Reduction of mass loss by the hot Jupiter WASP-12b due to its magnetic field

Arakcheev, A. S.; Жилкин, А. Г.; Kaigorodov, P. V.; Bisikalo, D. V.; Kosovichev, A. G.

doi:10.1134/s1063772917110014

Cited by 56 publications

(19 citation statements)

References 35 publications

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“…Characteristic size of the cell at the photometric radius of the planet was 0.02R p , while at the outer edge of the computational domain the cell size was equal, approximately, to 0.4R p . The boundary conditions were the same as in our recent work [24]. We carried out two calculations, which differed only in the value of the parameter B 0 , which determines the average magnetic field at the surface of the star.…”

Section: Results Of the Modelingmentioning

confidence: 99%

“…To describe the structure of the flow in the vicinity of hot Jupiter, we will use the system of equations of ideal one-fluid magnetic hydrodynamics with background field [24,35,36]. Under this approach, the full magnetic field B is represented as a superposition of the background magnetic field H and the magnetic field b induced by the currents in the plasma itself, B = H + b.…”

Section: Basic Equationsmentioning

confidence: 99%

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On Possible Types of Magnetospheres of Hot Jupiters

Жилкин

Бисикало

2019

Astron. Rep.

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We show that the orbits of exoplanets of the "hot Jupiter" type, as a rule, are located close to the Alfven point of the stellar wind of the parent star. At this, many hot Jupiters can be located in the sub-Alfven zone in which the magnetic pressure of the stellar wind exceeds its dynamic pressure. Therefore, magnetic field of the wind must play an extremely important role for the flow of the stellar wind around the atmospheres of the hot Jupiters. This factor must be considered both in theoretical models and in the interpretation of observational data. The analysis shows that many typical hot Jupiters should have shock-less intrinsic magnetospheres, which, apparently, do not have counterparts in the Solar System. Such magnetospheres are characterized, primarily, by the absence of the bow shock, while the magnetic barrier (ionopause) is formed by the induced currents in the upper layers of the ionosphere. We confirmed this inference by the three-dimensional numerical simulation of the flow of the parent star stellar wind around the hot Jupiter HD 209458b in which we took into account both proper magnetic field of the planet and magnetic field of the wind. *

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Section: Results Of the Modelingmentioning

confidence: 99%

Section: Basic Equationsmentioning

confidence: 99%

On Possible Types of Magnetospheres of Hot Jupiters

Жилкин

Бисикало

2019

Astron. Rep.

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“…Allowing outflow only along open field lines at latitudes above the sub-stellar point significantly reduced the mass-loss rates below those calculations without strong magnetic fields, or those assumed from one-dimensional calculations that solve for the flow solution only from the sub-stellar point. For field strengths of a few Gauss (comparable to Jupiter's magnetic field) around hot Jupiters, Owen & Adams (2014), Khodachenko et al (2015) and Arakcheev et al (2017) found the mass-loss rates were suppressed by an order of magnitude. The effect of planetary magnetic fields around lower mass super-Earths/mini-Neptunes remains unexplored; however, an order of magnitude correction to the mass-loss rates typically taken from one-dimensional calculations would have significant implications on our understanding of the evolution of close-in, low-mass exoplanets.…”

Section: The Role Of Magnetic Fieldsmentioning

confidence: 99%

Atmospheric Escape and the Evolution of Close-In Exoplanets

Owen

2019

Annu. Rev. Earth Planet. Sci.

249

165

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Exoplanets with substantial Hydrogen/Helium atmospheres have been discovered in abundance, many residing extremely close to their parent stars. The extreme irradiation levels these atmospheres experience causes them to undergo hydrodynamic atmospheric escape. Ongoing atmospheric escape has been observed to be occurring in a few nearby exoplanet systems through transit spectroscopy both for hot Jupiters and lower-mass super-Earths/mini-Neptunes. Detailed hydrodynamic calculations that incorporate radiative transfer and ionization chemistry are now common in one-dimensional models, and multi-dimensional calculations that incorporate magnetic-fields and interactions with the interstellar environment are cutting edge. However, there remains very limited comparison between simulations and observations. While hot Jupiters experience atmospheric escape, the mass-loss rates are not high enough to affect their evolution. However, for lower mass planets atmospheric escape drives and controls their evolution, sculpting the exoplanet population we observe today.

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“…Nonetheless, the presence of strong magnetic fields will act to reduce the overall mass-loss rate. For example, simulations have shown a field strength of 1 gauss is sufficient to reduce the mass-loss rates by an order of magnitude in hot-jupiters (e.g., Adams 2011; Owen & Adams 2014;Arakcheev et al 2017). For the population of close-in super-Earths and mini-Neptunes, an order of magnitude reduction in the mass-loss rates would make ice-rich cores, rather than iron-rich cores, consistent with the observed valley location.…”

Section: Suppression Of Mass-loss By Planetary Magnetic Fieldsmentioning

confidence: 80%

Effects of magnetic fields on the location of the evaporation valley for low-mass exoplanets

Owen

Adams

2019

Monthly Notices of the Royal Astronomical Society

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The observed distribution of radii for exoplanets shows a bimodal form that can be explained by mass-loss from planetary atmospheres due to high energy radiation emitted by their host stars. The location of the minimum of this radius distribution depends on the mass-radius relation, which in turn depends on the composition of planetary cores. Current studies suggest that super-Earth and mini-Neptune planets have ironrich and hence largely Earth-like composition cores. This paper explores how non-zero planetary magnetic fields can decrease the expected mass-loss rates from these planets. These lower mass-loss rates, in turn, affect the location of the minimum of the radius distribution and the inferred chemical composition of the planetary cores.

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Reduction of mass loss by the hot Jupiter WASP-12b due to its magnetic field

Cited by 56 publications

References 35 publications

On Possible Types of Magnetospheres of Hot Jupiters

On Possible Types of Magnetospheres of Hot Jupiters

Atmospheric Escape and the Evolution of Close-In Exoplanets

Effects of magnetic fields on the location of the evaporation valley for low-mass exoplanets

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