Charge transfer in<mml:math xmlns:mml="http://www.w3.org/1998/Math/MathML" display="inline"><mml:mrow><mml:msup><mml:mrow><mml:mi mathvariant="normal">H</mml:mi></mml:mrow><mml:mrow><mml:mo>+</mml:mo></mml:mrow></mml:msup></mml:mrow></mml:math>-H and<mml:math xmlns:mml="http://www.w3.org/1998/Math/MathML" display="inline"><mml:mrow><mml:msup><mml:mrow><mml:mi mathvariant="normal">H</mml:mi></mml:mrow><mml:mrow><mml:mo>+</mml:mo></mml:mrow></mml:msup></mml:mrow></mml:math>-D collisions within the energy ran

Newman, J. H.; Cogan, J.; Ziegler, D. L.; Nitz, D. E.; Rundel, R. D.; Smith, K. A.; Stebbings, R. F.

doi:10.1103/physreva.25.2976

Cited by 84 publications

(35 citation statements)

References 15 publications

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“…Figure 1 shows the integral charge-transfer cross section over a projectile energy range from 2 eV to 2 keV. The calculated cross sections show good agreement with experimental values [59,60] over the entire range of projectile energies. The calculations were done in a basis of TAO's written as linear combinations of Gaussians, including five orbitals (the ls, 2s, and 2p orbitals) on each center.…”

Section: Comyarison Of Asymptotic Values With Other Worksupporting

confidence: 52%

Time-dependent many-electron approach to slow ion-atom collisions: The coupling of electronic and nuclear motions

Micha

Runge

1994

Phys. Rev. A

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We describe the coupling of electronic and nuclear motions in slow atomic collisions using a combination of the eikonal and time-dependent Hartree-Fock (TDHF) approximations. Starting with an eikonal representation of the total wave function, a wave function is constructed from classical trajectories in a way suitable for describing atomic co11isions with velocities down to a fraction of an atomic unit. The TDHF formulation is developed in terms of its density operator. The differential equations coupling the density operator to the nuclear motions have been solved with a procedure developed to account for the coupling of fast (electronic) and slow (nuclear) degrees of freedom. This is based on a local-interaction picture and on a temporal linearization of the equations, allowing for the integration of the electronic density over large time intervals. Density-matrix equations are derived in a basis of traveling atomic orbitals, and numerical results are presented for H++H and He ++H. Good agreement is found with experimental results for H++H, comparing integral electron transfer cross sections from 2 to 2000 eV. In addition, an analysis of the time dependence of atomic orbital populations provides insight on electronic rearrangement during collisions and shows that even very small contributions from the driving forces of the nuclei on the electrons have a cumulative effect on the density operator that can substantially change final populations.

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Section: Comyarison Of Asymptotic Values With Other Worksupporting

confidence: 52%

Time-dependent many-electron approach to slow ion-atom collisions: The coupling of electronic and nuclear motions

Micha

Runge

1994

Phys. Rev. A

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“…The penetration thickness depends on the process that could drag the atoms: essentially by charge-exchange and by ionization via the interaction with the protons confined in the external layer. The cross sections of such processes are strongly dependent on velocity (McClure 1966;Newman et al 1982;Peek 1966;Ptak & Stoner 1973), and variations of the surface density in the external layer give rise to changes of the thickness moving away from the stagnation point. In our previous paper we have evaluated the thickness using the two thin layer model limited to a region near the axis.…”

Section: Penetration Thickness For Neutral Hydrogenmentioning

confidence: 99%

Pulsar bow-shock nebulae

Bucciantini

2002

A&A

129

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Abstract. We present hydrodynamical simulations, using a 2-D two component model (ambient medium and pulsar wind have different specific heat ratios), of bow shocks in a representative regime for pulsar wind driven bow-shock nebulae. We also investigate the behaviour of a passive toroidal magnetic field wound around the pulsar velocity direction. Moreover we estimate the opacity of the bow-shock to penetration of ISM neutral hydrogen: this quantity affects observable properties of the nebula, like its size, shape, velocity and surface brightness distribution. Finally we compare these numerical results with those from an analytical model. The development of more realistic models is needed in order to tune the criteria for searches of new such objects, as well as to interpret data on the known objects.

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“…The cross sections used in this paper come from Ptak & Stoner (1973) for ionization and from McClure (1966), Newman (1982) and Peek (1966) for charge-exchange.…”

Section: Microphysical Processesmentioning

confidence: 99%

Pulsar bow-shock nebulae

Bucciantini

Bandiera

2001

A&A

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Abstract. Pulsar bow-shock nebulae originate from the interaction of the ambient medium with the wind of a moving pulsar. The properties of these nebulae depend on both the physical conditions in the ambient medium and the characteristics of the pulsar wind, and may thus represent a powerful diagnostic tool. The main limits to this study are, on the observational side, the very limited sample of pulsar bow-shock nebulae known so far and, on the theoretical one, a still limited understanding of the physical conditions in these nebulae: in particular, classical bow-shock models are not appropriate to describe these objects. In this paper we outline the most likely physical regimes for nebulae associated with typical pulsars, and discuss why classical models cannot be applied to these objects. We also discuss how microphysical processes may affect both the dynamics of the flow and the properties of the emission (mostly in Balmer lines). We finally put forward a criterion to select among the known pulsars those with the highest probability of having a detectable bow-shock nebula.

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Charge transfer inH+-H andH+-D collisions within the energy ran

Cited by 84 publications

References 15 publications

Time-dependent many-electron approach to slow ion-atom collisions: The coupling of electronic and nuclear motions

Time-dependent many-electron approach to slow ion-atom collisions: The coupling of electronic and nuclear motions

Pulsar bow-shock nebulae

Pulsar bow-shock nebulae

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