Ia型超新星爆发前的观测性质
Pre-Explosive Observational Properties of Type Ia Supernovae
摘要：
在双简并旋转驱动吸积的框架下，旋转CO WD直接吸积富CO物质的演化路径被跟踪到爆炸爆发前几秒钟。我们发现，演化特性只依赖于实际质量的吸积WD，而不是在以前的历史。我们确定预期的频率和振幅的引力波发射，这发生在质量传递过程中，作为一个自调谐机制的吸积过程本身。与银河系源有关的引力信号可以很容易地用下一代空间干涉仪检测到，并可以为祖先模型提供显着的约束。银河系中爆炸前物体的预期统计分布也在有效温度-视热星等图中提供，这些图可用于通过紫外线勘测确定合并的DD系统。我们强调，热核爆炸的发生是由于物理条件的衰减保持过稳定的结构以上的经典Ehrasekhar限制，而不是由一个稳定的WD质量增加到这个限制。这一结论与祖先的进化情景无关，但它是旋转稳定效应的直接结果。这样的发生是认识论的变化，在定义的点火过程中吸积WD的角度。此外，这需要一个很长的进化时期（几百万年），以达到爆炸后，上述条件停止保持稳定的WD。因此，实际上不可能在最近的爆炸前帧中探测到甚至非常接近SN Ia的爆炸WD伴星的痕迹。
英文摘要：
The evolutionary path of rotating CO WDs directly accreting CO-rich matter is followed up to few seconds before the explosive breakout in the framework of the Double Degenerate rotationally-driven accretion scenario. We find that the evolutionary properties depend only on the actual mass of the accreting WD and not on the previous history. We determine the expected frequency and amplitude of the gravitational wave emission, which occurs during the mass transfer process and acts as a self-tuning mechanism of the accretion process itself. The gravitational signal related to Galactic sources can be easily detected with the next generation of space-born interferometers and can provide notable constraints to the progenitor model. The expected statistical distribution of pre-explosive objects in the Galaxy is provided also in the effective temperature-apparent bolometric magnitude diagrams which can be used to identify merged DD systems via UV surveys. We emphasize that the thermonuclear explosion occurs owing to the decay of physical conditions keeping over-stable the structure above the classical Chandrasekhar limit and not by a steady increase of the WD mass up to this limit. This conclusion is independent of the evolutionary scenario for the progenitors, but it is a direct consequence of the stabilizing effect of rotation. Such an occurrence is epistemological change of the perspective in defining the ignition process in accreting WDs. Moreover, this requires a long evolutionary period (several million years) to attain the explosion after the above mentioned conditions cease to keep stable the WD. Therefore it is practically impossible to detect the trace of the exploding WD companion in recent pre-explosion frames of even very near SN Ia.
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