WIND-ACCRETION DISKS IN WIDE BINARIES, SECOND-GENERATION PROTOPLANETARY DISKS, AND ACCRETION ONTO WHITE DWARFS
WIND-ACCRETION DISKS IN WIDE BINARIES, SECOND-GENERATION PROTOPLANETARY DISKS, AND ACCRETION ONTO WHITE DWARFS
复制标题
宽双星中的风吸积盘、第二代原行星盘以及白矮星上的吸积
DOI：
10.1088/0004-637x/764/2/169
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发表时间：
2012
期刊：
影响因子：
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通讯作者：
S. Kenyon
中科院分区：
文献类型：
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作者：
H. Perets;S. Kenyon
从演化的施主星星到它的伴星的质量转移是双星演化的标准特征。在宽联星中，伴星星星捕获了主星星在风中喷射的一些质量。被捕获的物质形成一个吸积盘。在这里，我们研究风吸积盘的演变，使用数值方法，使我们能够遵循长期的演变。对于一个广泛的初始条件，我们推导出的径向密度和温度分布的磁盘。在大多数情况下，风吸积会导致在渐近巨分支施主星星的整个生命周期中形成长寿命的稳定盘。这些盘的质量是10−5-10−3 M的数倍，表面密度和温度分布遵循破幂律。圆盘中的总质量与所使用的粘度参数近似线性地成比例。大约有50%-80%的质量落入盘中，并与中心的星星吸积;其余的则从盘的外缘流出，进入主星的恒星风中。对于吸积速率大的系统，次级吸积高达0.1 M。当次级恒星是一颗白色矮星时，吸积自然会导致新星和超新星爆发。对于所有类型的二级星星，大质量盘的表面密度和温度分布类似于在原行星盘中观察到的结构，这表明协调的观测计划可能会提高我们对不确定的盘物理的理解。
Mass transfer from an evolved donor star to its binary companion is a standard feature of stellar evolution in binaries. In wide binaries, the companion star captures some of the mass ejected in a wind by the primary star. The captured material forms an accretion disk. Here, we study the evolution of wind-accretion disks, using a numerical approach which allows us to follow the long-term evolution. For a broad range of initial conditions, we derive the radial density and temperature profiles of the disk. In most cases, wind accretion leads to long-lived stable disks over the lifetime of the asymptotic giant branch donor star. The disks have masses of a few times 10−5–10−3 M☉, with surface density and temperature profiles that follow broken power laws. The total mass in the disk scales approximately linearly with the viscosity parameter used. Roughly, 50%–80% of the mass falling into the disk accretes onto the central star; the rest flows out through the outer edge of the disk into the stellar wind of the primary. For systems with large accretion rates, the secondary accretes as much as 0.1 M☉. When the secondary is a white dwarf, accretion naturally leads to nova and supernova eruptions. For all types of secondary star, the surface density and temperature profiles of massive disks resemble structures observed in protoplanetary disks, suggesting that coordinated observational programs might improve our understanding of uncertain disk physics.