A study explores how dark energy (DE) evolves over time, as suggested by the Dark Energy Spectroscopic Instrument (DESI) data. The research shows that the DESI-preferred DE equation of state, parameterized by $ w_{0}w_{a} $, can be recovered when DE is produced by baryon conversion in cosmologically coupled black holes (BHs). This recovery does not require any ad hoc parameter adjustments and relies solely on the independently measured cosmic star formation rate density. The study discusses the implications of this result in the context of the missing baryon problem and the anomalously low sum of neutrino masses preferred by DESI. The global evolution of DE is an orthogonal probe of cosmological coupling, complementing constraints on BH mass growth from various sources. A DE density that correlates with star formation is a natural outcome of cosmological coupling in BH populations. The study also highlights the potential of DESI and future Stage IV surveys to provide positive evidence for DE within cosmologically coupled BHs. The results show that the $ w_{0}w_{a} $ evolution expected from BH DE matches the DESI most-likely $ w_{0}w_{a} $ models when those models include any SNe datasets. The study concludes that DESI data suggest time-evolution in the dark energy density at 2.5-3.9σ confidence when combining its Baryon Acoustic Oscillation measurements with Cosmic Microwave Background and various supernovae datasets. The time-evolution is characterized by a two-parameter dark energy equation of state $ w = w_{0} + w_{a}(1 - a) $, where a is the scale factor. The analysis shows that the DESI most-likely values for $ w_{0} $ and $ w_{a} $ are recovered when a $ w_{0}w_{a} $ model is fit to dark energy produced by baryon conversion in cosmologically coupled black holes. Baryon conversion is constrained solely by measurements of the comoving star formation rate density, which are independent of the DESI measurements and previous observational studies of cosmologically coupled black hole solutions. As DESI gathers more data, the increased statistical precision will further constrain $ w_{0} $ and $ w_{a} $, potentially enabling DESI to measure the time evolution of dark energy independently, without relying on external Type Ia Supernova data.A study explores how dark energy (DE) evolves over time, as suggested by the Dark Energy Spectroscopic Instrument (DESI) data. The research shows that the DESI-preferred DE equation of state, parameterized by $ w_{0}w_{a} $, can be recovered when DE is produced by baryon conversion in cosmologically coupled black holes (BHs). This recovery does not require any ad hoc parameter adjustments and relies solely on the independently measured cosmic star formation rate density. The study discusses the implications of this result in the context of the missing baryon problem and the anomalously low sum of neutrino masses preferred by DESI. The global evolution of DE is an orthogonal probe of cosmological coupling, complementing constraints on BH mass growth from various sources. A DE density that correlates with star formation is a natural outcome of cosmological coupling in BH populations. The study also highlights the potential of DESI and future Stage IV surveys to provide positive evidence for DE within cosmologically coupled BHs. The results show that the $ w_{0}w_{a} $ evolution expected from BH DE matches the DESI most-likely $ w_{0}w_{a} $ models when those models include any SNe datasets. The study concludes that DESI data suggest time-evolution in the dark energy density at 2.5-3.9σ confidence when combining its Baryon Acoustic Oscillation measurements with Cosmic Microwave Background and various supernovae datasets. The time-evolution is characterized by a two-parameter dark energy equation of state $ w = w_{0} + w_{a}(1 - a) $, where a is the scale factor. The analysis shows that the DESI most-likely values for $ w_{0} $ and $ w_{a} $ are recovered when a $ w_{0}w_{a} $ model is fit to dark energy produced by baryon conversion in cosmologically coupled black holes. Baryon conversion is constrained solely by measurements of the comoving star formation rate density, which are independent of the DESI measurements and previous observational studies of cosmologically coupled black hole solutions. As DESI gathers more data, the increased statistical precision will further constrain $ w_{0} $ and $ w_{a} $, potentially enabling DESI to measure the time evolution of dark energy independently, without relying on external Type Ia Supernova data.