By P. Schmelcher, W. Schweizer
This e-book includes contributions to the 172. WE-Heraeus-Seminar “Atoms and Molecules in powerful exterior Fields,” which happened April 7–11 1997 on the Phys- zentrum undesirable Honnef (Germany). The designation “strong fields” applies to exterior static magnetic, and/or electrical fields which are sufficiently extreme to reason changes within the atomic or molecular str- ture and dynamics. the categorical subject matters taken care of are the habit and homes of atoms in powerful static fields, the basic points and digital constitution of molecules in robust magnetic fields, the dynamics and features of chaos in hugely excited R- berg atoms in exterior fields, topic within the surroundings of astrophysical gadgets (white dwarfs, neutron stars), and quantum nanostructures in powerful magnetic fields. it really is seen that the elaboration of the corresponding homes in those regimes reasons the best problems, and is incomplete even at the present time. Present-day know-how has made it attainable for plenty of learn teams to review the habit of subject in robust exterior fields, either experimentally and theore- cally, the place the word “experimentally” contains the astronomical observations. - derstanding those platforms calls for the improvement of recent theories and strong computational innovations. Interdisciplinary collaborations can be precious and priceless in constructing extra effective how you can comprehend those very important platforms. consequently the belief was once to collect humans from diversified fields like atomic and molecular physics, theoretical chemistry, astrophysics and all these colleagues attracted to features of few-body structures in exterior fields.
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Extra info for Atoms and Molecules in Strong External Fields
The integration should be performed with allowance for the gravitational bending of photon trajectories (e. , 1995). , 1995; Zavlin and Pavlov, 1997b). An important result of the atmosphere fits is that they yield effective temperatures considerably lower than those obtained from the blackbody fits, usually below the temperatures predicted by the standard NS cooling models (see Introduction). However, in many cases both the blackbody and atmosphere models give statistically acceptable fits because of the narrowness of the X-ray energy range and poor spectral resolution of current X-ray detectors.
The corresponding wavelengths are 4820, 7730 and 2250 Å. and ACKNOWLEDGEMENTS This work was supported by the Deutsche Forschungsgemeinschaft (DFG) and the Foundation for Research Development(FRD) of South Africa. , Pekeris, C. L. and Schiff, B. 1971 Phys. Rev. , 1993, Finite element calculations for S states of helium, Phys. Rev. , Wunner, G. , and Geyer. , 1990, On the spectrum and field strength of the magnetic white dwarf GD229, Astrophys. J. 350:758 Tang. J. , 1992, Dipole density function and evaluation of the oscillator strengths of He, Phys.
12 white dwarf radii along and perpendicular to the magnetic axis, respectively, and a dipole field strength of 800 T. The inclination of the rotation axis is 20° and the colatitude 50°. It is obvious especially from the polarization spectrum that there are clear deviations between the radiative transfer model and observation. They might be caused in the first place by the Holtsmark distribution, not valid for magnetic fields, and secondly by the approximation for the bound-free opacities. In Fig.