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Auer, I.P.; Ditzler, W. R.; Hill, D.; Spinka, H.; Toshioka, K.; Underwood, D. G.; Wagner, R. G.; Yokosawa, A.; Hoffman, E. W.; Jarmer, J.J.; Burleson, G. R.; Cottingame, W. B.; Greene, S. J.; Stuart, S.

doi:10.1103/physrevd.29.2435

Cited by 31 publications

(12 citation statements)

References 157 publications

(1 reference statement)

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“…This procedure yields similar results to a complete linearization method, but has a much shorter computing time (Saumon et al 1994, hereafter SBLHB). Additional economy of execution time is obtained from formulating the radiative transfer in terms of moment equations, with closure using variable Eddington factors (Auer & Mihalas 1970).…”

Section: Methodsmentioning

confidence: 99%

Hydrogen-model atmospheres for white dwarf stars

Rohrmann

2001

Monthly Notices of the Royal Astronomical Society

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We present a detailed calculation of model atmospheres for DA white dwarfs. Our atmosphere code solves the atmosphere structure in local thermodynamic equilibrium with a standard partial linearization technique, which takes into account the energy transfer by radiation and convection. This code incorporates recent improved and extended data base of collision‐induced absorption by molecular hydrogen. We analyse the thermodynamic structure and emergent flux of atmospheres in the range 2500Teff60 000 K and 6.5log g9.0. Bolometric correction and colour indices are provided for a subsample of the model grid. Comparison of the colours is made with published observational material and results of other recent model calculations. Motivated by the increasing interest in helium‐core white dwarfs, we analyse the photometric characteristics of these stars during their cooling, using evolutionary models recently available. Effective temperatures, surface gravities, masses and ages have been determined for some helium‐core white dwarf candidates, and their possible binary nature is briefly discussed.

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Section: Methodsmentioning

confidence: 99%

Hydrogen-model atmospheres for white dwarf stars

Rohrmann

2001

Monthly Notices of the Royal Astronomical Society

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“…For p lab ≤ 1 GeV/c, σ tot can be as small as 25 mb or so and ∆σ L can reach the value −30 mb, so by using Eq. (4.7) one gets |∆σ T | ≤ 10 mb, with some errors, an interesting limit which is, indeed, satisfied by the data [141,142]. …”

Section: (44)mentioning

confidence: 80%

Spin observables and spin structure functions: Inequalities and dynamics

et al. 2009

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Model-independent identities and inequalities which relate the various spin observables of collisions in nuclear and particle physics are reviewed in a unified formalism. Their physical interpretation and their implications for dynamical models are also discussed. These constraints between observables can be obtained in several ways: from the explicit expression of the observables in terms of a set of helicity or transversity amplitudes, a non-trivial algebraic exercise which can be preceded by numerical simulation with randomly chosen amplitudes, from anticommutation relations, or from the requirement that any polarisation vector is less than unity. The most powerful tool is the positivity of the density matrices describing the spins in the initial or final state of the reaction or its crossed channels. The inequalities resulting from positivity need to be projected to single out correlations between two or three observables. The quantum aspects of the information carried by spins, in particular entanglement, are considered when deriving and discussing the constraints Several examples are given, with a comparison with experimental data in some cases. For the exclusive reactions, the cases of the strangeness-exchange proton-antiproton scattering and the photoproduction of pseudoscalar mesons are treated in some detail: all triples of observables are constrained, and new results are presented for the allowed domains. The positivity constraints for total cross-sections and for the simplest observables of single-particle inclusive reactions are reviewed. They also apply to spin-dependent structure functions and parton distributions, both integrated or transverse-momentum dependent. The corresponding inequalities are shown to be preserved by the evolution equations of quantum chromodynamics.Inequalities on spin observables 3

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“…This [2] ; Q ZGS-ANL, reference 78/L-52/ in [2] ; GJ ZGS-ANL, reference 77/M-97/ in [2] ; 0 Satume I, reference 67/C-26/ in [2] ; V LAMPF, reference 80/M-111/ in [2] ; * LAMPF, reference [43] ; + Gatchina, reference [36] ; 0 Gatchina, reference [37] ; 0 Gatchina, reference [38]; . Saturne II, references [32,45] ; Symbols for Aookk: 0 LAMPF, reference [20] ; fl3 ZGS-ANL, reference [69] and reference 78/A-165/ in [2] (numerical values) ; Saturne II, references [47,48].…”

Section: Formalismmentioning

confidence: 99%

“…[1] ; -·-· reference [3] ; --------AOL(el), this PSA and reference [1] ; N SIN, reference [68] ; 9 Saturne II, reference [21] ; D TRIUMF, reference [67] ; 0 LAMPF, reference [20] ; V ZGS-ANL, reference 78/A-164/ in [2].…”

Section: Formalismmentioning

confidence: 99%