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 compute the mass, radius and tidal deformability of stars containing phasetransitions from hadronic to quark phase(s). These quantities are computed forthree types of hadronic envelopes: purely nuclear, hyperonic, and$\Delta$-resonance--hyperon admixed matter. We consider either a singlefirst-order phase transition to a quark phase with a maximally stiff equationof state (EOS) or two sequential first-order phase transitions mimicking atransition from hadronic to a quark matter phase followed by a second phasetransition to another quark phase. We explore the parameter space whichproduces low-mass twin and triplet configurations where equal-mass stars havesubstantially different radii and tidal deformabilities. We demonstrate thatwhile for purely hadronic stiff EOS the obtained maximum mass is inconsistentwith the upper limit on this quantity placed by GW170817, the inclusion of thehyperonic and $\Delta$-resonance degrees of freedom, as well as thedeconfinement phase transition at sufficiently low density, produces aconfiguration of stars consistent with this limit. The obtained hybrid starconfigurations are in the mass range relevant for the interpretation of theGW170817 event. We compare our results for the tidal deformability with thelimits inferred from GW170817 showing that the onset of non-nucleonic phases,such as $\Delta$-resonance--hyperon admixed phase and/or the quark phase(s),are favored by this data if the nuclear EOS is stiff. Also, we show thatlow-mass twins and especially triplets proliferate the number of combinationsof possible types of stars that can undergo a merger event, the maximal numberbeing six in the case of triplets. The prospects for uncovering the first-orderphase transition(s) to and in quark matter via measurements of tidaldeformabilities in merger events are discussed.

Relativistic hybrid stars with sequential first-order phase transitions and heavy-baryon envelopes