Multi-Component MHD Model of Hot Jupiter Envelopes

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 f...

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Autores principales:	Andrey Zhilkin, Dmitri Bisikalo
Formato:	article
Lenguaje:	EN
Publicado:	MDPI AG 2021
Materias:	numerical simulation magnetic hydrodynamics (MHD) hot Jupiters Elementary particle physics QC793-793.5
Acceso en línea:	https://doaj.org/article/88e357a64e5240ec90c3e1f514178cc1
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spelling	oai:doaj.org-article:88e357a64e5240ec90c3e1f514178cc12021-11-25T19:09:38ZMulti-Component MHD Model of Hot Jupiter Envelopes10.3390/universe71104222218-1997https://doaj.org/article/88e357a64e5240ec90c3e1f514178cc12021-11-01T00:00:00Zhttps://www.mdpi.com/2218-1997/7/11/422https://doaj.org/toc/2218-1997A 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.Andrey ZhilkinDmitri BisikaloMDPI AGarticlenumerical simulationmagnetic hydrodynamics (MHD)hot JupitersElementary particle physicsQC793-793.5ENUniverse, Vol 7, Iss 422, p 422 (2021)
institution	DOAJ
collection	DOAJ
language	EN
topic	numerical simulation magnetic hydrodynamics (MHD) hot Jupiters Elementary particle physics QC793-793.5
spellingShingle	numerical simulation magnetic hydrodynamics (MHD) hot Jupiters Elementary particle physics QC793-793.5 Andrey Zhilkin Dmitri Bisikalo Multi-Component MHD Model of Hot Jupiter Envelopes
description	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.
format	article
author	Andrey Zhilkin Dmitri Bisikalo
author_facet	Andrey Zhilkin Dmitri Bisikalo
author_sort	Andrey Zhilkin
title	Multi-Component MHD Model of Hot Jupiter Envelopes
title_short	Multi-Component MHD Model of Hot Jupiter Envelopes
title_full	Multi-Component MHD Model of Hot Jupiter Envelopes
title_fullStr	Multi-Component MHD Model of Hot Jupiter Envelopes
title_full_unstemmed	Multi-Component MHD Model of Hot Jupiter Envelopes
title_sort	multi-component mhd model of hot jupiter envelopes
publisher	MDPI AG
publishDate	2021
url	https://doaj.org/article/88e357a64e5240ec90c3e1f514178cc1
work_keys_str_mv	AT andreyzhilkin multicomponentmhdmodelofhotjupiterenvelopes AT dmitribisikalo multicomponentmhdmodelofhotjupiterenvelopes
_version_	1718410229366915072

Multi-Component MHD Model of Hot Jupiter Envelopes

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