  Solar coronal mass ejections (CMEs) have a strong association with solar
flares that is not fully understood. This characteristic of our Sun's magnetic
activity may also occur on other stars, but the lack of successfully detected
stellar CMEs makes it difficult to perform statistical studies that might show
a similar association between CMEs and flares. Because of the potentially
strong association, the search for stellar CMEs often starts with a successful
search for superflares on magnetically active stars. Regardless of the flare's
presence, we emphasize the utility of searching for CME-specific spectroscopic
signatures when attempting to find and confirm stellar CME candidates. We use
solar CMEs as examples of why a multitude of ultraviolet emission lines, when
detected simultaneously, can substantially improve the credibility of
spectroscopically discovered stellar CME candidates. We make predictions on how
bright CME-related emission lines can be if they derived from distant stars. We
recommend the use of three emission lines in particular (C IV 1550 Angstroms, O
VI 1032 Angstroms, and C III 977 Angstroms) due to their potentially bright
signal and convenient diagnostic capabilities that can be used to confirm if an
observational signature truly derives from a stellar CME.
