Using the 1-m telescope at Ritter Observatory , we took 36 observations of \zeta ^ { 2 } Coronae Borealis with a fiber-fed échelle spectrograph .
From these observations , \zeta ^ { 2 } CrB was found to be a triple system and a new spectroscopic orbit was calculated .
This orbit has two periods , a 1.72357 day period for the inner binary composed of \zeta ^ { 2 } CrB A & B and a 251 day period for the outer binary composed of \zeta ^ { 2 } CrB AB & C. The inner binary is a double-lined spectroscopic binary composed of two B7 V stars .
The inner binary ’ s center of mass ( \zeta ^ { 2 } CrB AB ) describes a long-period single-lined variation identified with the outer binary .
The inner binary period is significantly shorter than the 12.5842 day period previously calculated by Abhyankar & Sarma ( 1966 ) .
The inner binary possesses an essentially circular orbit ( e = 0.01 ) while the outer binary has an eccentric orbit ( e = 0.48 ) .
From the widths of their Si II 6371 Å lines , the v \sin i ’ s were calculated to be 46 \pm 7 km s ^ { -1 } for \zeta ^ { 2 } CrB A and 7.5 \pm 2 km s ^ { -1 } for \zeta ^ { 2 } CrB B .
As \zeta ^ { 2 } CrB A & B have similar masses , their different rotational velocities make this system a sensitive test of synchronization theories .