Combining multiple structural inversions to constrain the solar modelling problem
Combining multiple structural inversions to constrain the solar modelling problem
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结合多个结构反演来约束太阳建模问题
DOI：
10.1051/0004-6361/201833971
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发表时间：
2019
影响因子：
6.5
通讯作者：
Buldgen G
中科院分区：
文献类型：
--
作者：
Buldgen G
上下文太阳是所有恒星中研究最多的，它是宇宙中所有其他观测到的恒星的参考。此外，它还充当基础物理学的特权实验室，可以帮助我们更好地了解在地球上不可复制的条件下发生的过程。然而，我们对我们的星星的理解目前减少了所谓的太阳建模问题，从理论太阳模型的比较日震的限制。这些差异可能源于各种原因，如辐射不透明度，状态方程以及化学元素的混合。目标。通过分析结合多个地震反演信息的潜力，我们的目标是帮助解开太阳能建模问题的起源。我们结合反演的绝热声速，熵代理和勒杜判别与其他约束条件，如对流区的基地和光球氦丰度的位置。首先，我们测试了可用于太阳建模的标准成分的各种组合，如丰度表，状态方程，对流和扩散的形式主义和不透明度表。其次，我们研究了诊断潜力的反演模型，包括特设修改的不透明度配置文件和额外的混合下的对流信封。结果我们表明，结合反演提供了严格的限制所需的修改，太阳能成分，远远超出了可以实现的声速反演。我们约束太阳能模型中所需的不透明度增加的形式和幅度，并表明在log T = 6.35时增加15%提供了显着的改善，但本身是不够的。一个更全球性的增加不透明度，在目前的表格的不确定性，再加上一个本地化的额外的混合在对流区的底部提供了最好的协议低金属丰度模型。我们发现，高金属丰度模型并不满足所有的反演结果。我们的结论是，太阳能建模问题可能发生从多个小的贡献者，作为其他成分，如状态方程或对流的形式主义可以引起小，但显着的变化模型，并使用相移分析结合我们的方法是下一步更好地了解太阳能模型的不准确性低于对流包络。
Context. The Sun is the most studied of all stars, which serves as a reference for all other observed stars in the Universe. Furthermore, it also serves the role of a privileged laboratory of fundamental physics and can help us better understand processes occuring in conditions irreproducible on Earth. However, our understanding of our star is currently lessened by the so-called solar modelling problem, resulting from comparisons of theoretical solar models to helioseismic constraints. These discrepancies can stem from various causes, such as the radiative opacities, the equation of state as well as the mixing of the chemical elements. Aims. By analysing the potential of combining information from multiple seismic inversions, our aim is to help disentangle the origins of the solar modelling problem.Methods. We combined inversions of the adiabatic sound speed, an entropy proxy and the Ledoux discriminant with other constraints such as the position of the base of the convective zone and the photospheric helium abundance. First, we tested various combinations of standard ingredients available for solar modelling such as abundance tables, equation of state, formalism for convection and diffusion and opacity tables. Second, we studied the diagnostic potential of the inversions on models including ad hoc modifications of the opacity profile and additional mixing below the convective envelope. Results. We show that combining inversions provides stringent constraints on the required modifications to the solar ingredients, far beyond what can be achieved from sound speed inversions alone. We constrain the form and amplitude of the opacity increase required in solar models and show that a 15% increase at log T= 6.35 provides a significant improvement, but is insufficient on its own. A more global increase in the opacity, within the uncertainties of the current tables, coupled with a localized additional mixing at the bottom of the convective zone provides the best agreement for low-metallicity models. We show that high-metallicity models do not satisfy all the inversion results. We conclude that the solar modelling problem likely occurs from multiple small contributors, as other ingredients such as the equation of state or the formalism of convection can induce small but significant changes in the models and that using phase shift analyses combined with our approach is the next step for a better understanding of the inaccuracies of solar models just below the convective envelope.
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影响因子：
4.8
作者：
G. Buldgen;S. Salmon;M. Godart;A. Noels;R. Scuflaire;M. Dupret;D. Reese;J. Colgan;C. Fontes;P. Eggenberger;P. Hakel;D. Kilcrease;O. Richard
通讯作者：
G. Buldgen;S. Salmon;M. Godart;A. Noels;R. Scuflaire;M. Dupret;D. Reese;J. Colgan;C. Fontes;P. Eggenberger;P. Hakel;D. Kilcrease;O. Richard
通过地震反演估计恒星平均密度
影响因子：
6.5
作者：
Reese D
通讯作者：
Reese D
太阳等离子体：热力学函数和状态方程的计算
DOI：
--
发表时间：
2006
期刊：
影响因子：
--
作者：
V. Gryaznov;S. Ayukov;V. A. Baturin;I. Iosilevskiy;A. N. Starostin;V. Fortov
通讯作者：
V. Fortov
部分电离太阳等离子体中的元素扩散和分离过程
DOI：
--
发表时间：
2010
期刊：
影响因子：
--
作者：
A. Gorshkov;V. Baturin
通讯作者：
V. Baturin
太阳和恒星物理学的进展：日震学和星震学的新时代
DOI：
--
发表时间：
2013
期刊：
影响因子：
--
作者：
L. P.;T. A.;L. H.;D. J.;B. P.G.;B. S.;K. N.;D. A.;S. J.;T. P.;T. J.
通讯作者：
T. J.