X-Ray and Euv Spectroscopy of Various Astrophysical and Laboratory Plasmas: Collisional, Photoionization and Charge-Exchange Plasmas

Liang, G. Y.; Li, F.; Wang, F. L.; Wu, Yong; Zhong, Jiayong; Zhao, Gang

doi:10.1088/0004-637x/783/2/124

Cited by 16 publications

(13 citation statements)

References 92 publications

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“… can be obtained. The atomic data of level energies and radiative decays have been reported by Liang et al (2014Liang et al ( , 2021. Here the chargeexchange cross sections are from the Kronos v3.1 database 9 that is implemented by Stancil research group in a series of studies (Cumbee et al 2014(Cumbee et al , 2018Mullen et al 2016Mullen et al , 2017 that use multiple methods, including multichannel Landau-Zener (MCLZ), atomic-orbital close-coupling (AOCC), molecular-orbital close-coupling (MOCC), and classical trajectory Monte Carlo methods.…”

Section: Emission Modelmentioning

confidence: 99%

X-Ray Morphology Due to Charge-exchange Emissions Used to Study the Global Structure around Mars

Liang

Sun

et al. 2023

ApJ

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Soft X-ray emissions induced by solar wind ions that collide with neutral material in the solar system have been detected around planets, and were proposed as a remote probe for solar wind interaction with the Martian exosphere. A multi-fluid three-dimensional magnetohydrodynamic model is adopted to derive the global distributions of solar wind particles. Spherically symmetric exospheric H, H2, He, O, and CO2 density profiles and a sophisticated hybrid model that includes charge-exchange and proton–neutral excitation processes are used to study the low triplet line ratio G = i + f r (0.77 ± 0.58) of O vii and the total X-ray luminosity around Mars. We further calculate the emission factor α-value with different neutrals over wide ion-abundance and velocity ranges. Our results are in good agreement with those of previous reports. The evolution of the charge stage of solar wind ions shows that sequential recombination due to charge-exchange can be negligible in the interaction region. This only appears below an altitude of 400 km. The anonymous low disk G-ratio can be easily explained by the collisional quenching effect at neutral densities higher than 1011 cm−3. However, the quenching contribution is small in Mars’ exosphere and only appears below 400 km. Charge-exchange with H2 and N2 is still the most likely reason for this low G-ratio. X-ray emissivity maps in collisions with different neutrals differ from each other. A clear bow shock arising from the collision with all the neutrals is in accordance with previous reports. The resulting total X-ray luminosity of 6.55 MW shows better agreement with the XMM-Newton observation of 12.8 ± 1.4 MW than that of previous predictions.

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Section: Emission Modelmentioning

confidence: 99%

X-Ray Morphology Due to Charge-exchange Emissions Used to Study the Global Structure around Mars

Liang

Sun

et al. 2023

ApJ

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“…Once the SMILE mission targeting Earth's magnetosphere is launched, we will understand more clearly the changes in SWCX spectra due to incoming solar wind ions. Note this method is limited by a lack of accurate cross sections and we look forward to further collaboration with atomic physicists to improve the model (Liang et al 2014(Liang et al , 2021.…”

Section: Spectral Diagnosis Of Swcx Emissionsmentioning

confidence: 99%

Solar Wind Charge Exchange Soft X-Ray Emissions in the Magnetosphere during an Interplanetary Coronal Mass Ejection Compared to Its Driven Sheath

Zhang¹,

Sun²,

Wang

et al. 2022

ApJL

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Soft X-ray emissions from solar wind charge exchange (SWCX) are applied in a recently developed approach to study the magnetosphere using panoramic soft X-ray imaging. This study represents the first attempt to distinguish magnetospheric SWCX emissions observed by XMM-Newton during the impact of an interplanetary coronal mass ejection (ICME) and its driven sheath on Earth. In addition, data from the Advanced Composition Explorer (ACE) were available during this same observational period, which is rare in previous studies. Results showed that SWCX emissions peaked during the ICME at approximately 2.3 times the mean of the observation period, although the solar wind flux decreased to a much lower level. A comparison of spectral results with ion data probed by ACE revealed that high ionization states in the ICME effectively enhanced line emission intensity for heavy ions (e.g., Ne, Mg, and Al). Thus, despite a low proton flux, elevated high-valence ion abundance in the ICME favors magnetospheric soft X-ray observations. Furthermore, the fitted X-ray flux of ion line emissions was consistent with elemental abundance ratios determined in situ by ACE, particularly for C5+, C6+, Ne9+, Mg11+, and Mg12+. This confirms the viability of spectral diagnosis of SWCX emissions as a new method for remotely analyzing high-state ion distributions in solar wind. A time-correlated or two-stage efficiency factor is further suggested to better estimate X-ray intensity during an ICME impact, which was ∼1.7 times higher in the ICME than in the sheath.

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“…Several similar codes, which are being used for analysis of astrophysical spectra, have already been published in the literature. Examples are GALAXY (Rose 1998, Foord et al 2004, Foord et al 2006, Rose et al 2004), NIMP (Djaoui & Rose 1992, Rose et al 2004), FLYCHK (Chung et al 2003), CLOUDY (Ferland et al 1998), XSTAR (Kallman et al 1996, Kallman et al 2004, Boroson et al 2003, PhiCRE (Salzmann et al 2011 and SASAL (Liang et al 2014). Some of these codes are used to interpret laboratory experiments (GALAXY, FLYCHK, NIMP and PhiCRE), while others are used in analysis of astrophysical spectra (CLOUDY and XSTAR), while RCF is designed to be applicable to both of the conditions above.…”

Section: Reactionmentioning

confidence: 99%

“…A distribution of iron charge states was deduced from the absorption spectrum. A number of papers (Foord et al 2004, Foord et al 2006, Han et al 2013, Liang et al 2014) tried reproducing the measured charge state distribution using different models and computer codes. All these works assumed a steady state photoionized plasma, which is also adopted by RCF.…”

Section: Simulation Of Sandia Photoionization Experimentsmentioning

confidence: 99%

Modeling non-local thermodynamic equilibrium plasma using the Flexible Atomic Code data

Han

Wang

Salzmann

et al. 2015

Publications of the Astronomical Society of Japan

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We present a new code, RCF("Radiative-Collisional code based on FAC"), which is used to simulate steady-state plasmas under non local thermodynamic equilibrium condition, especially photoinization dominated plasmas. RCF takes almost all of the radiative and collisional atomic processes into rate equation to interpret the plasmas systematically. The Flexible Atomic Code (FAC) supplies all the atomic data RCF needed, which insures calculating completeness and consistency of atomic data. With four input parameters relating to the radiation source and target plasma, RCF calculates the population of levels and charge states, as well as potentially emission spectrum. In preliminary application, RCF successfully reproduces the results of a photoionization experiment with reliable atomic data. The effects of the most important atomic processes on the charge state distribution are also discussed.

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X-Ray and Euv Spectroscopy of Various Astrophysical and Laboratory Plasmas: Collisional, Photoionization and Charge-Exchange Plasmas

Cited by 16 publications

References 92 publications

X-Ray Morphology Due to Charge-exchange Emissions Used to Study the Global Structure around Mars

X-Ray Morphology Due to Charge-exchange Emissions Used to Study the Global Structure around Mars

Solar Wind Charge Exchange Soft X-Ray Emissions in the Magnetosphere during an Interplanetary Coronal Mass Ejection Compared to Its Driven Sheath

Modeling non-local thermodynamic equilibrium plasma using the Flexible Atomic Code data

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