Trachenko K, Brazhkin V V, Bolmatov D
South East Physics Network and School of Physics and Astronomy, Queen Mary University of London, Mile End Road, London E1 4NS, United Kingdom.
Institute for High Pressure Physics, RAS, Moscow 142190, Russia.
Phys Rev E Stat Nonlin Soft Matter Phys. 2014 Mar;89(3):032126. doi: 10.1103/PhysRevE.89.032126. Epub 2014 Mar 21.
Understanding the physics of gas giants requires knowledge about the behavior of hydrogen at extreme pressures and temperatures. Molecular hydrogen in these planets is supercritical, and has been considered as a physically homogeneous state where no differences can be made between a liquid and a gas and where all properties undergo no marked or distinct changes with pressure and temperature, the picture believed to hold below the dissociation and metallization transition. Here, we show that in Jupiter and Saturn, supercritical molecular hydrogen undergoes a dynamic transition around 10 GPa and 3000 K from the "rigid" liquid state to the "nonrigid" gas-like fluid state at the Frenkel line recently proposed, with the accompanying qualitative changes of all major physical properties. The consequences of this finding are discussed, including a physically justified way to demarcate the interior and the atmosphere in gas giants.
了解气态巨行星的物理性质需要掌握氢在极端压力和温度下的行为。这些行星中的分子氢处于超临界状态，一直被视为一种物理上均匀的状态，在这种状态下，液体和气体之间没有区别，所有性质随压力和温度的变化都不显著，人们认为这种情况在解离和金属化转变温度以下成立。在此，我们表明，在木星和土星中，超临界分子氢在最近提出的弗伦克尔线处，于约10吉帕和3000开尔文的条件下经历从“刚性”液态到“非刚性”气态流体状态的动态转变，同时所有主要物理性质发生定性变化。我们讨论了这一发现的后果，包括一种从物理角度合理划分气态巨行星内部和大气层的方法。
