论文标题
星号学：在红色超级巨星Alpha Ori中寻找轴
Asteroseismology: Looking for axions in the red supergiant star Alpha Ori
论文作者
论文摘要
在这项工作中，我们首次使用地震数据和表面丰度来对超级巨头$α$ -ORI进行建模，目的是设置轴 - 光子耦合常数$ g_ g_ g_ {aγ} $的上限。我们发现，总的来说，在[0.002; 2.0] \ times 10^{ - 10} {\ rm gev}^{ - 1} $中具有$ g_ {aγ} \的恒星模型与观察数据相一致，但是在该上限之外，我们并未找到与观察性约束构成的Stellar模型。从$ g_ {aγ} = 3.5 \ times 10^{ - 10} {\ rm gev}^{ - 1} $ on，该算法找不到任何拟合模型。然而，所有考虑的所有轴子模型都呈现出与参考案例的独特内部轮廓，而没有轴。此外，随着轴心能量损失变得越来越重要，即使具有非常相似的输入参数，恒星模型的行为也会变得更加多样化。但是，$ g_ {aγ} $的连续增量仍然显示出系统的趋势，这是由于轴突能量损失所致。此外，我们建立了三个重要的结论：（1）亮度增加和中微子产生的增加是可测量的效果，可能与轴突能量损失有关。 （2）带有轴心能量损失的恒星模型显示出非常不同的内部结构。 （3）未来的星号传教士在观察大型恒星中低度非降低模式中的重要性：内部重力波探测轴法效应最强烈的近核区域。因此，更多的地震数据将使我们能够更好地限制$ g_ {aγ} $，并证明或忽略大型恒星内轴心能量损失的存在。
In this work, for the first time, we use seismic data as well as surface abundances to model the supergiant $α$-Ori, with the goal of setting an upper bound on the axion-photon coupling constant $g_{aγ}$. We found that, in general, the stellar models with $g_{a γ} \in [0.002;2.0]\times 10^{-10}{\rm GeV}^{-1}$ agree with observational data, but beyond that upper limit, we did not find stellar models compatible with the observational constraints, and current literature. From $g_{a γ} = 3.5 \times 10^{-10} {\rm GeV}^{-1}$ on, the algorithm did not find any fitting model. Nevertheless, all axionic models considered, presented a distinct internal profile from the reference case, without axions. Moreover, as axion energy losses become more significant, the behaviour of the stellar models becomes more diversified, even with very similar input parameters. Nonetheless, the consecutive increments of $g_{a γ}$ still show systematic tendencies, resulting from the axion energy losses. Moreover, we establish three important conclusions: (1) The increased luminosity and higher neutrino production are measurable effects, possibly associated with axion energy losses. (2) Stellar models with axion energy loss show a quite distinct internal structure. (3) The importance of future asteroseismic missions in observing low-degree non-radial modes in massive stars:internal gravity waves probe the near-core regions, where axion effects are most intense. Thus, more seismic data will allow us to constrain $g_{aγ}$ better and prove or dismiss the existence of axion energy loss inside massive stars.
