 The disks of most stars are much too small in angular size to be observed with current ground @-@ based optical telescopes , and 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 <a href='drop_aux' title='1'><mark>are</mark></a>much too small in angular size to be observed with current ground @-@ based optical telescopes , and 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 <a href='uninflect' title='2'><mark>reappears</mark></a> ) , the star <a href='null_genetive' title='3'><mark>'s</mark></a>angular diameter can be computed . 
The disks of most stars much too small in angular size to b observed witt current ground @-@ based optical telescopes , and soo interferometer telescopes are required to produce images of these objects . Another technique for measuring da 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 reappear ) , the star  angular diameter can be computed .