compact object). Under the assumption that this event isa binary black hole (BBH) merger formed through the isolated binary evolutionchannel, we reanalyze the publicly released data of GW190814 with the modifiedastrophysical priors on the effective spin $\chi_{\rm eff}$, and furtherexplore its formation history using detailed binary modeling. We show thatGW190814 is likely to have been formed through the classical common envelopechannel. Our findings show that the properties inferred using the modifiedastrophysical priors are consistent with those inferred by the uniform priors.With the newly-inferred properties of GW190814, we perform detailed binaryevolution of the immediate progenitor of the BBH (namely a close binary systemcomposed of a BH and a helium star) in a large parameter space, taking intoaccount mass-loss, internal differential rotation, supernova kicks, and tidalinteractions between the helium star and the BH companion. Our findings showthat GW190814-like events could be formed in limited initial conditions justafter the common envelope phase: a $\sim 23$ $M_{\odot}$ BH and a helium starof $M_{\rm ZamsHe}$ $\sim$ 8.5 $M_{\odot}$ at solar metallicity ($\sim$ 7.5$M_{\odot}$ at 10\% solar metallicity) with an initial orbital period at around1.0 day. Additionally, the inferred low spin of the secondary indicates thatthe required metallicity for reproducing GW190814-like events should not be toolow (e.g., Z $\gtrsim$ 0.1 $Z_{\odot}$).

Revisiting the Properties of GW190814 and Its Formation History