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We measure the stellar mass-star formation rate relation in star-forming diskgalaxies at z<0.085, using Galaxy~Zoo morphologies to examine differentpopulations of spirals as classified by their kiloparsec-scale structure. Weexamine the number of spiral arms, their relative pitch angle, and the presenceof a galactic bar in the disk, and show that both the slope and dispersion ofthe M-SFR relation is constant when varying all the above parameters. We alsoshow that mergers (both major and minor), which represent the strongestconditions for increases in star formation at a constant mass, only boost theSFR above the main relation by ~0.3 dex; this is significantly smaller than theincrease seen in merging systems at z>1. Of the galaxies lying significantlyabove the M-SFR relation in the local Universe, more than 50% are mergers. Weinterpret this as evidence that the spiral arms, which are imperfectreflections of the galaxy's current gravitational potential, are either fullyindependent of the various quenching mechanisms or are completely overwhelmedby the combination of outflows and feedback. The arrangement of the starformation can be changed, but the system as a whole regulates itself even inthe presence of strong dynamical forcing.

Galaxy Zoo: the dependence of the star formation-stellar mass relation on spiral disk morphology