Electron radiative recombination with a hydrogen-like ion

Kotelnikov, I. A.; Milstein, A. I.

doi:10.1088/1402-4896/ab060a

Cited by 14 publications

(4 citation statements)

References 64 publications

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“…Matveyev et al [30] derived a mean rate coefficient [24]. Radiative recombination cross section of T + from [29] for comparison. Data provided for the frame of reference, where the ion is at rest.…”

Section: Recombination Of Electrons With Tritium Ionsmentioning

confidence: 99%

Monte Carlo simulations of the electron — gas interactions in the KATRIN experiment

Kellerer¹,

Spanier

2022

J. Inst.

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At the KATRIN experiment, the electron antineutrino mass is inferred from the shape of the β-decay spectrum of tritium. Important systematic effects in the Windowless Gaseous Tritium Source (WGTS) of the experiment include the energy loss by electron scattering, and the extended starting potential. In the WGTS, primary high-energy electrons from β-decay produce an extended secondary spectrum of electrons through various atomic and molecular processes including ionization, recombination, cluster formation and scattering. In addition to providing data essential to the simulation of energy loss processes, the electron spectrum also provides information important in the simulation of plasma processes. These simulations will then provide an insight on the starting potential. Here, a Monte Carlo approach is used to model the electron spectrum in the source for a given magnetic and electric field configuration. The spectrum is evaluated at different positions within the WGTS, which allows for a direct analysis of the spectrum close to the rear wall and detector end of the experiment. Alongside electrons, also ions are tracked by the simulation, resulting in a full description of the currents in the source.

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Section: Recombination Of Electrons With Tritium Ionsmentioning

confidence: 99%

Monte Carlo simulations of the electron — gas interactions in the KATRIN experiment

Kellerer¹,

Spanier

2022

J. Inst.

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“…Those data are fitted by the Chebyshev polynomials with twenty terms. For the hydrogen-like atoms, the fitting function is given by Kotelnikov & Milstein (2019).…”

Section: Physical Model Of Downstream Ionization Balance and Ion Inte...mentioning

confidence: 99%

X-ray Line Diagnostics of Ion Temperature at Cosmic-Ray Accelerating Collisionless Shocks

Shimoda,

Ohira,

Bamba

et al. 2022

Preprint

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A novel collisionless shock jump condition is suggested by modeling the entropy production at the shock transition region. We also calculate downstream developments of the atomic ionization balance and the ion temperature relaxation in supernova remnants (SNRs). The injection process and subsequent acceleration of cosmic-rays (CRs) in the SNR shocks are closely related to the formation process of the collisionless shocks. The formation of the shock is caused by wave-particle interactions. Since the wave-particle interactions result in energy exchanges between electromagnetic fields and charged particles, the randomization of particles associated with the shock transition may occur with the rate given by the scalar product of the electric field and current. We find that order-of-magnitude estimates of the randomization with reasonable strength of the electromagnetic fields in the SNR constrain the amount of the CR nuclei and ion temperatures. The constrained amount of the CR nuclei can be sufficient to explain the Galactic CRs. The ion temperature becomes significantly lower than the case of no CRs. To distinguish the case without CRs, we perform synthetic observations of atomic line emissions from the downstream region of the SNR RCW 86. Future observations by XRISM and Athena can distinguish whether the SNR shock accelerates the CRs or not from the ion temperatures.

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“…The energy of the photon, hν, ionizing a hydrogenic ion of charge z can be expressed in terms of ionization threshold energy of hydrogen, I H as hω = hν = hRcz 2 1…”

Section: Photoionization Of Hydrogenic Ionsmentioning

confidence: 99%

Photoionization and Electron-Ion Recombination of n = 1 to Very High n-Values of Hydrogenic Ions

Nahar

2021

Atoms

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Single electron hydrogen or hydrogenic ions have analytical forms to evaluate the atomic parameters for the inverse processes of photoionization and electron-ion recombination (H I + hν↔ H II + e) where H is hydrogen. Studies of these processes have continued until the present day (i) as the computations are restricted to lower principle quantum number n and (ii) to improve the accuracy. The analytical expressions have many terms and there are numerical instabilities arising from cancellations of terms. Strategies for fast convergence of contributions were developed but precise computations are still limited to lower n. This report gives a brief review of the earlier precise methodologies for hydrogen, and presents numerical tables of photoionization cross sections (σPI), and electron-ion recombination rate coefficients (αRC) obtained from recombination cross sections (σRC) for all n values going to a very high value of 800. σPI was obtained using the precise formalism of Burgess and Seaton, and Burgess. αRC was obtained through a finite integration that converge recombination exactly as implemented in the unified method of recombination of Nahar and Pradhan. Since the total electron-ion recombination includes all levels for n = 1 −∞, the total asymptotic contribution of n=801−∞, called the top-up, is obtained through a n−3 formula. A FORTRAN program “hpxrrc.f” is provided to compute photoionization cross sections, recombination cross sections and rate coefficients for any nl. The results on hydrogen atom can be used to obtain those for any hydrogenic ion of charge z through z-scaling relations provided in the theory section. The present results are of high precision and complete for astrophysical modelings.

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Electron radiative recombination with a hydrogen-like ion

Cited by 14 publications

References 64 publications

Monte Carlo simulations of the electron — gas interactions in the KATRIN experiment

Monte Carlo simulations of the electron — gas interactions in the KATRIN experiment

X-ray Line Diagnostics of Ion Temperature at Cosmic-Ray Accelerating Collisionless Shocks

Photoionization and Electron-Ion Recombination of n = 1 to Very High n-Values of Hydrogenic Ions

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