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We use a sample built on the SDSS DR7 catalogue and the bulge-discdecomposition of Simard et al. (2011) to study how the bulge and disccomponents contribute to the parent galaxy's star formation activity, bydetermining its position in the star formation rate (SFR) - stellar mass(M$_{\star}$) plane at 0.02$<z<$0.1. We use the bulge and disc colours as proxyfor their SFRs. We study the mean galaxy bulge-total mass ratio (B/T) as afunction of the residual from the MS ($\Delta_{MS}$) and find that theB/T-$\Delta_{MS}$ relation exhibits a parabola-like shape with the peak of theMS corresponding to the lowest B/Ts at any stellar mass. The lower and upperenvelop of the MS are populated by galaxies with similar B/T, velocitydispersion and concentration ($R_{90}/R_{50}$) values. Bulges above the MS arecharacterised by blue colours or, when red, by a high level of dustobscuration, thus indicating that in both cases they are actively star forming.When on the MS or below it, bulges are mostly red and dead. At stellar massesabove $10^{10.5} $M$_{\odot}$, bulges on the MS or in the green valley tend tobe significantly redder than their counterparts in the quiescence region,despite similar levels of dust obscuration. The disc color anti-correlates atany mass with the distance from the MS, getting redder when approaching the MSlower envelope and the quiescence region. We conclude that the position of agalaxy in the LogSFR-LogM$_{\star}$ plane depends on the star formationactivity of its components: above the MS both bulge and disk are actively starforming. The nuclear activity is the first to be suppressed, moving thegalaxies on the MS. Once the disk stops forming stars as well, the galaxy movesbelow the MS and eventually to the quiescence region. This is confirmed by alarge fraction ($\sim45\%$) of passive galaxies with a secure two componentmorphology.

Bulges and disks in the local Universe. Linking the galaxy structure to star formation activity