By Detlev Koester (auth.), P. Schmelcher, W. Schweizer (eds.)
This e-book includes contributions to the 172. WE-Heraeus-Seminar “Atoms and Molecules in robust exterior Fields,” which came about 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 severe to reason changes within the atomic or molecular str- ture and dynamics. the categorical issues handled are the habit and homes of atoms in robust static fields, the basic facets and digital constitution of molecules in robust magnetic fields, the dynamics and facets 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 robust magnetic fields. it's visible that the elaboration of the corresponding homes in those regimes motives the best problems, and is incomplete even this present day. Present-day expertise has made it attainable for lots of study teams to review the habit of topic in powerful exterior fields, either experimentally and theore- cally, the place the word “experimentally” contains the astronomical observations. - derstanding those structures calls for the advance of contemporary theories and strong computational ideas. Interdisciplinary collaborations might be worthy and priceless in constructing extra effective tips on how to comprehend those very important platforms. as a result the belief used to be to assemble humans from assorted fields like atomic and molecular physics, theoretical chemistry, astrophysics and all these colleagues attracted to facets of few-body structures in exterior fields.
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We also give those obtained by watanabe et al. (1992). It is seen that the agreement is fair to good except for which is due to the small energy difference involved. However the corresponding wavelength is very large and thus unimportant for astrophysical applications. e. for field strengths up to Tesla. In figures 1 to 3 we show the wavelengths obtained for a few selected transitions between singlet states with . It is seen that as function of the magnetic field strength, the wavelengths vary by approximately a factor of 2.
1996, On cooling of magnetized neutron stars, Astron. Astrophys. 309:171. Shibanov, Yu. , Zavlin, V. , Pavlov, G. , 1992, Model atmospheres of magnetic neutron stars: I. The fully ionized case, Astron. Astrophys. 266:313. Shibanov, Yu. , Pavlov, G. , Zavlin, V. , 1995, Anisotropic cooling and atmospheric radiation of neutron stars with strong magnetic field, Ann. NY Acad. , 759:291. Shibazaki, N . , and Lamb, F. , 1989, Neutron star evolution with internal heating, Astrophys. J. 346:808. 47 Taylor, J.