  The bright and understudied classical Be star HD 6226 has exhibited multiple
outbursts in the last several years during which the star grew a viscous
decretion disk. We analyze 659 optical spectra of the system collected from
2017-2020, along with a UV spectrum from the Hubble Space Telescope and high
cadence photometry from both TESS and the KELT survey. We find that the star
has a spectral type of B2.5IIIe, with a rotation rate of 74% of critical. The
star is nearly pole-on with an inclination of $13.4$ degree. We confirm the
spectroscopic pulsational properties previously reported, and report on three
photometric oscillations from KELT photometry. The outbursting behavior is
studied with equivalent width measurements of H$\alpha$ and H$\beta$, and the
variations in both of these can be quantitatively explained with two
frequencies through a Fourier analysis. One of the frequencies for the emission
outbursts is equal to the difference between two photometric oscillations,
linking these pulsation modes to the mass ejection mechanism for some
outbursts. During the TESS observation time period of 2019 October 7 to 2019
November 2, the star was building a disk. With a large dataset of H$\alpha$ and
H$\beta$ spectroscopy, we are able to determine the timescales of dissipation
in both of these lines, similar to past work on Be stars that has been done
with optical photometry. HD 6226 is an ideal target with which to study the Be
disk-evolution given its apparent periodic nature, allowing for targeted
observations with other facilities in the future.
