•In our letter, we address the dominant uncertainty regarding the extent of the rp-process flow bypass around <math altimg="si1.svg"><mmultiscripts><mrow><mi mathvariant="normal">Ni</mi></mrow><mprescripts/><none/><mrow><mn>56</mn></mrow></mmultiscripts></math> waiting point for astrophysical conditions relevant to Type-1 X-ray bursts.•We removed the final significant uncertainty, the beta-delayed proton branching ratio for <math altimg="si13.svg"><mmultiscripts><mrow><mi mathvariant="normal">Zn</mi></mrow><mprescripts/><none/><mrow><mn>57</mn></mrow></mmultiscripts></math>, definitively determining that there is a <math altimg="si1.svg"><mmultiscripts><mrow><mi mathvariant="normal">Ni</mi></mrow><mprescripts/><none/><mrow><mn>56</mn></mrow></mmultiscripts></math> bypass.•In addition, we also identified the second case of the exotic <math altimg="si3.svg"><mi>β</mi><mo linebreak="goodbreak" linebreakstyle="after">−</mo><mi>γ</mi><mo linebreak="goodbreak" linebreakstyle="after">−</mo><mi>p</mi></math> decay mode in the fp-shell. We measured the <math altimg="si13.svg"><mmultiscripts><mrow><mi mathvariant="normal">Zn</mi></mrow><mprescripts/><none/><mrow><mn>57</mn></mrow></mmultiscripts></math>β-delayed proton (βp) and γ emission at the National Superconducting Cyclotron Laboratory. We find a <math altimg="si13.svg"><mmultiscripts><mrow><mi mathvariant="normal">Zn</mi></mrow><mprescripts/><none/><mrow><mn>57</mn></mrow></mmultiscripts></math> half-life of <math altimg="si4.svg"><mn>43.6</mn><mo>±</mo><mn>0.2</mn></math> ms, βp branching ratio of <math altimg="si5.svg"><mo stretchy="false">(</mo><mn>84.7</mn><mo>±</mo><mn>1.4</mn><mo stretchy="false">)</mo><mtext>%</mtext></math>, and identify four transitions corresponding to the exotic β-γ-p decay mode, the second such identification in the fp-shell. The p/γ ratio was used to correct for isospin mixing while determining the <math altimg="si13.svg"><mmultiscripts><mrow><mi mathvariant="normal">Zn</mi></mrow><mprescripts/><none/><mrow><mn>57</mn></mrow></mmultiscripts></math> mass via the isobaric multiplet mass equation. Previously, it was uncertain as to whether the rp-process flow could bypass the textbook waiting point <math altimg="si1.svg"><mmultiscripts><mrow><mi mathvariant="normal">Ni</mi></mrow><mprescripts/><none/><mrow><mn>56</mn></mrow></mmultiscripts></math> for astrophysical conditions relevant to Type-I X-ray bursts. Our results definitively establish the existence of the <math altimg="si1.svg"><mmultiscripts><mrow><mi mathvariant="normal">Ni</mi></mrow><mprescripts/><none/><mrow><mn>56</mn></mrow></mmultiscripts></math> bypass, with 14-17% of the rp-process flow taking this route.< Réduire