论文标题
快速喷射是由于Eta Carinae的大喷发中的喷射互动而产生的
Fast Ejecta Resulted from Jet-Wind Interaction in the Great Eruption of Eta Carinae
论文作者
论文摘要
$η$ carinae的19世纪大喷发（GE）的增生模型表明，从初级流出的质量被吸收到次级上，该大众的重力构成了亮度的增加，以及大部分弹性的能量。它进一步指出，积聚伴随着塑造双极舍氏星云的两种喷头的喷射。对GE的回声观察发现的发射线和宽阔的翅膀表明，赤道方向的某些质量达到了$ 10 \，000 \，\ rm {km {km \，s^{ - 1}} $。在GE期间，我们在Periastron通道后运行流体动力模拟，从次级产生了从初级爆发的气体爆发时发射喷气机。然后，我们遵循极性喷气机与周围的一级风的相互作用，因为它们将部分加速到速度$> 10 \，000 \，\ rm {km {km \，s^{ - 1}} $，并将其偏向下纬度。我们发现，在GE期间达到这些高速的质量量为$ M_H \ of约0.02 \，\ rm {m _ {\ odot}} $。该值达到最大值，然后随时间减小。我们的模拟与增值模型的先前结果一致，我们从中考虑了GE的能源预算，从中估算了$ M_H $。积聚模型可以解释具有已知两颗恒星的光回波中高速气体的观察结果，而不需要三颗星系统。
The accretion model for the nineteenth century Great Eruption (GE) of $η$ Carinae suggests that mass outflowing from the primary was accreted onto the secondary, and the gravitational energy of that mass accounts for the increase in luminosity and most of the kinetic energy of the ejecta. It further argues that the accretion was accompanied by the ejection of two jets that shaped the bipolar Homunculus nebula. Observations of echos from the GE found emission lines with broad wings suggesting some of the mass in equatorial directions reached more than $10\,000 \,\rm{km\,s^{-1}}$. We run hydrodynamic simulations following periastron passage during the GE, launching jets from the secondary as it accreted gas erupted from the primary. We then follow the interaction of the polar jets with the surrounding primary wind, as they accelerate part of the flow to velocities $ > 10\,000 \,\rm{km\,s^{-1}}$ and deflect it towards lower latitudes. We find that the amount of mass that reached these high velocities during the GE is $M_h \approx 0.02 \,\rm{M_{\odot}}$. This value reaches maximum and then decreases with time. Our simulations agree with previous results of the accretion model from which we estimate $M_h$ taking into account the energy budget of the GE. The accretion model can explain the observations of high velocity gas in light echos with the known two stars, and a triple star system is not required.
