To determine the spectral features that G-giant stars, such as those in the Capella system, do not have, we typically refer to the characteristics of their spectral classification. G-giant stars have specific features in their spectra, such as absorption lines due to hydrogen, calcium, and other metals, as well as their effective temperature influence on the presence of certain spectral lines.
Generally, spectral features that G-giant stars do not have include those that are characteristic of other spectral types. For example:
- O/B-type features: G-giant stars do not exhibit strong ionized helium (He II) lines, which are present in O and B-type stars.
- A-type features: They lack the pronounced Balmer lines that A-type stars exhibit.
- Wolf-Rayet features: They do not show the broad emission lines typical of Wolf-Rayet stars.
- M-type features: G-giants do not typically show prominent molecular bands seen in cooler M-type stars.
In summary, while G-giant stars have a specific set of spectral features, they do not exhibit the features prominent in hotter stars like O, B, A types, or cooler stars like M types. If you had specific spectral features listed in a table, you would look for those outside the characteristic range of G-giant stars, such as very strong helium lines or molecular bands unique to other types.