Search

Your search keyword '"Loisel, G."' showing total 176 results
Start Over Author "Loisel, G."
176 results on '"Loisel, G."'

1. Milestone 7714 National Opacity Program: High-Fidelity Iron Data on NIF

Author

Colgan, J., primary, Cowan, J., additional, Day, T., additional, Dodd, E., additional, Fontes, C., additional, Hakel, P., additional, Johns, H., additional, Krasheninnikova, N., additional, Perry, T., additional, Robey, H., additional, Urbatsch, T., additional, Usov, I., additional, Vodnik, D., additional, Aberg, D., additional, Grabowski, P., additional, Heeter, R., additional, Opachich, Y., additional, Posadas, R., additional, Rubery, M., additional, Wilson, B., additional, Bailey, J., additional, Hansen, S., additional, Jones, B., additional, Loisel, G., additional, Nagayama, T., additional, Dutra, E., additional, Heinmiller, J., additional, Knight, R., additional, Moy, K., additional, Wallace, M., additional, Mayes, D., additional, Huang, H., additional, Monton, C., additional, Sequoia, K., additional, and Weir, M., additional

Published
2022
Full Text
View/download PDF

2. Parallax diagnostics of radiation source geometric dilution for iron opacity experiments

Author

Nagayama, T., Bailey, J. E., Loisel, G., Rochau, G. A., and Falcon, R. E.

Subjects
Astrophysics - Instrumentation and Methods for Astrophysics, Astrophysics - Solar and Stellar Astrophysics
Abstract

Experimental tests are in progress to evaluate the accuracy of the modeled iron opacity at solar interior conditions [J.E. Bailey et al., Phys. Plasmas 16, 058101 (2009)]. The iron sample is placed on top of the Sandia National Laboratories z-pinch dynamic hohlraum (ZPDH) radiation source. The samples are heated to 150 - 200 eV electron temperatures and 7e21 - 4e22 e/cc electron densities by the ZPDH radiation and backlit at its stagnation [T. Nagayama et al., Phys. Plasmas 21, 056502 (2014)]. The backlighter attenuated by the heated sample plasma is measured by four spectrometers along +/- 9 degree with respect to the z-pinch axis to infer the sample iron opacity. Here we describe measurements of the source-to-sample distance that exploit the parallax of spectrometers that view the half-moon-shaped sample from +/-9 degree. The measured sample temperature decreases with increased source-to-sample distance. This distance must be taken into account for understanding the sample heating., Comment: Published online 17 July 2014 (http://scitation.aip.org/content/aip/journal/rsi/85/11/10.1063/1.4889776)

Published
2014
Full Text
View/download PDF

3. Control and diagnosis of temperature, density, and uniformity in x-ray heated iron/magnesium samples for opacity measurements

Author

Nagayama, T., Bailey, J. E., Loisel, G., Hansen, S. B., Rochau, G. A., Mancini, R. C., MacFarlane, J. J., and Golovkin, I.

Subjects
Astrophysics - Solar and Stellar Astrophysics, Physics - Plasma Physics
Abstract

Experimental tests are in progress to evaluate the accuracy of the modeled iron opacity at solar interior conditions, in particular to better constrain the solar abundance problem [S. Basu and H.M. Antia, Physics Reports 457, 217 (2008)]. Here we describe measurements addressing three of the key requirements for reliable opacity experiments: control of sample conditions, independent sample condition diagnostics, and verification of sample condition uniformity. The opacity samples consist of iron/magnesium layers tamped by plastic. By changing the plastic thicknesses, we have controlled the iron plasma conditions to reach i) Te=167+/-3 eV and ne=(7.1+/-1.5)e21 e/cc, ii) Te=170+/-2 eV and ne=(2.0+/-0.2)e22 e/cc, and iii) Te=196+/-6 eV and ne=(3.8+/-0.8)e22 e/cc, which were measured by magnesium tracer K-shell spectroscopy. The opacity sample non-uniformity was directly measured by a separate experiment where Al is mixed into the side of the sample facing the radiation source and Mg into the other side. The iron condition was confirmed to be uniform within their measurement uncertainties by Al and Mg K-shell spectroscopy. The conditions are suitable for testing opacity calculations needed for modeling the solar interior, other stars, and high energy density plasmas., Comment: Published online 14 May 2014

