Energy loss straggling of low-energy protons in carbon

Kalz, D.; Kreysch, G.; Müller‐Jahreis, U.

doi:10.1080/00337577808233178

Cited by 10 publications

(4 citation statements)

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“…TOF distributions can vary for individual ion species as the carbon foil effects (i.e., charge state modification, energy straggling, and angular scattering) depend on atomic species (e.g., Allegrini, Wimmer‐Schweingruber, Wurz, & Bochsler, ; Allegrini, McComas, et al, ; Allegrini, Ebert, Fuselier, et al, ; Allegrini, Ebert, Nicolaou, & Grubs, ; Allegrini, Ebert, & Funsten, ; Allegrini, Coulter, et al, ; Bürgi, Oetliker, Bochsler, Geiss, & Coplan, ; Ebert et al, ; Funsten, McComas, & Barraclough, ; Gonin, Kallenbach, & Bochsler, ; Gonin, Kallenbach, Bochsler, & Bürgi, ; Kallenbach, Gonin, Buĺrgi, & Bochsler, ; Kallenbach, Gonin, Bochsler, & Bürgi, ; Kalz, Kreysch, & Müller‐Jahreis, ; McComas et al, ; Wuest, ; Ziegler, Ziegler, & Biersack, ).…”

Section: Methodsmentioning

confidence: 99%

“…( Wimmer-Schweingruber, Wurz, & Bochsler, 2003;Allegrini, McComas, et al, 2006;Allegrini, Ebert, Fuselier, et al, 2014;Allegrini, Ebert, Nicolaou, & Grubs, 2015;Allegrini, Ebert, & Funsten, 2016;Allegrini, Coulter, et al, 2016;Bürgi, Oetliker, Bochsler, Geiss, & Coplan, 1990;Ebert et al, 2014;Funsten, McComas, & Barraclough, 1993;Gonin, Kallenbach, & Bochsler, 1994;Kallenbach, Gonin, Buĺrgi, & Bochsler, 1993;Kalz, Kreysch, & Müller-Jahreis, 1978;McComas et al, 2004;Wuest, 1998;Ziegler, Ziegler, & Biersack, 2010 Kim et al (2019) are multiplied to the generated E/Q distributions (from equation ( 3)) and provide a modeled E/Q-TOF spectra. Ion parameters are derived by minimizing a chi-squared 2 value defined as…”

Section: Methodsmentioning

confidence: 99%

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Survey of Ion Properties in Jupiter's Plasma Sheet: Juno JADE‐I Observations

et al. 2020

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This study presents a survey of ion flow speed, density, temperature, and composition observed by the Jovian Auroral Distributions Experiment Ion (JADE-I) sensor on Juno from 10-40 R J in the dawn to midnight sector of Jupiter's magnetosphere. The survey covers Juno orbits 5-22, and the observations are separated by equatorial (|z mag [R J ]| ≤ 1.5) and off-equator (|z mag [R J ]| > 1.5) regions. Plasma parameters for H + , O + , O 2+ , O 3+ , Na + , S + , S 2+ , and S 3+ are derived by forward modeling JADE-I's energy-per-charge versus time-of-flight spectra using omnidirectional averaged convected kappa distributions and modeled instrument responses. O + and S 2+ are resolved via a ray-tracing simulation based on carbon-foil-effects. The ion flow speed increases with radial distance and is comparable to rigid corotation speed out to ∼20 R J . Ion number densities decrease with radial distance, the primary species being H + , O + , and S 2+ . The relative contribution of H + and S 2+ increases and decreases, respectively, in the off-equator regions, supporting the interpretation that the latitudinal distribution of ions is mass dependent. The O + to S 2+ and O n+ to S n+ number density ratios are variable, the 5 R J bin averages for O + to S 2+ ranging from ∼0.75-1.5 (equator) and ∼1.1-1.8 (off-equator) and O n+ to S n+ from ∼0.6-0.9 (equator) and ∼0.8-1.1 (off-equator). Both proton and heavy ion temperatures show order of magnitude increases between 10 and 20 R J and range from ∼100 eV to 10 keV and 1 keV to a few tens of keV, respectively. Plain Language Summary The Jovian Auroral Distributions Experiment (JADE) on Juno hascontinuously investigated the plasma environment in Jupiter's magnetosphere since its arrival in August 2016. The polar-orbiting spacecraft enables JADE to explore both equatorial and off-equator regions of Jupiter's plasma sheet. In this study, we present plasma sheet ion characteristics such as ion composition, flow speed, and temperatures for H + , O + , O 2+ , O 3+ , Na + , S + , S 2+ , and S 3+ that are originating from the innermost Galilean satellite Io. A spatial dependence of ion characteristics is discussed and compared to previous observations. While the density profiles agree well with the Voyager-based studies, temperatures found in this study show at least an order of magnitude higher values. A new addition to this paper is that the latitudinal distribution of ions shows trend in the mass. Relative composition of protons increases compared to the heavier ions in the off-equator regions. These observations provide insights on how the ions are distributed throughout Jupiter's magnetosphere and improve our current understanding on ion dynamics in the plasma sheet. Key Points:• Ion flow speed, number density, temperature, and composition in Jupiter's plasma sheet show radial and/or latitudinal trends • H + , O + , and S 2+ are the primary ions, the contribution of H + and S 2+ increasing and decreasing, respectively, in the off-equator region • The O + to S 2+ density ratio is vari...

