论文标题
一颗巨大的恒星诞生了：恒星风，辐射压力和准直流的反馈如何限制在巨大的恒星上
A Massive Star is Born: How Feedback from Stellar Winds, Radiation Pressure, and Collimated Outflows Limits Accretion onto Massive Stars
论文作者
论文摘要
巨大的质体在积极积聚时获得了高亮度，并且在恒星大气中施加的辐射压力可能会引起各向同性高速风。这些风将与周围的气体产生冲击热（$ t \ sim 10^7 $ k）的脆弱气体碰撞，该气体绝热地扩展并推出可能会积聚的密集气体。我们提出了一套3D辐射 - 磁性水力动力学模拟，对大量的Prestellar核心崩溃，包括来自恒星和粉尘的辐射场的辐射反馈，流出的流出，并首次引起了同位素的恒星风，以对这些过程产生大量形成的星星，这是对大型星星的模型。我们发现，当大量原始恒星仍在积聚时，最初发射风，并且随着原恒星签约的主要收入，其风能也会发展。风反馈驱动具有双相形态的不对称绝热风气泡，因为密集的偶然物质会夹住热冲击加热的气体的膨胀。我们将其称为“风洞效应”。如果芯被磁化，风反馈最初在驱动绝热风气泡方面的效率较低，因为磁张力会延迟其生长。我们发现，风反馈最终将积聚在$ \ sim $ 30 $ 30 $ \ rm {m _ {\ rm \ odot}}} $ protostars中，这些$ protostar是从此处模拟的隔离核的崩溃中形成的。因此，我们的结果表明$ \ gtrsim $ 30 $ \ rm {m _ {\ rm \ odot}} $ stars可能需要从主机云中进行大规模的动态流入才能克服风反馈。此外，我们讨论了用\ textit {chandra}观察绝热风泡的含义，而大规模的质子仍然高度嵌入。
Massive protostars attain high luminosities as they are actively accreting and the radiation pressure exerted on the gas in the star's atmosphere may launch isotropic high-velocity winds. These winds will collide with the surrounding gas producing shock-heated ($T\sim 10^7$ K) tenuous gas that adiabatically expands and pushes on the dense gas that may otherwise be accreted. We present a suite of 3D radiation-magnetohydrodynamic simulations of the collapse of massive prestellar cores and include radiative feedback from the stellar and dust-reprocessed radiation fields, collimated outflows, and, for the first time, isotropic stellar winds to model how these processes affect the formation of massive stars. We find that winds are initially launched when the massive protostar is still accreting and its wind properties evolve as the protostar contracts to the main-sequence. Wind feedback drives asymmetric adiabatic wind bubbles that have a bipolar morphology because the dense circumstellar material pinches the expansion of the hot shock-heated gas. We term this the "wind tunnel effect." If the core is magnetized, wind feedback is less efficient at driving adiabatic wind bubbles initially because magnetic tension delays their growth. We find that wind feedback eventually quenches accretion onto $\sim$30 $\rm{M_{\rm \odot}}$ protostars that form from the collapse of the isolated cores simulated here. Hence, our results suggest that $\gtrsim$30 $\rm{M_{\rm \odot}}$ stars likely require larger-scale dynamical inflows from their host cloud to overcome wind feedback. Additionally, we discuss the implications of observing adiabatic wind bubbles with \textit{Chandra} while the massive protostars are still highly embedded.
