Outflows and Bubbles in Taurus: Star-formation Feedback Sufficient to Maintain Turbulence

Abstract

We have identified outflows and bubbles in the Taurus molecular cloud based on the $\sim 100$ deg${}^2$ Five College Radio Astronomy Observatory ${}^{12}$CO(1-0) and ${}^{13}$CO(1-0) maps and the Spitzer young stellar object catalogs. In the main 44 deg${}^2$ area of Taurus we found 55 outflows, of which 31 were previously unknown. We also found 37 bubbles in the entire 100 deg${}^2$ area of Taurus, all of which had not been found before. The total kinetic energy of the identified outflows is estimated to be $\sim 3.9\times 10^{45}$ erg, which is \textbf{1\%} of the cloud turbulent energy. The total kinetic energy of the detected bubbles is estimated to be $\sim 9.2\times 10^{46}$ erg, which is 29\% of the turbulent energy of Taurus. The energy injection rate from outflows is $\sim 1.3\times 10^{33}\mathrm{erg}{\mathrm{s}}^{-1}$, \textbf{0.4 - 2 times} the dissipation rate of the cloud turbulence. The energy injection rate from bubbles is $\sim 6.4\times 10^{33}$ erg s${}^{-1}$, \textbf{2 - 10 times} the turbulent dissipation rate of the cloud. The gravitational binding energy of the cloud is $\sim 1.5\times 10^{48}$ {\bf erg}, \textbf{385} and 16 times the energy of outflows and bubbles, respectively. We conclude that neither outflows nor bubbles can \textbf{provide enough energy to balance the overall gravitational binding energy and the turbulent energy of Taurus. However,} in the current epoch, stellar feedback is sufficient to maintain the observed turbulence in Taurus.

More figures can be found from the link: http://adsabs.harvard.edu/abs/2015ApJS..219...20L

References in corpus (3)

• Theory of Star Formation
• The relation between gas and dust in the Taurus Molecular Cloud
• The Five College Radio Astronomy Observatory CO Mapping Survey of the Taurus Molecular Cloud

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