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Section: Methodsmentioning

confidence: 99%

Section: Methodsmentioning

confidence: 99%

Survey of Ion Properties in Jupiter's Plasma Sheet: Juno JADE‐I Observations

et al. 2020

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“…Ions also lose energy while passing through the foil. Typically, the residual energy (i.e., exit energy of the ion after the carbon foil) of the transmitted ions have dispersion in their distribution due to the energy straggling process (Kalz et al, 1978). Like other carbon foil effects, energy loss varies for individual ions and depends on the physical parameter of the foil (e.g., Allegrini et al, 2006Allegrini et al, , 2015.…”

Section: A1 Modelmentioning

confidence: 99%

Method to Derive Ion Properties From Juno JADE Including Abundance Estimates for O⁺ and S²⁺

et al. 2020

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The Jovian Auroral Distributions Experiment Ion sensor (JADE‐I) on Juno is a plasma instrument that measures the energy‐per‐charge (E/Q) distribution of 0.01 to 46.2 keV/q ions over a mass‐per‐charge (M/Q) range of 1– 64 amu/q. However, distinguishing O+ and S2+ from JADE‐I's measurements is a challenging task due to similarities in their M/Q (∼16 amu/q). Because of this, O+ and S2+ have not been fully resolved in the in situ measurements made by plasma instruments at Jupiter (e.g., Voyager PLS and Galileo PLS) and their relative ratios has been studied using physical chemistry models and ultraviolet remote observations. To resolve this ambiguity, a ray tracing simulation combined with carbon foil effects is developed and used to obtain instrument response functions for H+, O+, O2+, O3+, Na+, S+, S2+, and S3+. The simulation results indicate that JADE‐I can resolve the M/Q ambiguity between O+ and S2+ due to a significant difference in their charge state modification process and a presence of a large electric potential difference (∼8 kV) between its carbon foils and MCPs. A forward model based on instrument response functions and convected kappa distributions is then used to obtain ion properties at the equatorial plasma sheet (∼36 RJ) in the predawn sector of magnetosphere. The number density ratio between O+ and S2+ for the selected plasma sheet crossings ranges from 0.2 to 0.7 (0.37 ± 0.12) and the number density ratio between total oxygen ions to total sulfur ions ranges from 0.2 to 0.6 (0.41 ± 0.09).

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“…The total energy loss straggling can be written as: Where, Ω 0 is the "intrinsic" energy loss straggling due to the statistics of collision as shown in equation (2), Ω r is the surface roughness contribution which can be expressed through a simple equation (see Ref. [3]). This relation for the straggling is given by: Ω 2 r = ρ 2 ∆E 2 and can be derived from a roughness analysis of a film with only two steps.…”

Section: Energy Loss Stragglingmentioning

confidence: 99%

Surface roughness of thin gold films and its effects on the proton energy loss straggling

Celedón¹,

Flores²,

Häberle³

et al. 2006

Braz. J. Phys.

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We present a description of the effect of the surface roughness on the energy straggling associated to the energy loss distributions of protons transmitted through a self supported metallic thin foil. For this purpose we prepared a polycrystalline gold thin films using the standard sputtering method with different deposition rates. The statistics of the surface height distribution induced in these thin films were determined using Atomic Force Microscopy. The measured surface roughness allowed us to quantify the ion energy loss straggling in these samples for different deposition parameters and as a function of the incident ion energy.

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Energy loss straggling of low-energy protons in carbon

Cited by 10 publications

References 1 publication

Survey of Ion Properties in Jupiter's Plasma Sheet: Juno JADE‐I Observations

Survey of Ion Properties in Jupiter's Plasma Sheet: Juno JADE‐I Observations

Method to Derive Ion Properties From Juno JADE Including Abundance Estimates for O⁺ and S²⁺

Surface roughness of thin gold films and its effects on the proton energy loss straggling

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Energy loss straggling of low-energy protons in carbon

Cited by 10 publications

References 1 publication

Survey of Ion Properties in Jupiter's Plasma Sheet: Juno JADE‐I Observations

Survey of Ion Properties in Jupiter's Plasma Sheet: Juno JADE‐I Observations

Method to Derive Ion Properties From Juno JADE Including Abundance Estimates for O+ and S2+

Surface roughness of thin gold films and its effects on the proton energy loss straggling

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Method to Derive Ion Properties From Juno JADE Including Abundance Estimates for O⁺ and S²⁺