Published
2014
Full Text
View/download PDF

4. Fusion reactions initiated by laser-accelerated particle beams in a laser-produced plasma

Author

Labaune, C., Baccou, C., Depierreux, S., Goyon, C., Loisel, G., Yahia, V., and Rafelski, J.

Subjects
Physics - Plasma Physics, Nuclear Experiment, Physics - Accelerator Physics, Physics - Optics
Abstract

The advent of high-intensity pulsed laser technology enables the generation of extreme states of matter under conditions that are far from thermal equilibrium. This in turn could enable different approaches to generating energy from nuclear fusion. Relaxing the equilibrium requirement could widen the range of isotopes used in fusion fuels permitting cleaner and less hazardous reactions that do not produce high energy neutrons. Here we propose and implement a means to drive fusion reactions between protons and boron-11 nuclei, by colliding a laser-accelerated proton beam with a laser-generated boron plasma. We report proton-boron reaction rates that are orders of magnitude higher than those reported previously. Beyond fusion, our approach demonstrates a new means for exploring low-energy nuclear reactions such as those that occur in astrophysical plasmas and related environments., Comment: 7 pages, 5 figures

Published
2013
Full Text
View/download PDF

5. Comparison of Fe and Ni opacity calculations for a better understanding of pulsating stellar envelopes

Author

Gilles, D., Turck-Chièze, S., Loisel, G., Piau, L., Ducret, J. -E., Poirier, M., Blenski, T., Thais, F., Blancard, C., Cossé, P., Faussurier, G., Gilleron, F., Pain, J. -C., Porcherot, Q., Guzik, J. A., Kilcrease, D. P., Magee, N. H., Harris, J., Busquet, M., Delahaye, F., Zeippen, C. J., and Bastiani-Ceccotti, S.

Subjects
Astrophysics - Solar and Stellar Astrophysics, Physics - Atomic Physics, Physics - Plasma Physics
Abstract

Opacity is an important ingredient of the evolution of stars. The calculation of opacity coefficients is complicated by the fact that the plasma contains partially ionized heavy ions that contribute to opacity dominated by H and He. Up to now, the astrophysical community has greatly benefited from the work of the contributions of Los Alamos [1], Livermore [2] and the Opacity Project (OP) [3]. However unexplained differences of up to 50% in the radiative forces and Rosseland mean values for Fe have been noticed for conditions corresponding to stellar envelopes. Such uncertainty has a real impact on the understanding of pulsating stellar envelopes, on the excitation of modes, and on the identification of the mode frequencies. Temperature and density conditions equivalent to those found in stars can now be produced in laboratory experiments for various atomic species. Recently the photo-absorption spectra of nickel and iron plasmas have been measured during the LULI 2010 campaign, for temperatures between 15 and 40 eV and densities of ~3 mg/cm3. A large theoretical collaboration, the "OPAC", has been formed to prepare these experiments. We present here the set of opacity calculations performed by eight different groups for conditions relevant to the LULI 2010 experiment and to astrophysical stellar envelope conditions., Comment: 15 pages, 10 figures

Published
2012
Full Text
View/download PDF

6. On plasma radiative properties in stellar conditions

Author

Turck-Chièze, S., Delahaye, F., Gilles, D., Loisel, G., and Piau, L.

