The Simulation of Nova Evolution with Optically Thick Winds
The Simulation of Nova Evolution with Optically Thick Winds
复制标题
光学厚风下新星演化的模拟
DOI：
10.1086/305280
复制
发表时间：
1998
期刊：
影响因子：
--
通讯作者：
A. Kovetz
中科院分区：
文献类型：
--
作者：
A. Kovetz
致密星星表面的热核逃逸是由于富含核燃料的物质的吸积，导致物质通过光学厚风被驱逐。对这种现象的模拟要么依赖于恒星演化代码，其中添加了一些特别的质量损失处方，要么依赖于风方程的积分，类似的特别处方用于构建一系列这样的解决方案，以代表不断发展的爆炸。本文提出了一种结合上述两种极端情况的方法。两点边值风问题是由一个有效的松弛算法。然后将风场解作为恒星程序的外边界条件。恒星演化与光学厚风的自洽结合足够快，并且用途广泛，可以处理致密星星表面附近的热核爆炸。一个例子是一个中等速度（t3 = 49天）的经典新星爆发的模拟。整个风相可以被详细地跟踪：由此产生的可见光曲线类似于实际的中等速度的新星，并且膨胀速度是正确的大小。
Thermonuclear runaways at the surface of a compact star, due to accretion of nuclear fuel-rich matter, lead to expulsion of matter through optically thick winds. Simulations of such phenomena have relied either on stellar evolution codes, to which some ad hoc prescriptions for mass loss were added, or on integrations of the wind equations, with a similarly ad hoc prescription for the construction of a sequence of such solutions to represent an evolving explosion. A method is presented which combines the foregoing two extremes. The two-point boundary-value wind problem is solved by an efficient relaxation algorithm. And the wind solution is then used as an outer boundary condition in the stellar code. The self-consistent combination of stellar evolution with an optically thick wind is sufficiently fast, and versatile, to handle thermonuclear explosions near the surface of a compact star. An example is given of the simulation of a moderately fast (t3 = 49 days) classical nova outburst. The entire wind phase can be followed in detail: the resulting visual light curve resembles those of actual moderately fast novae, and the expansion velocity is of the right magnitude.