Publications (122)293.05 Total impact
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ABSTRACT: Although the fundamental physics behind radiation and matter flow is understood, many uncertainties remain in the exact behavior of macroscopic fluids in systems ranging from pure turbulence to coupled radiation hydrodynamics. Laboratory experiments play an important role in studying this physics to allow scientists to test their macroscopic models of these phenomena. However, because the fundamental physics is well understood, precision experiments are required to validate existing codes already tested by a suite of analytic, manufactured and convergence solutions. To conduct such highprecision experiments requires a detailed understanding of the experimental errors and the nature of their uncertainties on the observed diagnostics. In this paper, we study the uncertainties plaguing many radiationflow experiments, focusing on those using a hohlraum (dynamic or laserdriven) source and a foamdensity target. This study focuses on the effect these uncertainties have on the breakout time of the radiation front. We find that, even if the errors in the initial conditions and numerical methods are Gaussian, the errors in the breakout time are asymmetric, leading to a systematic bias in the observed data. We must understand these systematics to produce the highprecision experimental results needed to study this physics.  [Show abstract] [Hide abstract]
ABSTRACT: We present a new, publicly available, set of Los Alamos OPLIB opacity tables for the elements hydrogen through zinc. Our tables are computed using the Los Alamos ATOMIC opacity and plasma modeling code, and make use of atomic structure calculations that use finestructure detail for all the elements considered. Our equationofstate (EOS) model, known as ChemEOS, is based on the minimization of free energy in a chemical picture and appears to be a reasonable and robust approach to determining atomic state populations over a wide range of temperatures and densities. In this paper we discuss in detail the calculations that we have performed for the 30 elements considered, and present some comparisons of our monochromatic opacities with measurements and other opacity codes. We also use our new opacity tables in solar modeling calculations and compare and contrast such modeling with previous work. 
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ABSTRACT: Aims. Our goal is to test the newly developed OPLIB opacity tables from Los Alamos National Laboratory and check their influence on the pulsation properties of Btype stars. Methods. We calculated models using MESA and Dziembowski codes for stellar evolution and linear, nonadiabatic pulsations, respectively. We derived the instability domains of β Cephei and SPBtypes for different opacity tables OPLIB, OP, and OPAL. Results. The new OPLIB opacities have the highest Rosseland mean opacity coefficient near the socalled Zbump. Therefore, the OPLIB instability domains are wider than in the case of OP and OPAL data.  [Show abstract] [Hide abstract]
ABSTRACT: We have studied the excitation of Hlike and Helike uranium (U91+ and U90+) in relativistic collisions with gaseous targets by observing the subsequent xray emission. The experiment was conducted at the ESR storage ring of the GSI accelerator facility in Darmstadt, Germany. The measurements were performed with a newly developed multiphase target at different collision energies. This enabled us to explore the proton (nucleus) impact excitation as well as the electron impact excitation processes in the relativistic collisions. The large finestructure splitting in uranium allowed us to unambiguously resolve excitation to different Lshell levels. Moreover, information about the population of different magnetic sublevels has been obtained via an angular differential study of the decay photons associated with the subsequent deexcitation process. The experimental results are compared with calculations performed within the relativistic framework including excitation mechanisms due to both protons (nucleus) and electrons.  [Show abstract] [Hide abstract]
