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We present observations toward HOPS 383, the first known outbursting Class 0protostar located within the Orion molecular cloud using ALMA, VLA, and SMA.The SMA observations reveal envelope scale continuum and molecular lineemission surrounding HOPS 383 at 0.85 mm, 1.1 mm, and 1.3 mm. The images showthat HCO$^+$ and H$^{13}$CO$^+$ peaks on or near the continuum, whileN$_2$H$^+$ is reduced at the same position. This reflects the underlyingchemistry where CO evaporating close to the protostar destroys N$_2$H$^+$ whileforming HCO$^+$. We also observe the molecular outflow traced by $^{12}$CO ($J= 2 \rightarrow 1$) and ($J = 3 \rightarrow 2$). A disk is resolved in the ALMA0.87 mm dust continuum, orthogonal to the outflow direction, with an apparentradius of $\sim$62 AU. Radiative transfer modeling of the continuum gives diskmasses of 0.02 M$_{\odot}$ when fit to the ALMA visibilities. The modelsincluding VLA 8 mm data indicate that the disk mass could be up to a factor of10 larger due to lower dust opacity at longer wavelengths. The disk temperatureand surface density profiles from the modeling, and an assumed protostar massof 0.5 M$_{\odot}$ suggest that the Toomre $Q$ parameter $< 1$ before theoutburst, making gravitational instability a viable mechanism to explainoutbursts at an early age if the disk is sufficiently massive.

Constraining the Chemical Signatures and the Outburst Mechanism of the Class 0 Protostar HOPS 383