X‐ray imaging of the solar wind—Mars interaction

Holmström, Mats; Barabash, S.; Kallio, Esa

doi:10.1029/2000gl012381

Cited by 47 publications

(43 citation statements)

References 14 publications

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“…If we also adjust to the average slow SW ion abundances, then our simulated luminosity can reach between 1.2 and 2.0 MW, which brings us to almost perfect agreement with previous simulations (Krasnopolsky 2000;Holmström et al 2001;Gunell et al 2004), but still a far way from the observed values.…”

Section: Discussionsupporting

confidence: 69%

“…Previous simulations from Holmström et al (2001) with similar SW conditions (V sw = 400 km s −1 , n sw = 2.5 cm −3 ) yielded 2.4 MW (1.52 × 10 25 eV/s) for solar minimum and 1.5 MW (0.93 × 10 25 eV/s) for solar maximum conditions of the neutral coronas, within a 10 R M radius. On the other hand, Gunell et al (2004) find 1.8 MW for a 6 R M simulation box (with V sw = 330 km s −1 , n sw = 4.4 cm −3 inputs).…”

Section: Discussionmentioning

confidence: 99%

“…Martian CX emission was predicted for the first time by Cravens (2000), and the first estimates of the Martian SWCX emission based on comet observations and calculations were given by Krasnopolsky (2001). Following that, the first model of minor ion propagation through a simplified SW-Martian exosphere interface was devised by Holmström et al (2001). Thanks to the absence of an internal magnetic field, the SW can interact directly with the upper martian atmosphere, and CX collisions between multiply charged heavy SW ions and atmospheric neutral constituents may occur at high altitudes.…”

Section: Introductionmentioning

confidence: 99%

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Solar wind charge exchange X-ray emission from Mars

Koutroumpa¹,

Modolo²,

Chanteur³

et al. 2012

A&A

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Aims. We study the soft X-ray emission induced by charge exchange (CX) collisions between solar-wind, highly charged ions and neutral atoms of the Martian exosphere. Methods. A 3D multispecies hybrid simulation model with improved spatial resolution (130 km) is used to describe the interaction between the solar wind and the Martian neutrals. We calculated velocity and density distributions of the solar wind plasma in the Martian environment with realistic planetary ions description, using spherically symmetric exospheric H and O profiles. Following that, a 3D test-particle model was developed to compute the X-ray emission produced by CX collisions between neutrals and solar wind minor ions. The model results are compared to XMM-Newton observations of Mars. Results. We calculate projected X-ray emission maps for the XMM-Newton observing conditions and demonstrate how the X-ray emission reflects the Martian electromagnetic structure in accordance with the observed X-ray images. Our maps confirm that X-ray images are a powerful tool for the study of solar wind-planetary interfaces. However, the simulation results reveal several quantitative discrepancies compared to the observations. Typical solar wind and neutral coronae conditions corresponding to the 2003 observation period of Mars cannot reproduce the high luminosity or the corresponding very extended halo observed with XMM-Newton. Potential explanations of these discrepancies are discussed.

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Section: Discussionsupporting

confidence: 69%

Section: Discussionmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

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Solar wind charge exchange X-ray emission from Mars

Koutroumpa¹,

Modolo²,

Chanteur³

et al. 2012

A&A

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“…This was the result of numerical simulations (Holmström et al 2001, Plate 1), which predicted a crescent-like structure that resembles (on a smaller scale) the observed emission in ionized carbon (Fig. 7f).…”

Section: Fig 8 A) Superposition Of the Rgs Images Inmentioning

confidence: 99%

First observation of Mars with XMM-Newton

Dennerl

Lisse

Bhardwaj

et al. 2006

A&A

119

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In the first observation of Mars with XMM-Newton, on 20−21 November 2003, this planet is clearly detected as an X-ray source. High resolution X-ray spectroscopy with the Reflection Grating Spectrometer (RGS) confirms that the X-ray radiation from Mars is composed of two different components: one due to fluorescent scattering of solar X-rays in its upper atmosphere and the other one due to solar wind charge exchange in its exosphere. Close to Mars, the RGS spectrum is dominated by two pronounced CO 2 fluorescence lines at 23.5 Å and 23.7 Å. Fluorescence from N 2 at 31.5 Å is also observed. With increasing distance from Mars, these lines fade, while numerous (∼12) emission lines become prominent at the positions expected for de-excitation of highly ionized C, N, O, and Ne atoms, strongly resembling a cometary X-ray spectrum. The He-like O 6+ multiplet is resolved and is dominated by the spin-forbidden magnetic dipole transition 2 3 S 1 → 1 1 S 0 , confirming charge exchange as the origin of the emission, while the resonance line 2 1 P 1 → 1 1 S 0 increases in intensity closer to Mars, where the density of the exosphere is higher. The high spectral dispersion and throughput of XMM-Newton / RGS make it possible to produce X-ray images of the Martian exosphere in individual emission lines, free from fluorescent radiation. They show extended emission out to ∼8 Mars radii, with morphological differences between individual ions and ionization states. This is the first definite detection of charge exchange induced X-ray emission from the exosphere of another planet, providing a direct link to cometary X-ray emission.

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“…The geometry of the solar wind flow around the ionospheric obstacles of these nonmagnetized planets resembles that around the Earth's magnetosphere. In 2001 the Chandra X-ray observatory detected an X-ray halo due to solar wind charge exchange around Mars [Gunell et al, 2004;Holmström et al, 2001]. In 2006 and 2007, Chandra observations also revealed that the Venusian exosphere emits solar wind charge exchange soft X-rays [Dennerl, 2008].…”

Section: Imaging the Magnetospherementioning

confidence: 99%

Astrophysics Noise: A Space Weather Signal

et al. 2010

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Imagine the accuracy of terrestrial weather forecasts if society relied on only a handful of isolated weather stations to supply all the input to meteorological models. Yet that is precisely the daunting situation faced by space weather forecasters, who seek to predict when and how ejections of plasma from the Sun will interact with the Earth's magnetosphere. These interactions can damage spacecraft electronics, produce spurious global positioning and navigation readings, interfere with radio communications, and disrupt electrical power line grids on the ground. Though modern society increasingly relies on satellite technology and electrical conveniences, only a handful of operating heliophysics missions supply the bulk of space weather model inputs.

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X‐ray imaging of the solar wind—Mars interaction

Cited by 47 publications

References 14 publications

Solar wind charge exchange X-ray emission from Mars

Solar wind charge exchange X-ray emission from Mars

First observation of Mars with XMM-Newton

Astrophysics Noise: A Space Weather Signal

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