论文标题
透明的窗口，进入早期型恒星变异性
A Transparent Window into Early-Type Stellar Variability
论文作者
论文摘要
地下对流区域在早期型星中无处不在。在狭窄的不透明度峰的驱动下，这些薄的对流区域很少传输热量，但在设置恒星的磁性特性和表面变异性方面起着重要作用。在这里，我们证明了这些对流区域是\ emph {not}，如前所述的恒星中存在。特别是，有一些区域是1D恒星进化模型报告的对流不稳定，但在对流发作的情况下低于关键的瑞利数字。为了获得亚微度金属性，这将打开一个没有地下对流区域的\ emph {stosity窗口}。对于LMC金属性，此表面稳定区域大约在$ 8M_ \ ODOT $和1600万美元\ ODOT $之间，增加到800万美元\ odot $ - $ 3500万\ odot $用于SMC金属性。然后，此类窗口是探测大型恒星中地下对流和其他光度变异源的相对影响的绝佳目标。
Subsurface convection zones are ubiquitous in early-type stars. Driven by narrow opacity peaks, these thin convective regions transport little heat but play an important role in setting the magnetic properties and surface variability of stars. Here we demonstrate that these convection zones are \emph{not} present in as wide a range of stars as previously believed. In particular, there are regions which 1D stellar evolution models report to be convectively unstable but which fall below the critical Rayleigh number for onset of convection. For sub-solar metallicity this opens up a \emph{stability window} in which there are no subsurface convection zones. For LMC metallicity this surface stability region extends roughly between $8M_\odot$ and $16M_\odot$, increasing to $8M_\odot$ -- $35M_\odot$ for SMC metallicity. Such windows are then an excellent target for probing the relative influence of subsurface convection and other sources of photometric variability in massive stars.
