热磁星相干射电辐射和物理参数之间标度关系的检验
Testing a scaling relation between coherent radio emission and physical parameters of hot magnetic stars
摘要：
来自热磁星的电子回旋脉泽辐射（ECME）的相干射电辐射在二十多年前就被发现了，但是使ECME产生有利的物理条件仍然不确定。直到最近才有人提出一个经验关系，将ECME光度与恒星的磁场和温度联系起来，解释是什么使热磁星能够产生ECME。然而，这个关系仅用14颗星就得到了。因此，重要的是要检查这种关系是否稳健。为了测试鲁棒性，我们对五颗热磁星进行了射电观测。这导致了另外三颗产生ECME的恒星的发现。我们发现，建议的标度关系仍然有效后，新发现的恒星。然而，我们发现磁场和有效温度与$T_\mathrm{eff}\lesssim 16$ kK相关（可能是小样本量的伪影），使得ECME光度和$T_\mathrm{eff}$之间的联系不可靠。根据非相干射电辐射的标度律检验了经验关系，得出了两种类型的辐射都是由相同的磁层现象提供动力的结论。像非相干辐射一样，对于晚B型和A型恒星，相干射电辐射与$T_\mathrm{eff}$无关，但对于早B型恒星，$T_\mathrm{eff}$似乎变得很重要，这可能是由于较高的吸收，或者是发射点较高的等离子体密度抑制了发射的产生。
英文摘要：
Coherent radio emission via electron cyclotron maser emission (ECME) from hot magnetic stars was discovered more than two decades ago, but the physical conditions that make the generation of ECME favourable remain uncertain. Only recently was an empirical relation, connecting ECME luminosity with the stellar magnetic field and temperature, proposed to explain what makes a hot magnetic star capable of producing ECME. This relation was, however, obtained with just fourteen stars. Therefore, it is important to examine whether this relation is robust. With the aim of testing the robustness, we conducted radio observations of five hot magnetic stars. This led to the discovery of three more stars producing ECME. We find that the proposed scaling relation remains valid after the addition of the newly discovered stars. However we discovered that the magnetic field and effective temperature correlate for $T_\mathrm{eff}\lesssim 16$ kK (likely an artifact of the small sample size), rendering the proposed connection between ECME luminosity and $T_\mathrm{eff}$ unreliable. By examining the empirical relation in light of the scaling law for incoherent radio emission, we arrive at the conclusion that both types of emission are powered by the same magnetospheric phenomenon. Like the incoherent emission, coherent radio emission is indifferent to $T_\mathrm{eff}$ for late-B and A-type stars, but $T_\mathrm{eff}$ appears to become important for early-B type stars, possibly due to higher absorption, or, higher plasma density at the emission sites suppressing the production of the emission.
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