We study the spectroscopic properties of a sample of 10 ^ { 3 } void galaxies from the Sloan Digital Sky Survey ( SDSS ) and compare these with the properties of galaxies in higher density regions ( wall galaxies ) .
This sample of void galaxies covers the range of absolute magnitude from M _ { r } = -13.5 to M _ { r } = -22.5 in regions with density contrast \delta \rho / \rho < -0.6 .
In this paper we compare the equivalent widths of H \alpha , [ OII ] , [ NII ] , H \beta , and [ OIII ] of void and wall galaxies of similar luminosities and find that void galaxies have larger values , indicating that they are still forming stars at a high rate .
A comparison of the Balmer break , as measured by the parameter D _ { n } ( 4000 ) , reveals that void galaxies have younger stellar populations than wall galaxies .
Using standard techniques , we estimate H \alpha and [ OII ] star formation rates of the void and wall galaxies and along with estimates of the stellar masses , we compute specific star formation rates .
In most cases , we find that void galaxies have similar SFRs to wall galaxies but they are fainter and smaller mass .
This means that , consistent with the EWs , void galaxies have higher specific star formation rates than wall galaxies .