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We study the association of solar flares with coronal mass ejections (CMEs)during the deep, extended solar minimum of 2007-2009, using extreme-ultraviolet(EUV) and white-light (coronagraph) images from the {\it Solar TerrestrialRelations Observatory} (STEREO). Although all of the fast (v $>$ 900 kms$^{-1}$) {\it and} wide ($\theta >$ 100$\arcdeg$) CMEs are associated with aflare that is at least identified in GOES soft X-ray light curves, a majorityof flares with relatively high X-ray intensity for the deep solar minimum (e.g.$\gtrsim$1 \times 10^{-6}$ W m$^{-2}$ or C1) are not associated with CMEs.Intense flares tend to occur in active regions with strong and complexphotospheric magnetic field, but the active regions that produce CME-associatedflares tend to be small, including those that have no sunspots and therefore noNOAA active-region numbers. Other factors on scales comparable to and largerthan active regions seem to exist that contribute to the association of flareswith CMEs. We find the possible low coronal signatures of CMEs, namelyeruptions, dimmings, EUV waves, and Type III bursts, in 91%, 74%, 57%, and 74%,respectively, of the 35 flares that we associate with CMEs. None of theseobservables can fully replace direct observations of CMEs by coronagraphs.

The Association of Solar Flares with Coronal Mass Ejections During the Extended Solar Minimum