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Morphology and structure of galaxies reflect their star formation andassembly histories. We use the framework of mutual information ($\mathrm{MI}$)to quantify interdependence among several structural variables and to rank themaccording to their relevance for predicting specific star formation rate (SSFR)by comparing the $\mathrm{MI}$ of the predictor variables with SSFR andpenalizing variables that are redundant. We apply this framework to study $\sim3,700$ face-on star-forming galaxies (SFGs) with varying degrees of bulgedominance and central concentration and with stellar mass $M_\star \approx10^9\,M_\odot - 5\times 10^{11}\,M_\odot$ at redshift $z = 0.02-0.12$. We usethe Sloan Digital Sky Survey (SDSS) Stripe 82 deep $i$-band imaging data, whichimprove measurements of asymmetry and bulge dominance indicators. We find thatstar-forming galaxies are a multi-parameter family. In addition to $M_\star$,asymmetry emerges as the most powerful predictor of SSFR residuals of SFGs,followed by bulge prominence/concentration. Star-forming galaxies with higherasymmetry and stronger bulges have higher SSFR at a given $M_\star$. Theasymmetry reflects both irregular spiral arms and lopsidedness in seeminglyisolated SFGs and structural perturbations by galaxy interactions or mergers.

What is Important? Morphological Asymmetries are Useful Predictors of Star Formation Rates of Star-forming Galaxies in SDSS Stripe 82