Subjects
Astrophysics - Solar and Stellar Astrophysics, Physics - Plasma Physics
Abstract

The knowledge of stellar evolution is evolving quickly thanks to an increased number of opportunities to scrutinize the stellar internal plasma properties by stellar seismology and by 1D and 3D simulations. These new tools help us to introduce the internal dynamical phenomena in stellar modeling. A proper inclusion of these processes supposes a real confidence in the microscopic physics used, partly checked by solar or stellar acoustic modes. In the present paper we first recall which fundamental physics has been recently verified by helioseismology. Then we recall that opacity is an important ingredient of the secular evolution of stars and we point out why it is necessary to measure absorption coefficients and degrees of ionization in the laboratory for some well identified astrophysical conditions. We examine two specific experimental conditions which are accessible to large laser facilities and are suitable to solve some interesting questions of the stellar community: are the solar internal radiative interactions properly estimated and what is the proper role of the opacity in the excitation of the non radial modes in the envelop of the $\beta$ Cephei and the Be stars ? At the end of the paper we point out the difficulties of the experimental approach that we need to overcome., Comment: 7 pages, 6 figures, published in HEDP 2009

Published
2012
Full Text
View/download PDF

7. Iron and Nickel spectral opacity calculations in conditions relevant for pulsating stellar envelopes and experiments

Author

Gilles, D., Turck-Chièze, S., Busquet, M., Thais, F., Loisel, G., Piau, L., Ducret, J. E., Blenski, T., Blancard, C., Cossé, P., Faussurier, G., Gilleron, F., Pain, J. C., Porcherot, Q., Guzik, J. A., Kilcrease, D. P., Magee, N. H., Harris, J., Bastiani-Ceccotti, S., Delahaye, F., and Zeippen, C. J.

Subjects
Astrophysics - Solar and Stellar Astrophysics, Physics - Atomic Physics, Physics - Plasma Physics
Abstract

Seismology of stars is strongly developing. To address this question we have formed an international collaboration OPAC to perform specific experimental measurements, compare opacity calculations and improve the opacity calculations in the stellar codes [1]. We consider the following opacity codes: SCO, CASSANDRA, STA, OPAS, LEDCOP, OP, SCO-RCG. Their comparison has shown large differences for Fe and Ni in equivalent conditions of envelopes of type II supernova precursors, temperatures between 15 and 40 eV and densities of a few mg/cm3 [2, 3, 4]. LEDCOP, OPAS, SCO-RCG structure codes and STA give similar results and differ from OP ones for the lower temperatures and for spectral interval values [3]. In this work we discuss the role of Configuration Interaction (CI) and the influence of the number of used configurations. We present and include in the opacity code comparisons new HULLAC-v9 calculations [5, 6] that include full CI. To illustrate the importance of this effect we compare different CI approximations (modes) available in HULLAC-v9 [7]. These results are compared to previous predictions and to experimental data. Differences with OP results are discussed., Comment: 4 pages, 3 figures, conference Inertial Fusion Sciences and Applications, Bordeaux, 12th to 16th September 2011; EPJ web of Conferences 2012

Published
2012
Full Text
View/download PDF

8. Radiative properties of stellar plasmas and open challenges

Author

Turck-Chièze, S., Loisel, G., Gilles, D., Piau, L., Blancard, C., Blenski, T., Busquet, M., Caillaud, T., Cossé, P., Delahaye, F., Faussurier, G., Fariaut, J., Gilleron, F., Guzik, J. A., Harris, J., Kilcrease, D. P., Magee, N. H., Pain, J. C., Porcherot, Q., Poirier, M., Soullier, G., Zeippen, C. J., Bastiani-Ceccotti, S., Reverdin, C., Silvert, V., Thais, F., and Villette, B.

