Plasma environment effects on K lines of astrophysical interest

Deprince, J.; Bautista, M. A.; Fritzsche, S.; García, Javier A.; Kallman, Timothy R.; Mendoza, C.; Palmeri, P.; Quinet, Pascal

doi:10.1051/0004-6361/201935444

Cited by 16 publications

(11 citation statements)

References 59 publications

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“…However, atomic data that take the density effect into account are extremely lacking for dense plasmas under solar-interior conditions. Very recently, Deprince et al have investigated plasma-environment effects on the K lines of oxygen (Deprince et al 2019a) and iron (Deprince et al 2019b) ions in accretion disks around black holes. Magnetohydrodynamic simulations show that the electron temperatures and densities span the ranges of 10 5 -10 7 K and 10 18 -10 22 cm −3 , respectively (Schnittman et al 2013).…”

Section: Introductionmentioning

confidence: 99%

Screening potential and continuum lowering in a dense plasma under solar-interior conditions

Zeng

Cheng

et al. 2020

A&A

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An accurate description of the screening potential induced by a hot, dense plasma is a fundamental problem in atomic physics and plasma physics, and it plays a pivotal role in the investigation of microscopic atomic processes and the determination of macroscopic physical properties, such as opacities and equations of state as well as nuclear fusion cross sections. Recent experimental studies show that currently available analytical models of plasma screening have difficulty in accurately describing the ionization-potential depression, which is directly determined by the screening potential. Here, we propose a consistent approach to determine the screening potential in dense plasmas under solar-interior conditions from the free-electron micro-space distribution. It is assumed that the screening potential for an ion embedded in a dense plasma is predominately determined by the free electrons in the plasma. The free-electron density is obtained by solving the ionization-equilibrium equation for an average-atom model to obtain the average degree of ionization of the plasma. The proposed model was validated by comparing the theoretically predicted ionization-potential depression of a solid-density Si plasma with recent experiments. Our approach was applied to investigate the screening potential and ionization-potential depression of Si plasmas under solar-interior conditions over a temperature range of 150–500 eV and an electron-density range of 5.88 × 1022–3.25 × 1024 cm−3. It can be easily incorporated into atomic-structure codes and used to investigate basic atomic processes, such as photoionization, electron-ion collisional excitation and ionization, and Auger decay, in a dense plasma.

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Section: Introductionmentioning

confidence: 99%

Screening potential and continuum lowering in a dense plasma under solar-interior conditions

Zeng

Cheng

et al. 2020

A&A

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“…We have recently introduced high-density (n e > 10 18 cm −3 ) effects in the XSTAR database, which come into play in the reflection spectra of the inner region of the accretion disks around compact objects (e.g., black-hole candidates and neutron stars): continuum lowering [40][41][42][43][44][45]; dielectronic recombination suppression [48,49]; collisional ionization; three-body recombination; and stimulated emission. Since the Fe abundance is a key measure of line reprocessing in reflection models [50], we are now in a good position to test if the neglect of such high-density effects is responsible for the anomalously high abundances recurrently derived [51].…”

Section: Introductionmentioning

confidence: 99%

The XSTAR Atomic Database

Mendoza¹,

Bautista²,

Deprince³

et al. 2021

Atoms

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We describe the atomic database of the xstar spectral modeling code, summarizing the systematic upgrades carried out in the past twenty years to enable the modeling of K-lines from chemical elements with atomic number Z≤30 and recent extensions to handle high-density plasmas. Such plasma environments are found, for instance, in the inner region of accretion disks round compact objects (neutron stars and black holes), which emit rich information about the system’s physical properties. Our intention is to offer a reliable modeling tool to take advantage of the outstanding spectral capabilities of the new generation of X-ray space telescopes (e.g., xrism and athena) to be launched in the coming years. Data curatorial aspects are discussed and an updated list of reference sources is compiled to improve the database provenance metadata. Two xstar spin-offs—the ISMabs absorption model and the uaDB database—are also described.

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“…The importance of high-density effects are now being recognized for the radiative properties of accretion disks surrounding black holes as well as for the radiation transport and opacity of stellar interiors [7,8]. Field-induced spectral line broadening has also been recognized as an important diagnostic tool for inferring the density of laboratory plasmas, e.g., those produced in inertial confinement fusion experiments, and this effect has been observed in a variety laboratory plasmas [9][10][11].…”

Section: Introductionmentioning

confidence: 99%

Stark shift and width of x-ray lines from highly charged ions in dense plasmas

Beiersdörfer

2020

Phys. Rev. A

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We implement several plasma screening potentials to calculate the level energy shifts of highly charged ions in warm dense plasmas. The Stark widths of transitions are treated with an empirical interpolation scheme combining the impact approximation and the quasi-contiguous approximation. The resulting shift-width relationship is compared with recent experimental measurements of the K β transition of He-like Cl from the ORION laser facility.

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Plasma environment effects on K lines of astrophysical interest

Cited by 16 publications

References 59 publications

Screening potential and continuum lowering in a dense plasma under solar-interior conditions

Screening potential and continuum lowering in a dense plasma under solar-interior conditions

The XSTAR Atomic Database

Stark shift and width of x-ray lines from highly charged ions in dense plasmas

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