Energetic neutral atom imaging of comets

Ekenbäck, A.; Holmström, Mats; Barabash, S.; Gunell, H.

doi:10.1029/2007gl032955

Cited by 8 publications

(11 citation statements)

References 18 publications

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“…The system given in equation 2shows the equations of the ideal MHD adapted for the present problem, with the source terms representing the comet at the right hand [2]. It is used the non-dimensional form, that is, without the constants 4π and µ 0 .…”

Section: The Mhd Modelmentioning

confidence: 99%

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Simulating the interaction of a comet with the solar wind using a magnetohydrodynamic model

Evangelista¹,

Domingues²,

Mendes³

et al. 2016

Proceedings of the 6th International Conference on Nonlinear Science and Complexity

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This paper presents the simulation of the interaction of a comet with the solar wind. It is used the formalism of the ideal magnetohydrodynamics (MHD) in order to simulate the behaviour of such a system. The comet itself is inserted in the equations as a spherically symmetric source of ions. Specifically, this source term represents the process of mass-loading, that is, the phenomenon where the heavy cometary ions are picked up by the solar wind. From the numerical viewpoint, it is used the FLASH code to solve the system of equations of the MHD and to generate the output files. It is investigated the influence of the physical characteristics of the solar wind, such as velocity and magnetic field, on the coma and tail of the comet. This issue is addressed by performing simulations considering, for sake of comparison, three regimes of solar activity, namely: low activity, "mean" or typical activity and intense activity.

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Section: The Mhd Modelmentioning

confidence: 99%

“…It is worth mentioning that such data were collected at the distance of ∼1 AU from the Sun 8 . On the other hand, the data for the typical case are given in [2]. Figures 1-3 show the simulation of the comet for the three scenarios, respectively: calm, typical and intense.…”

Section: Numerical Aspectsmentioning

confidence: 99%

Simulating the interaction of a comet with the solar wind using a magnetohydrodynamic model

Evangelista¹,

Domingues²,

Mendes³

et al. 2016

Proceedings of the 6th International Conference on Nonlinear Science and Complexity

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“…Similar as in Holmström et al [2008] and Ekenbäck et al [2010] we apply the so-called FLASH-code which was developed at the University of Chicago for the study of astrophysical thermonuclear flashes which originate from Xray bursts and super novae explosions [Fryxell et al, 2000]. The FLASH-code provides adaptive grids and is parallelized and extended for a planetary exosphere Direct Simulation Monte Carlo (DSMC) model [Ekenbäck and Holmström 2006;Ekenbäck et al, 2008] which is run by us via the High Performance Computing Center North (HPC2N), Umeå University, in Sweden.…”

Section: Stellar Wind Interaction With Hd 209458b and Production Ofmentioning

confidence: 99%

Exoplanet Magnetic Field Estimation via Energetic Neutral Atoms (ENAs) and Hydrogen Cloud Observations and Modelling

Lämmer¹,

Kislyakova²,

Holmström³

et al. 2011

Planetary Radio Emissions Vii

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The discovery of more than 500 exoplanets during the past 15 years has enabled us to characterize the upper atmosphere structure of some exosolar gas giants and to compare observational and modelling results to the known planets in the Solar System. It is of great interest to understand if these exosolar "Hot Jupiters" share similar physical processes compared to the giant planets (Jupiter and Saturn) in the Solar System with regard to their magnetic dynamos and the corresponding expected magnetic field strengths. In this work we discuss how observations of stellar Lyman-α absorption by so-called Energetic Neutral Atoms (ENAs) around transiting exoplanets together with theoretical modelling efforts can be used as a tool for estimating magnetic obstacle sizes and the corresponding magnetic field strength. For demonstrating this method we model the production of stellar wind related planetary hydrogen and ENA populations around the exosolar gas giant HD 209458b and show how a detailed analysis of attenuation spectra obtained during transits can be used for the estimation of the planet's magnetic obstacle size and hence its dynamo field strength. Our study indicates that the magnetic field strength of HD 209458b which is able to balance the stellar wind plasma flow by a magnetic obstacle around the planet which can explain the observed Lyman-α line profiles observed before and during the transits by HST corresponds to a magnetic dipole moment which is ∼40 % of Jupiters value.

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“…It is worth mentioning that such data were collected at the distance of ∼1 AU from the Sun 8 . On the other hand, the data for the typical case are given in [2]. 4 Results Figures 1-3 show the simulation of the comet for the three scenarios, respectively: calm, typical and intense.…”

Section: Numerical Aspectsmentioning

confidence: 99%

“…The system given in equation (2) shows the equations of the ideal MHD adapted for the present problem, with the source terms representing the comet at the right hand [2]. It is used the non-dimensional form, that is, without the constants 4π and µ 0 .…”

Section: The Mhd Modelmentioning

confidence: 99%

Simulating the interaction of a comet with the solar wind using a magnetohydrodynamic model

Evangelista¹,

Domingues²,

Mendes³

et al. 2017

Proceeding Series of the Brazilian Society of Computational and Applied Mathematics

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Abstract. This paper presents the simulation of the interaction of a comet with the solar wind. It is used the formalism of the ideal magnetohydrodynamics (MHD) in order to simulate the behaviour of such a system. The comet itself is inserted in the equations as a spherically symmetric source of ions. Specifically, this source term represents the process of mass-loading, that is, the phenomenon where the heavy cometary ions are picked up by the solar wind. From the numerical viewpoint, it is used the FLASH code to solve the system of equations of the MHD and to generate the output files. It is investigated the influence of the physical characteristics of the solar wind, such as velocity and magnetic field, on the coma and tail of the comet. This issue is addressed by performing simulations considering, for sake of comparison, three regimes of solar activity, namely: low activity, "mean" or typical activity and intense activity.

show abstract

Energetic neutral atom imaging of comets

Cited by 8 publications

References 18 publications

Simulating the interaction of a comet with the solar wind using a magnetohydrodynamic model

Simulating the interaction of a comet with the solar wind using a magnetohydrodynamic model

Exoplanet Magnetic Field Estimation via Energetic Neutral Atoms (ENAs) and Hydrogen Cloud Observations and Modelling

Simulating the interaction of a comet with the solar wind using a magnetohydrodynamic model

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