Subjects
Astrophysics - Solar and Stellar Astrophysics, Physics - Plasma Physics
Abstract

The lifetime of solar-like stars, the envelope structure of more massive stars, and stellar acoustic frequencies largely depend on the radiative properties of the stellar plasma. Up to now, these complex quantities have been estimated only theoretically. The development of the powerful tools of helio- and astero- seismology has made it possible to gain insights on the interiors of stars. Consequently, increased emphasis is now placed on knowledge of the monochromatic opacity coefficients. Here we review how these radiative properties play a role, and where they are most important. We then concentrate specifically on the envelopes of $\beta$ Cephei variable stars. We discuss the dispersion of eight different theoretical estimates of the monochromatic opacity spectrum and the challenges we need to face to check these calculations experimentally., Comment: 6 pages, 5 figures, in press (conference HEDLA 2010)

Published
2011
Full Text
View/download PDF

9. Theoretical and experimental activities on opacities for a good interpretation of seismic stellar probes

Author

Turck-Chièze, S, Loisel, G, Gilles, D, Thais, F, Bastiani, S, Blancard, C, Busquet, M, Caillaud, T, Cosse, P, Blenski, T, Delahaye, F, Ducret, J E, Faussurier, G, Gilleron, F, Guzik, J, Harris, J W, Kilcrease, D P, Magee, N H, Piau, L, Pain, J C, Poirier, M, Porcherot, Q, Reverdin, C, Silvert, V, Villette, B, and Zeippen, C

Subjects
Astrophysics - Solar and Stellar Astrophysics
Abstract

Opacity calculations are basic ingredients of stellar modelling. They play a crucial role in the interpretation of acoustic modes detected by SoHO, COROT and KEPLER. In this review we present our activities on both theoretical and experimental sides. We show new calculations of opacity spectra and comparisons between eight groups who produce opacity spectra calculations in the domain where experiments are scheduled. Real differences are noticed with real astrophysical consequences when one extends helioseismology to cluster studies of different compositions. Two cases are considered presently: (1) the solar radiative zone and (2) the beta Cephei envelops. We describe how our experiments are performed and new preliminary results on nickel obtained in the campaign 2010 at LULI 2000 at Polytechnique., Comment: 6 pages, 4 figures, invited talk at SOHO24

Published
2011
Full Text
View/download PDF

12. Domination of the K-Radiation at a Z-Pinch Stagnation on Z by Numerous Tiny Spots and the Properties of the Spots Inferred by Experimental Determination of the K-Line Opacities

Author

Maron, Y., primary, Bernshtam, V., additional, Zarnitsky, Y., additional, Fisher, V., additional, Nedostup, O., additional, Ampleford, D. J., additional, Jennings, C. A., additional, Jones, B., additional, Cuneo, M. E., additional, Rochau, G. A., additional, Dunham, G. S., additional, and Loisel, G. P., additional

Published
2022
Full Text
View/download PDF

13. Development and integration of photonic Doppler velocimetry as a diagnostic for radiation driven experiments on the Z-machine

Author

Swanson, K. J., primary, Jaar, G. S., additional, Mayes, D. C., additional, Mancini, R. C., additional, Ivanov, V. V., additional, Astanovitskiy, A. L., additional, Dmitriev, O., additional, Klemmer, A. W., additional, De La Cruz, C., additional, Dolan, D., additional, Porwitzky, A., additional, Loisel, G. P., additional, and Bailey, J. E., additional

Published
2022
Full Text
View/download PDF

14. Radiative properties of stellar envelopes: Comparison of asteroseismic results to opacity calculations and measurements for iron and nickel

Author

Turck-Chièze, S., Gilles, D., Le Pennec, M., Blenski, T., Thais, F., Bastiani-Ceccotti, S., Blancard, C., Busquet, M., Caillaud, T., Colgan, J., Cossé, P., Delahaye, F., Ducreta, J.E., Faussurier, G., Fontes, C.J., Gilleron, F., Guzik, J., Harris, J.W., Kilcrease, D.P., Loisel, G., Magee, N.H., Pain, J.C., Reverdin, C., Silvert, V., Villette, B., and Zeippen, C.J.

