标题： 在中等质量恒星周围吹泡泡：主序星风的反馈不足以 显示英文标题

标题： Blowing Bubbles around Intermediate-Mass Stars: Feedback from Main-Sequence Winds is not Enough

摘要： 在年轻的恒星形成环境中，已经观测到许多球形“壳层”，这些环境包含低质量和中等质量的恒星。 这些观测表明，这些壳层可能是由年轻主序星各向同性的恒星风反馈产生的。 然而，这些壳层的驱动机制仍然不确定，因为风注入的动量太低，无法解释它们的大小和动力学，这是由于它们的质量损失率较低。 然而，这些研究忽略了风的动能如何传递给星际介质，而是假设它通过辐射立即丢失，这表明这些壳层是动量驱动的。 中等质量恒星具有快速（$v_w \gtrsim 1000$km/s）的恒星风，因此风注入的能量应该产生比动量驱动的风泡更大的能量驱动绝热风泡。 在这里，我们通过执行一系列三维磁流体动力学模拟，研究能量驱动的风反馈是否可以产生观测到的壳层，这些模拟涉及放置在磁化、湍流分子云中的中等质量恒星和大质量恒星。 我们发现，对于模拟的大质量恒星，能量驱动的风反馈在分子云中产生了$\sim$pc尺度的风泡，这与观测到的壳层大小一致，但中等质量恒星的风无法产生类似的壳层，这是由于它们的质量损失率和速度较低。 因此，这样的壳层必须是由低质量和中等质量恒星形成过程中固有的其他反馈过程驱动的。 显示英文摘要

摘要： Numerous spherical ``shells" have been observed in young star-forming environments that host low- and intermediate-mass stars. These observations suggest that these shells may be produced by isotropic stellar wind feedback from young main-sequence stars. However, the driving mechanism for these shells remains uncertain because the momentum injected by winds is too low to explain their sizes and dynamics due to their low mass-loss rates. However, these studies neglect how the wind kinetic energy is transferred to the ISM and instead assume it is instantly lost via radiation, suggesting that these shells are momentum-driven. Intermediate-mass stars have fast ($v_w \gtrsim 1000$ km/s) stellar winds and therefore the energy injected by winds should produce energy-driven adiabatic wind bubbles that are larger than momentum-driven wind bubbles. Here, we explore if energy-driven wind feedback can produce the observed shells by performing a series of 3D magneto-hydrodynamic simulations of wind feedback from intermediate-mass and high-mass stars that are placed in a magnetized, turbulent molecular cloud. We find that, for the high-mass stars modeled, energy-driven wind feedback produces $\sim$pc scale wind bubbles in molecular clouds that agree with the observed shell sizes but winds from intermediate-mass stars can not produce similar shells because of their lower mass-loss rates and velocities. Therefore, such shells must be driven by other feedback processes inherent to low- and intermediate-mass star formation.