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

摘要: We present observations toward HOPS 383, the first known outbursting Class 0 protostar located within Orion molecular cloud using ALMA, VLA, and SMA. The SMA reveal envelope scale continuum line emission surrounding 383 at 0.85 mm, 1.1 1.3 mm. images show that HCO$^+$ H$^{13}$CO$^+$ peaks on or near continuum, while N$_2$H$^+$ is reduced same position. This reflects underlying chemistry where CO evaporating close to destroys forming HCO$^+$. also observe outflow traced by $^{12}$CO ($J = 2 \rightarrow 1$) 3 2$). A disk resolved in ALMA 0.87 mm dust orthogonal direction, with an apparent radius of $\sim$62 AU. Radiative transfer modeling gives masses 0.02 M$_{\odot}$ when fit visibilities. models including VLA 8 data indicate mass could be up a factor 10 larger due lower opacity longer wavelengths. temperature surface density profiles from modeling, assumed 0.5 suggest Toomre $Q$ parameter $< 1$ before outburst, making gravitational instability viable mechanism explain outbursts early age if sufficiently massive.