ABSTRACT: The Los Alamos suite of relativistic atomic physics codes is a robust, mature platform that has been used to model highly charged ions in a variety of ways. The suite includes capabilities for calculating data related to fundamental atomic structure, as well as the processes of photoexcitation, electronimpact excitation and ionization, photoionization and autoionization within a consistent framework. These data can be of a basic nature, such as cross sections and collision strengths, which are useful in making predictions that can be compared with experiments to test fundamental theories of highly charged ions, such as quantum electrodynamics. The suite can also be used to generate detailed models of energy levels and rate coefficients, and to apply them in the collisionalradiative modeling of plasmas over a wide range of conditions. Such modeling is useful, for example, in the interpretation of spectra generated by a variety of plasmas. In this work, we provide a brief overview of the capabilities within the Los Alamos relativistic suite along with some examples of its application to the modeling of highly charged ions.  [Show abstract] [Hide abstract]
ABSTRACT: We report on the use of the Los Alamos suite of relativistic atomic physics codes to generate radiative opacities for the modeling of astrophysically relevant plasmas under local thermodynamic equilibrium (LTE) conditions. The atomic structure calculations are carried out in finestructure detail, including full configuration interaction. Three example applications are considered: iron opacities at conditions relevant to the base of the solar convection zone, nickel opacities for the modeling of stellar envelopes, and samarium opacities for the modeling of light curves produced by neutron star mergers. In the first two examples, comparisons are made between opacities that are generated with the fully and semirelativistic capabilities in the Los Alamos suite of codes. As expected for these highly charged, ironpeak ions, the two methods produce reasonably similar results, providing confidence that the numerical methods have been correctly implemented. However, discrepancies greater than 10% are observed for nickel and investigated in detail. In the final application, the relativistic capability is used in a preliminary investigation of the complicated absorption spectrum associated with cold lanthanide elements. 
Article: An Equation of State for Partially Ionized Plasmas: The Coulomb Contribution to the Free Energy
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ABSTRACT: We have previously developed an equation of state (EOS) model called ChemEOS (Hakel and Kilcrease, Atomic Processes in Plasmas, Eds., J. Cohen et al., AIP, 2004) for a plasma of interacting ions, atoms and electrons. It is based on a chemical picture of the plasma and is derived from an expression for the Helmholtz free energy of the interacting species. All other equilibrium thermodynamic quantities are then obtained by minimizing this free energy subject to constraints, thus leading to a thermodynamically consistent EOS. The contribution to this free energy from the Coulomb interactions among the particles is treated using the method of Chabrier and Potekhin (Phys. Rev. E 58, 4941 (1998)) which we have adapted for partially ionized plasmas. This treatment is further examined and is found to give rise to unphysical behavior for various elements at certain values of the density and temperature where the Coulomb coupling begins to become significant and the atoms are partially ionized. We examine the source of this unphysical behavior and suggest corrections that produce acceptable results. The sensitivity of the thermodynamic properties and frequencydependent opacity of iron is examined with and without these corrections. The corrected EOS is used to determine the fractional ion populations and level populations for a new generation of OPLIB lowZ opacity tables currently being prepared at Los Alamos National Laboratory with the ATOMIC code. 

