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In the group of B stars with spectroscopic peculiarities, we can find the Beand the B[e] stars. The Be stars are early-type rapid rotators that present, astheir principal characteristic, emission lines of hydrogen and singly ionizedmetals due to the presence of a gaseous envelope. The B[e] stars present intheir spectra heterogeneous features that reveal the presence of regions withvery different properties in a gaseous and dusty envelope. Our goal is to studythe evolution of the disks around peculiar B stars through the variability oftheir physical properties and dynamical structure, as well as to setconstraints on different models and disk forming mechanisms. Throughout thelast decade, we have carried out temporal monitoring of a sample of objects inthe near infrared using spectroscopic facilities at the Gemini and Las CampanasObservatories. In the present work, we focus on the classical Be star 12 Vul,for which also optical spectra have been collected quasi-simultaneously. Weobserved variability in the hydrogen line profiles of 12 Vul, attributed todissipating and building-up processes of the circumstellar envelope. Also, wefound that this Be star presented the $^{12}$CO band heads in emission in oneobservation. The emission of this molecule has not been previously reported ina Be star, while it is a common feature among B[e] stars. We obtainedparameters to describe the $^{12}$CO emitting region and propose differentscenarios to explain this intriguing emission.

Intriguing detection of $^{12}$CO molecular emission in a classical Be star