  We have conducted a high-dispersion ($R \sim$ 34,000) optical spectroscopic
study of 10 young stars near the cometary gloule CG 30 in the Gum Nebula, a
diffuse H \textsc{ii} region home to at least 32 cometary globules. All 10
spectroscopically observed stars at the nebula's northern edge are of low mass
(spectral types M4.5 - K5), have broad H$\alpha$ emission, and show spectral
veiling. Eight of the 10 are classical T Tauri stars. We spectroscopically
measure the photospheric properties of CG 30 IRS 4 inside CG 30. Though
embedded, CG 30 IRS 4 is T Tauri-like, with relatively slow projected rotation
and moderate veiling. Undepleted Li absorptions, strong H$\alpha$ emissions,
and positions well above the main sequence on an HR diagram suggest the 10
stars are $\lesssim$1 Myr old. Using our measurements, previous spectroscopy,
and previous photometry of 11 other young stars in the area, we determine
stellar, kinematic, and accretion properties of a total of 21 young stars.
Shared radial velocities, proper motions, distances, and ages suggest 14 of the
young stars (including CG 30 IRS 4) are kinematically related to CG 30. From
\textit{Gaia} DR2 distances to 6 of these stars, we derive a distance of
$358.1\pm2.2$ pc to the cometary globule complex CG 30/31/38. The CG 30
association has an accretor fraction of $29\pm14$\%, low for quiescent clusters
of similar age but consistent with other irradiated clusters. The Gum Nebula's
moderate radiation environment ($G_0=6.6^{+3.2}_{-2.7}$ at CG 30) may be strong
enough to shorten disk lifetimes.