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ABSTRACT: Recent measurements using an Xray Free Electron Laser (XFEL) and an Electron Beam Ion Trap at the Linac Coherent Light Source facility highlighted large discrepancies between the observed and theoretical values for the Fe XVII 3C/3D line intensity ratio. This result raised the question of whether the theoretical oscillator strengths may be significantly in error, due to insufficiencies in the atomic structure calculations. We present timedependent spectral modeling of this experiment and show that nonequilibrium effects can dramatically reduce the predicted 3C/3D line intensity ratio, compared with that obtained by simply taking the ratio of oscillator strengths. Once these nonequilibrium effects are accounted for, the measured line intensity ratio can be used to determine a revised value for the 3C/3D oscillator strength ratio, giving a range from 3.0 to 3.5. We also provide a framework to narrow this range further, if more precise information about the pulse parameters can be determined. We discuss the implications of the new results for the use of Fe XVII spectral features as astrophysical diagnostics and investigate the importance of timedependent effects in interpreting XFELexcited plasmas. 
Article: The creation, destruction and transfer of multipole moments in electron–ion threebody recombination
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ABSTRACT: We use the wavepacket propagation scheme of Goldberger and Watson to define multipole moment creation, destruction, and transfer rates for the threebody recombination (TBR) of electrons with ions. We first assume shortrange interaction potentials and then consider Coulomb interactions, for which we use Dollards theory of multichannel scattering. We present the multipole moment rate coefficients in terms of the TBR amplitudes. Finally, we discuss timereversal invariance and the reciprocity relations, both for the shortrange case and for the Coulombinteraction case, and show that the multipole moment rate coefficients can be expressed in terms of electronimpact ionization amplitudes.  [Show abstract] [Hide abstract]
ABSTRACT: Relativistic distortedwave collision strengths have been calculated for the 185 δn=0 transitions with n=2 in the 67 Clike ions with nuclear charge number Z in the range 26≤Z≤92. The calculations were made for the six final, or scattered, electron energies E'=0.03,0.08,0.20,0.42,0.80, and 1.40, where E' is in units of Zeff2 Ry with Zeff=Z4.17. In addition, electric dipole oscillator strengths are provided. In the present collisionstrength calculations, an improved "topup" method, which employs relativistic plane waves, was used to obtain the high partialwave contribution for each transition, in contrast to the partialrelativistic CoulombBethe approximation used in previous work by Zhang and Sampson [H.L. Zhang, D.H. Sampson, At. Data Nucl. Data Tables 63 (1996) 275]. In that earlier work, collision strengths were also provided for the same 185 δn=0 transitions in Clike ions, but for the more limited list of 46 ions with Z in the range 9≤Z≤54. The collision strengths covered in the present work, particularly those for optically allowed transitions, should be more accurate than the corresponding data given by Zhang and Sampson [H.L. Zhang, D.H. Sampson, At. Data Nucl. Data Tables 63 (1996) 275] and are presented here to replace those earlier results.  [Show abstract] [Hide abstract]
ABSTRACT: Relativistic distortedwave collision strengths have been calculated for the 16 δn=0 optically allowed transitions with n=2 in the 67 Olike ions with nuclear charge number Z in the range 26≤Z≤92. The calculations were made for the four final, or scattered, electron energies E'=0.20, 0.42, 0.80, and 1.40, where E' is in units of Zeff2 Ry with Zeff=Z5.83. In the present calculations, an improved "topup" method, which employs relativistic plane waves, was used to obtain the high partialwave contribution for each transition, in contrast to the partialrelativistic CoulombBethe approximation used in previous work by Zhang and Sampson [H.L. Zhang, D.H. Sampson, At. Data Nucl. Data Tables 82 (2002) 357]. In that earlier work, collision strengths were also provided for Olike ions, but for a more comprehensive data set consisting of all possible 45 δn=0 transitions, six scattered energies, and the 79 ions with Z in the range 14≤Z≤92. The collision strengths covered in the present work should be more accurate than the corresponding data given by Zhang and Sampson [H.L. Zhang, D.H. Sampson, At. Data Nucl. Data Tables 82 (2002) 357] and are presented here to replace those earlier results.  [Show abstract] [Hide abstract]
