Laboratory simulation of cometary X-rays using a high-resolution microcalorimeter

Beiersdörfer, P.; Chen, H.; Boyce, K. R.; Brown, G. V.; Kelley, R. L.; Kilbourne, C. A.; Porter, F. S.; Kahn, S. M.

doi:10.1016/j.nimb.2005.03.156

Cited by 5 publications

(5 citation statements)

References 25 publications

(36 reference statements)

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“…Another study that we compare our theoretical data to is that of Beiersdorfer et al (2005) who used the same microcalorimeter spectrometer originally designed for the Astro-E mission. In Figure 6, we present theoretical spectra for O 8+ collisions with N 2 at a collision energy of 10 eV/u compared to the EBIT measurements that have an estimated collision energy of ∼10 eV/u.…”

Section: Appendixmentioning

confidence: 99%

Line Ratios for Solar Wind Charge Exchange with Comets

Mullen

Cumbee

Lyons

et al. 2017

ApJ

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Charge exchange (CX) has emerged in X-ray emission modeling as a significant process that must be considered in many astrophysical environments -particularly comets. Comets host an interaction between solar wind ions and cometary neutrals to promote solar wind charge exchange (SWCX). Xray observatories provide astronomers and astrophysicists with data for many X-ray emitting comets that are impossible to accurately model without reliable charge exchange data. Here, we utilize a streamlined set of computer programs incorporating multi-channel Landau-Zener theory and a cascade model for X-ray emission to generate cross sections and X-ray line ratios for a variety of bare and non-bare ion single electron capture (SEC) collisions. Namely, we consider collisions between the solar wind constituent bare and H-like ions of C, N, O, Ne, Na, Mg, Al, and Si and the cometary neutrals H 2 O, CO, CO 2 , OH, and O. To exemplify the application of this data, we model the X-ray emission of Comet C/2000 WM1 (linear) using the CX package in SPEX (Gu et al. 2016) and find excellent agreement with observations made with the XMM-Newton RGS detector. Our analyses show that the X-ray intensity is dominated by SWCX with H while H 2 O plays a secondary role. This is the first time, to our knowledge, that CX cross sections have been implemented into a X-ray spectral fitting package to determine the H to H 2 O ratio in cometary atmospheres. The CX data sets are incorporated into the modeling packages SPEX (Gu et al. 2016) and Kronos (Mullen et al. 2016).

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Section: Appendixmentioning

confidence: 99%

Line Ratios for Solar Wind Charge Exchange with Comets

Mullen

Cumbee

Lyons

et al. 2017

ApJ

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“…The striping is due to the survey geometry where great circles on the sky including the ecliptic poles were scanned precessing at ~1° per day. The spectra were measured on an electron beam ion trap at the Lawrence Livermore National Laboratory by Beiersdorfer et al (2005b). Note that Lyman-ε emanating from n = 6 is only seen in (a).…”

Section: Figure 47mentioning

confidence: 99%

“…High-resolution laboratory measurements have now revealed some of the details of the emission near the limit of the Lyman series (Beiersdorfer et al 2003(Beiersdorfer et al , 2005b. Replacing the rather low-resolution solid-state detectors used in the above-mentioned measurements with a microcalorimeter has enabled Beiersdorfer et al to resolve the Lyman lines, as illustrated in Fig.…”