Published
2013
Full Text
View/download PDF

23. Review of pulsed power-driven high energy density physics research on Z at Sandia

Author

Sinars, D. B., primary, Sweeney, M. A., additional, Alexander, C. S., additional, Ampleford, D. J., additional, Ao, T., additional, Apruzese, J. P., additional, Aragon, C., additional, Armstrong, D. J., additional, Austin, K. N., additional, Awe, T. J., additional, Baczewski, A. D., additional, Bailey, J. E., additional, Baker, K. L., additional, Ball, C. R., additional, Barclay, H. T., additional, Beatty, S., additional, Beckwith, K., additional, Bell, K. S., additional, Benage, J. F., additional, Bennett, N. L., additional, Blaha, K., additional, Bliss, D. E., additional, Boerner, J. J., additional, Bourdon, C. J., additional, Branch, B. A., additional, Brown, J. L., additional, Campbell, E. M., additional, Campbell, R. B., additional, Chacon, D. G., additional, Chandler, G. A., additional, Chandler, K., additional, Christenson, P. J., additional, Christison, M. D., additional, Christner, E. B., additional, Clay, R. C., additional, Cochrane, K. R., additional, Colombo, A. P., additional, Cook, B. M., additional, Coverdale, C. A., additional, Cuneo, M. E., additional, Custer, J. S., additional, Dasgupta, A., additional, Davis, J.-P., additional, Desjarlais, M. P., additional, Dolan, D. H., additional, Douglass, J. D., additional, Dunham, G. S., additional, Duwal, S., additional, Edens, A. D., additional, Edwards, M. J., additional, Evstatiev, E. G., additional, Farfan, B. G., additional, Fein, J. R., additional, Field, E. S., additional, Fisher, J. A., additional, Flanagan, T. M., additional, Flicker, D. G., additional, Furnish, M. D., additional, Galloway, B. R., additional, Gard, P. D., additional, Gardiner, T. A., additional, Geissel, M., additional, Giuliani, J. L., additional, Glinsky, M. E., additional, Gomez, M. R., additional, Gomez, T., additional, Grim, G. P., additional, Hahn, K. D., additional, Haill, T. A., additional, Hamlin, N. D., additional, Hammer, J. H., additional, Hansen, S. B., additional, Hanshaw, H. L., additional, Harding, E. C., additional, Harvey-Thompson, A. J., additional, Headley, D., additional, Herrmann, M. C., additional, Hess, M. H., additional, Highstrete, C., additional, Hurricane, O. A., additional, Hutsel, B. T., additional, Jennings, C. A., additional, Johns, O. M., additional, Johnson, D., additional, Johnston, M. D., additional, Jones, B. M., additional, Jones, M. C., additional, Jones, P. A., additional, Kalita, P. E., additional, Kamm, R. J., additional, Kellogg, J. W., additional, Kiefer, M. L., additional, Kimmel, M. W., additional, Knapp, P. F., additional, Knudson, M. D., additional, Kreft, A., additional, Laity, G. R., additional, Lake, P. W., additional, Lamppa, D. C., additional, Langston, W. L., additional, Lash, J. S., additional, LeChien, K. R., additional, Leckbee, J. J., additional, Leeper, R. J., additional, Leifeste, G. T., additional, Lemke, R. W., additional, Lewis, W., additional, Lewis, S. A., additional, Loisel, G. P., additional, Looker, Q. M., additional, Lopez, A. J., additional, Lucero, D. J., additional, MacLaren, S. A., additional, Magyar, R. J., additional, Mangan, M. A., additional, Martin, M. R., additional, Mattsson, T. R., additional, Matzen, M. K., additional, Maurer, A. J., additional, Mazarakis, M. G., additional, McBride, R. D., additional, McLean, H. S., additional, McCoy, C. A., additional, McKee, G. R., additional, McKenney, J. L., additional, Miles, A. R., additional, Mills, J. A., additional, Mitchell, M. D., additional, Moore, N. W., additional, Myers, C. E., additional, Nagayama, T., additional, Natoni, G., additional, Owen, A. C., additional, Patel, S., additional, Peterson, K. J., additional, Pointon, T. D., additional, Porter, J. L., additional, Porwitzky, A. J., additional, Radovich, S., additional, Raman, K. S., additional, Rambo, P. K., additional, Reinhart, W. D., additional, Robertson, G. K., additional, Rochau, G. A., additional, Root, S., additional, Rose, D. V., additional, Rovang, D. C., additional, Ruiz, C. L., additional, Ruiz, D. E., additional, Sandoval, D., additional, Savage, M. E., additional, Sceiford, M. E., additional, Schaeuble, M. A., additional, Schmit, P. F., additional, Schollmeier, M. S., additional, Schwarz, J., additional, Seagle, C. T., additional, Sefkow, A. B., additional, Seidel, D. B., additional, Shipley, G. A., additional, Shores, J., additional, Shulenburger, L., additional, Simpson, S. C., additional, Slutz, S. A., additional, Smith, I. C., additional, Speas, C. S., additional, Specht, P. E., additional, Speir, M. J., additional, Spencer, D. C., additional, Springer, P. T., additional, Steiner, A. M., additional, Stoltzfus, B. S., additional, Stygar, W. A., additional, Ward Thornhill, J., additional, Torres, J. A., additional, Townsend, J. P., additional, Tyler, C., additional, Vesey, R. A., additional, Wakeland, P. E., additional, Webb, T. J., additional, Weinbrecht, E. A., additional, Weis, M. R., additional, Welch, D. R., additional, Wise, J. L., additional, Wu, M., additional, Yager-Elorriaga, D. A., additional, Yu, A., additional, and Yu, E. P., additional

