Erratum: "The Effects of Metallicity and Grain Size on Gravitational Instabilities in Protoplanetary Disks" ([URL ADDRESS="/cgi-bin/resolve?2006ApJ...636L.149C" STATUS="OKAY"]ApJ 636, L149 [2006][/URL

Abstract

We have found that the total cumulative radiative energy losses shown in Figure 2 of the above-mentioned Letter were computed for only half the disk. This caused the final global cooling times tcool in the eighth column of the original Table 1 to be too large by a factor of 2. Proper values of tcool are given in the revised Table 1 below. To be more consistent with what the Letter states, we now use instantaneous values for both the total internal energy and the final total net cooling rates to compute final tcool’s, instead of averaging the loss rates over an interval of time at the end of the calculations before dividing, as was done in the Letter. We also take this opportunity to make a few other inconsequential corrections to the fourth column of the table. In addition to the changes to Table 1, the approximate initial tcool relation in the fourth paragraph of § 3.2 becomes to within tens t ∼ Z/Z cool , of percent. Despite the corrections, our conclusions in the Letter remain unchanged. Most importantly, the final tcool’s vary with metallicity and are still too long for disk fragmentation to occur with our equation of state over the range of Z examined. We regret any inconvenience our errors may have caused.