ABSTRACT: Nearly a century ago it was recognized1 that radiation absorption by stellar matter controls the internal temperature profiles within stars. Laboratory opacity measurements, however, have never been performed at stellar interior conditions, introducing uncertainties in stellar models25. A particular problem arose2,3,68 when refined photosphere spectral analysis9,10 led to reductions of 3050 per cent in the inferred amounts of carbon, nitrogen and oxygen in the Sun. Standard solar models11 using the revised element abundances disagree with helioseismic observations that determine the internal solar structure using acoustic oscillations. This could be resolved if the true mean opacity for the solar interior matter were roughly 15 per cent higher than predicted2,3,68, because increased opacity compensates for thedecreased element abundances. Iron accounts for a quarter of the total opacity2,12 at the solar radiation/convection zone boundary. Here we report measurements of wavelengthresolved iron opacity at electron temperatures of 1.92.3 million kelvin and electron densities of (0.74.0)31022 per cubic centimetre, conditions very similar to those inthe solar region that affects thediscrepancy themost: the radiation/convection zone boundary. Themeasured wavelengthdependent opacity is 30400 per cent higher than predicted. This represents roughly half the change in the mean opacity needed to resolve the solar discrepancy, even though iron is only one of many elements that contribute to opacity.  [Show abstract] [Hide abstract]
ABSTRACT: We present an annotation of Hans Bethe’s “Bremsformel für Elektronen relativistischer Geschwindigkeit” [Zeitschrift für Physik 76, 293 (1932)] (Braking Formula for Electrons of Relativistic Speed). The English translation of the paper appears as a companion to this annotation. We highlight the conceptual and historical aspects of the relevant quantum electrodynamics employed by Bethe, provide details in the derivation of several equations, and point out some typographical errors in the original manuscript.  [Show abstract] [Hide abstract]
ABSTRACT: An accurate knowledge of atomic collision processes is important for a better understanding of many astrophysical and laboratory plasmas. Collision databases which contain electronimpact excitation, ionization, and recombination cross sections and temperature dependent rate coefficients have been constructed using perturbative distortedwave methods and nonperturbative Rmatrix pseudostates and timedependent closecoupling methods. We present recent atomic collision results.  [Show abstract] [Hide abstract]
ABSTRACT: Relativistic distortedwave collision strengths have been calculated for the 49 Delta n = 0 optically allowed transitions with n = 2 in the 67 Nlike ions with nuclear charge number Z in the range 26 <= Z <= 92. The calculations were made for the four final, or scattered, electron energies E' = 0.20, 0.42, 0.80, and 1.40, where E' is in units of Z(eff)(2) Ry with Z(eff) = Z  5. In the present calculations, an improved "topup" method, which employs relativistic plane waves, was used to obtain the high partialwave contribution for each transition, in contrast to the partialrelativistic CoulombBethe approximation used in the previous work by Zhang and Sampson [H.L. Zhang and D.H. Sampson, At. Data Nucl. Data Tables 72 (1999) 153]. In that earlier work, collision strengths were also provided for Nlike ions, but for a more comprehensive data set consisting of all possible 105 Delta n = 0 transitions, six scattered energies and the 81 ions with Z in the range 12 <= Z <= 92. The collision strengths covered in the present work should be more accurate than the corresponding data given by Zhang and Sampson [H.L. Zhang,and D.H. Sampson, At. Data Nucl. Data Tables 72 (1999) 153] and are presented here to replace those earlier results.  [Show abstract] [Hide abstract]
ABSTRACT: A series of experiments featuring laserimploded plasticshell targets filled with hydrogen or deuterium were performed on the National Ignition Facility. The shells (some deuterated) were doped in selected locations with Cu, Ga, and Ge, whose spectroscopic signals (indicative of local plasma conditions) were collected with a timeintegrated, 1D imaging, spectrally resolved, and absoluteintensity calibrated instrument. The experimental spectra compare well with radiation hydrodynamics simulations postprocessed with a nonlocal thermal equilibrium atomic kinetics and spectroscopicquality radiationtransport model. The obtained degree of agreement between the modeling and experimental data supports the application of spectroscopic techniques for the determination of plasma conditions, which can ultimately lead to the validation of theoretical models for thermonuclear burn in the presence of mix. Furthermore, the use of a lowerZ dopant element (e.g., Fe) is suggested for future experiments, since the ∼2 keV electron temperatures reached in mixed regions are not high enough to drive sufficient Hlike Ge and Cu line emissions needed for spectroscopic plasma diagnostics.  [Show abstract] [Hide abstract]
ABSTRACT: The full text of this article is available in the PDF provided.
Publication Stats
1k  Citations  
293.05  Total Impact Points  
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Institutions

19942015

Los Alamos National Laboratory
 • Theoretical Division
 • Applied Physics Division
ЛосАламос, California, United States


2014

Atomic Energy and Alternative Energies Commission
Fontenay, ÎledeFrance, France


2011

University of Texas at San Antonio
 Department of Physics and Astronomy
San Antonio, Texas, United States


19962002

California State University, Fullerton
 Department of Physics
Fullerton, California, United States


2000

Drake University
 Physics and Astronomy
Des Moines, Iowa, United States


19901994

Pennsylvania State University
 • Department of Astronomy and Astrophysics
 • Department of Physics
University Park, Maryland, United States
