component in stellar burning in giants, depending on the low energy cross section. So far only extrapolations from higher-energy measurements exist and recent estimates vary by orders of magnitude. These large uncertainties call for an experimental reinvestigation of this reaction. We present a direct measurement of the 18O(p;)19F cross section using a high-eciency 4 BGO summing detector at the Laboratory for Underground Nuclear Astrophysics (LUNA). The reaction cross section has been directly determined for the rst time from 140 keV down to 85 keV and the dierent cross section components have been obtained individually. The previously highly uncertain strength of the 90 keV resonance was found to be 0.53 0.07 neV, three orders of magnitude lower than an indirect estimate based on nuclear properties of the resonant state and a factor of 20 lower than a recently established upper limit, excluding the possibility that the 90 keV resonance can contribute signicantly to the stellar reaction rate.