Charge Exchange Emission from Solar Wind Helium Ions

Bodewits, Dennis; Hoekstra, Ronnie; Seredyuk, B.; McCullough, R W; Jones, G. H.; Tielens, A. G. G. M.

doi:10.1086/500731

Cited by 56 publications

(92 citation statements)

References 51 publications

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“…This photon emission is called charge exchange emission (cxe) and it has been observed from comets, planets and the interstellar medium in X-rays and the Far-UV (Lisse et al 1996;Krasnopolsky 1997;Snowden et al 2004;Dennerl 2002). The spectral shape of the cxe depends on properties of both the neutral gas and the solar wind and the subsequent emission can therefore be regarded as Appendix A is only available in electronic form at http://www.aanda.org a fingerprint of the underlying interactions (Cravens et al 1997;Kharchenko & Dalgarno 2000, 2001Beiersdorfer et al 2003;Bodewits et al 2004aBodewits et al , 2006.…”

Section: Introductionmentioning

confidence: 99%

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Spectral analysis of theChandracomet survey

Bodewits

Christian²,

Torney³

et al. 2007

A&A

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Aims. We present results of the analysis of cometary X-ray spectra with an extended version of our charge exchange emission model (Bodewits et al. 2006). We have applied this model to the sample of 8 comets thus far observed with the Chandra X-ray observatory and acis spectrometer in the 300-1000 eV range. Methods. The interaction model is based on state selective, velocity dependent charge exchange cross sections and is used to explore how cometary X-ray emission depend on cometary, observational and solar wind characteristics. It is further demonstrated that cometary X-ray spectra mainly reflect the state of the local solar wind. The current sample of Chandra observations was fit using the constrains of the charge exchange model, and relative solar wind abundances were derived from the X-ray spectra. Results. Our analysis showed that spectral differences can be ascribed to different solar wind states, as such identifying comets interacting with (I) fast, cold wind, (II), slow, warm wind and (III) disturbed, fast, hot winds associated with interplanetary coronal mass ejections. We furthermore predict the existence of a fourth spectral class, associated with the cool, fast high latitude wind.

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Section: Introductionmentioning

confidence: 99%

“…We present results of the analysis of cometary X-ray spectra with an extended version of our charge exchange emission model (Bodewits et al 2006). We have applied this model to the sample of 8 comets thus far observed with the Chandra X-ray observatory and acis spectrometer in the 300-1000 eV range.…”

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confidence: 99%

Spectral analysis of theChandracomet survey

Bodewits

Christian²,

Torney³

et al. 2007

A&A

Self Cite

100

131

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“…This is especially attractive for comets since the large size of the interaction region make it difficult to get global, time dependent, information from in-situ measurements. Previously used global techniques for comets include solar wind charge exchange X-rays [Wegmann and Dennerl, 2005] and Extreme Ultraviolet imaging [Bodewits et al, 2006].…”

Section: Introductionmentioning

confidence: 99%

Energetic neutral atom imaging of comets

Ekenbäck

Holmström

Barabash

et al. 2008

Geophysical Research Letters

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[1] We present the first computer simulated images of energetic neutral atoms (ENAs) produced by charge exchange between solar wind protons and cometary neutrals. Proton bulk flow and temperature from MHD simulations are used along with a model of cometary neutral densities. The emission of hydrogen ENAs from the comet is then calculated using cross sections for the charge exchange collisions. The ENA production rate is integrated along lines of sight to produce an image of the fluxes. We find detection of hydrogen ENAs feasible and most favorable at solar zenith angles between 80 and 130 degrees.

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“…First, the charge transfer rates are obtained based on single electron capture in ion-neutral collision. Although multielectron neutral targets might be important for some environments (e.g., comets) where the channels of multi-electron capture do exist (e.g., Bodewits et al 2006), the data available on such reactions are much less complete than those for single electron capture. As shown in the experimental results of, for example, Greenwood et al (2001), single capture can provide a first-order approximation to multi-electron reactions.…”

Section: Assumptionsmentioning

confidence: 99%

Plasma code for astrophysical charge exchange emission at X-ray wavelengths

Kaastra

Raassen

2016

A&A

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Charge exchange X-ray emission provides unique insight into the interactions between cold and hot astrophysical plasmas. Besides its own profound science, this emission is also technically crucial to all observations in the X-ray band, since charge exchange with the solar wind often contributes a significant foreground component that contaminates the signal of interest. By approximating the cross sections resolved to n and l atomic subshells and carrying out complete radiative cascade calculation, we have created a new spectral code to evaluate the charge exchange emission in the X-ray band. Compared to collisional thermal emission, charge exchange radiation exhibits enhanced lines from large-n shells to the ground, as well as large forbidden-to-resonance ratios of triplet transitions. Our new model successfully reproduces an observed high-quality spectrum of comet C/2000 WM1 (LINEAR), which emits purely by charge exchange between solar wind ions and cometary neutrals. It demonstrates that a proper charge exchange model will allow us to probe the ion properties remotely, including charge state, dynamics, and composition, at the interface between the cold and hot plasmas.

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Charge Exchange Emission from Solar Wind Helium Ions

Cited by 56 publications

References 51 publications

Spectral analysis of theChandracomet survey

Spectral analysis of theChandracomet survey

Energetic neutral atom imaging of comets

Plasma code for astrophysical charge exchange emission at X-ray wavelengths

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