Abstract
A numerical model description of a hot Jupiter extended envelope based on the approximation of multi-component magnetic hydrodynamics is presented. The main attention is focused on the problem of implementing the completed MHD stellar wind model. As a result, the numerical model becomes applicable for calculating the structure of the extended envelope of hot Jupiters not only in the super-Alfvén and sub-Alfvén regimes of the stellar wind flow around and in the trans-Alfvén regime. The multi-component MHD approximation allows the consideration of changes in the chemical composition of hydrogen–helium envelopes of hot Jupiters. The results of calculations show that, in the case of a super-Alfvén flow regime, all the previously discovered types of extended gas-dynamic envelopes are realized in the new numerical model. With an increase in magnitude of the wind magnetic field, the extended envelope tends to become more closed. Under the influence of a strong magnetic field of the stellar wind, the envelope matter does not move along the ballistic trajectory but along the magnetic field lines of the wind toward the host star. This corresponds to an additional (sub-Alfvénic) envelope type of hot Jupiters, which has specific observational features. In the transient (trans-Alfvén) mode, a bow shock wave has a fragmentary nature. In the fully sub-Alfvén regime, the bow shock wave is not formed, and the flow structure is shock-less.
Highlights
Hot Jupiters are giant exoplanets with masses on the order of Jupiter’s mass, located in the immediate vicinity of a host star [1]
To investigate the process of the stellar wind matter flowing around hot Jupiters, considering both the planet own magnetic field and the wind magnetic field, we developed a three-dimensional numerical model based on the approximation of multi-component magnetic hydrodynamics
Our numerical model is based on the Roe–Einfeldt–Osher difference scheme of high resolution for the equations of multi-component magnetic hydrodynamics (MHD)
Summary
Hot Jupiters are giant exoplanets with masses on the order of Jupiter’s mass, located in the immediate vicinity of a host star [1]. Due to the close location to the host star and the relatively large size, gas envelopes of hot Jupiters can overfill their Roche lobes, resulting in intense gas outflows both at the night side (near the Lagrange point L2) and at the day side (near the inner Lagrange point L1) of the planet [3,4] The presence of such outflows is indirectly indicated by the excessive absorption of radiation in the near ultraviolet range observed in some hot Jupiters during their transit across the disk of their host star [5,6,7,8,9,10,11]. The study of the structure of gas envelopes of such objects is one of the most urgent problems of modern astrophysics [16]
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