Interaction of atoms, molecules, and ions with constant electric and magnetic fields

Johnson, Bruce R.; Hirschfelder, Joseph O.; Yang, Kuo‐Ho

doi:10.1103/revmodphys.55.109

Cited by 224 publications

(180 citation statements)

References 89 publications

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“…It has also been found that a velocity-dependent, Coriolis-like force in Newton's equations causes the ionization of the electron to exhibit chaotic scattering [MW92,UF95,JFU99]. All these phenomena, as well as renewed interest in the motional Stark effect [JHY83,F94], make the crossed-fields problem an experimental accessible paradigm for a wide variety of outstanding issues in atomic and molecular physics, solid-state physics [DS92,Schm93], nuclear physics [BM75], astrophysics [Ma89], and celestial mechanics [Mi82].…”

Section: Introductionmentioning

confidence: 99%

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Berglund

Uzer²

2001

Foundations of Physics

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Section: Introductionmentioning

confidence: 99%

Untitled

Berglund

Uzer²

2001

Foundations of Physics

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“…We recall the description of a charged particle in a uniform magnetic field (e.g., Johnson & Lippmann 1949;Landau & Lifshitz 1976;Johnson et al 1983). The Hamiltonian equals the kinetic energy operator…”

Section: Charged Particles In a Magnetic Fieldmentioning

confidence: 99%

Cyclotron harmonics in opacities of isolated neutron star atmospheres

Potekhin

2010

A&A

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Some X-ray dim isolated neutron stars (XDINS) and central compact objects in supernova remnants (CCO) contain absorption features in their thermal soft X-ray spectra. It has been hypothesized that this absorption may relate to periodic peaks in free-free absorption opacities, caused by either Landau quantization of electron motion in magnetic fields B < ∼ 10 11 G or analogous quantization of ion motion in magnetic fields B > 10 13 G. Here, I review the physics behind cyclotron quantum harmonics in free-free photoabsorption, discuss different approximations for their calculation, and explain why the ion cyclotron harmonics (beyond the fundamental) cannot be observed.

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“…The astrophysical simulations assume finite temperatures, hence thermal motion of particles. The theory of motion of a system of point charges in a constant magnetic field was reviewed by Johnson et al (1983). The canonical center-of-mass momentum P is not conserved in a magnetic field.…”

Section: Hydrogen Atom In a Strong Magnetic Fieldmentioning

confidence: 99%

Opacities and spectra of hydrogen atmospheres of moderately magnetized neutron stars

Potekhin

Chabrier

2014

A&A

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Context. There is observational evidence that central compact objects (CCOs) in supernova remnants have moderately strong magnetic fields B ∼ 10 11 G. Meanwhile, available models of partially ionized hydrogen atmospheres of neutron stars with strong magnetic fields are restricted to B 10 12 G. Extension of the applicability range of the photosphere models to lower field strengths is complicated by a stronger asymmetry of decentered atomic states and by the importance of excited bound states. Aims. We extend the equation of state and radiative opacities, as presented in previous papers for 10 12 G B 10 15 G, to weaker fields. Methods. We constructed analytical fitting formulae for binding energies, sizes, and oscillator strengths for different bound states of a hydrogen atom moving in moderately strong magnetic fields and calculate an extensive database for photoionization cross sections of such atoms. Using these atomic data, in the framework of the chemical picture of plasmas we solved the ionization equilibrium problem and calculated thermodynamic functions and basic opacities of partially ionized hydrogen plasmas at these field strengths. Then plasma polarizabilities were calculated from the Kramers-Kronig relation, and the radiative transfer equation for the coupled normal polarization modes was solved to obtain model spectra.Results. An equation of state and radiative opacities for a partially ionized hydrogen plasma are obtained at magnetic fields B, temperatures T , and densities ρ typical for atmospheres of CCOs and other isolated neutron stars with moderately strong magnetic fields. The first-and second-order thermodynamic functions, monochromatic radiative opacities, and Rosseland mean opacities are calculated and tabulated, considering partial ionization, for 3×10 10 G B 10 12 G, 10 5 K T 10 7 K, and a wide range of densities. Atmosphere models and spectra are calculated to verify the applicability of the results and to determine the range of magnetic fields and effective temperatures where the incomplete ionization of the hydrogen plasma is important.

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Interaction of atoms, molecules, and ions with constant electric and magnetic fields

Cited by 224 publications

References 89 publications

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Cyclotron harmonics in opacities of isolated neutron star atmospheres

Opacities and spectra of hydrogen atmospheres of moderately magnetized neutron stars

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