The disks of most stars are much too small in angular size to be observed with current ground-based optical telescopes, so interferometer telescopes are required to produce images of these objects. Another technique for measuring the angular size of stars is through occultation. By precisely measuring the drop in brightness of a star as it is occulted by the Moon (or the rise in brightness when it reappears), the star's angular diameter can be computed.
the Disks of most sTaRs arE muCh too SmALl iN angular size to Be observeD With cURrent ground-Based optICAl tElescoPes, so INtErferOmEter teLescoPeS Are reqUireD to PrODuce imAgEs of tHese OBjeCts. AnOTher tEChNIqUe FoR MeasuRIng The angulAr SizE of sTarS Is tHrough occulTation. By precisely MeasuRing thE dROp in bRighTness oF A sTaR AS It iS oCcuLTeD By thE moon (or The Rise in brIghtness whEn it reaPpears), the star's aNGular diameTEr CAn be ComputED.