Section: K-shell X-ray Spectramentioning

confidence: 99%

X-rays from solar system objects

Bhardwaj

Elsner²,

Gladstone³

et al. 2007

Planetary and Space Science

136

115

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During the last few years our knowledge about the X-ray emission from bodies within the solar system has significantly improved. Several new solar system objects are now known to shine in X-rays at energies below 2 keV. Apart from the Sun, the known X-ray emitters now include planets (Venus, Earth, Mars, Jupiter, and Saturn), planetary satellites (Moon, Io, Europa, and Ganymede), all active comets, the Io plasma torus (IPT), the rings of Saturn, the coronae (exospheres) of Earth and Mars, and the heliosphere. The advent of higher-resolution X-ray spectroscopy with the Chandra and XMM-Newton X-ray observatories has been of great benefit in advancing the field of planetary X-ray astronomy. Progress in modeling X-ray emission, laboratory studies of X-ray production, and theoretical calculations of cross-sections, have all contributed to our understanding of processes that produce X-rays from the solar system bodies. At Jupiter and Earth, both auroral and non-auroral disk X-ray emissions have been observed. X-rays have been detected from Saturn's disk, but no convincing evidence of an X-ray aurora has been observed. The first soft (0.1- 2 keV) X-ray observation of Earth's aurora by Chandra shows that it is highly variable. The non-auroral X-ray emissions from Jupiter, Saturn, and Earth, those from the disk of Mars, Venus, and Moon, and from the rings of Saturn, are mainly produced by scattering of solar X-rays. The spectral characteristics of X-ray emission from comets, the heliosphere, the geocorona, and the Martian halo are quite similar, but they appear to be quite different from those of Jovian auroral X-rays. X-rays from the Galilean satellites and the IPT are mostly driven by impact of Jovian magnetospheric particles. This paper reviews studies of the soft X-ray emission from the solar system bodies, excluding the Sun

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“…This strong enhancement of high-n Lyman emission is a key feature of low-collision-energy CX spectra. H-like CX spectra have also been obtained using EBITs for Xe 54+ + Xe [115,123], Ne 10+ + Ne [126,127], and O 8+ + various molecules [36]; the last two measurements used the XRS microcalorimeter.…”

Section: H-like Spectramentioning

confidence: 99%

EBIT charge-exchange measurements and astrophysical applications

Wargelin¹,

Beiersdörfer²,

Brown³

2008

Can. J. Phys.

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The past decade has seen a surge of interest in astrophysical charge exchange (CX). The impetus was the discovery of X-ray emission from comets in 1996, soon followed by the observation of CX emission in planetary atmospheres and throughout the heliosphere. Geocoronal and heliospheric CX are now recognized as contributing a considerable fraction of the soft X-ray background, and stellar-wind charge exchange is expected to occur in the astrospheres surrounding many stars. CX may also contribute to X-ray line emission in supernova remnants, the Galactic Center, and the Galactic Ridge. This article summarizes the key aspects of CX X-ray emission and its astrophysical relevance, and reviews related laboratory measurements and theoretical predictions with particular attention to spectroscopy experiments conducted on electron beam ion traps. PACS Nos.: 32.30. Rj, 34.70.+e, 39.10.+j, 95.30.Dr Résumé : La dernière décennie a vu croître l'intérêt pour les réactions d'échange de charge (CX) en astrophysique. La raison vient de la découverte d'émission-X par les comètes en 1996, rapidement suivie par l'observation d'émission CX dans les atmosphères planétaires et dans toute l'héliosphère. Nous croyons aujourd'hui que ces deux derniers types de source contribuent une fraction importante du signal de fond de rayons-X mous et on peut s'attendre à des échanges de charge dans les vents stellaires que l'on retrouve dans les atmosphères entourant beaucoup d'étoiles. Les émissions CX peuvent contribuer aux émissions-X dans les vestiges de supernova, le centre galactique et la dorsale galactique. Nous présentons ici un sommaire des aspects clés de l'émission-X par mécanisme CX et de son intérêt en astrophysique et passons en revue les mesures en laboratoire et les calculs théoriques pertinents, portant une attention spéciale aux expériences de spectroscopie faites à l'aide de pièges électroniques à faisceau d'électrons.[Traduit par la Rédaction]

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Laboratory simulation of cometary X-rays using a high-resolution microcalorimeter

Cited by 5 publications

References 25 publications

Line Ratios for Solar Wind Charge Exchange with Comets

Line Ratios for Solar Wind Charge Exchange with Comets

X-rays from solar system objects

EBIT charge-exchange measurements and astrophysical applications

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