Published
2020
Full Text
View/download PDF

25. Laser-plasma interaction physics for shock ignition

Author

Goyon C., Depierreux S., Michel D.T., Loisel G., Yahia V., Masson-Laborde P.E., Loiseau P., Hüller S., Borisenko N.G., Orekhov A., Rosmej O., Nicolaï P., Tikhonchuk V.T., and Labaune C.

Subjects
Physics, QC1-999
Abstract

In the shock ignition scheme, the ICF target is first compressed with a long (nanosecond) pulse before creating a convergent shock with a short (∼100 ps) pulse to ignite thermonuclear reactions. This short pulse is typically (∼2.1015–1016 W/cm2) above LPI (Laser Plasma Instabilities) thresholds. The plasma is in a regime where the electron temperature is expected to be very high (2–4 keV) and the laser coupling to the plasma is not well understood. Emulating LPI in the corona requires large and hot plasmas produced by high-energy lasers. We conducted experiments on the LIL (Ligne d'Integration Laser, 10 kJ at 3ω) and the LULI2000 (0.4 kJ at 2ω) facilities, to approach these conditions and study absorption and LPI produced by a high intensity beam in preformed plasmas. After introducing the main risks associated with the short pulse propagation, we present the latest experiment we conducted on LPI in relevant conditions for shock ignition.

Published
2013
Full Text
View/download PDF

26. Effects of hydrodynamics on Stimulated Brillouin Scattering in multiple plasma interaction

Author

Yahia V., Depierreux S., Goyon C., Loisel G., Borisenko N.G., Masson-Laborde P.E., Orekhov A., Rienecker T., Rosmej O., and Labaune C.

Subjects
Physics, QC1-999
Abstract

In this paper, an experiment carried out on LULI2000 facility is presented. It was designed to investigate how two successive plasmas interact through hydrodynamic coupling and electromagnetic radiations. Contributions of both effects have been successfully identified and the effects of hydrodynamic coupling on Stimulated Brillouin Scattering has been observed.

Published
2013
Full Text
View/download PDF

27. Theoretical interpretation for 2p − nd absorption spectra of iron, nickel, and copper in X-ray range measured at the LULI2000 facility

Author

Poirier M., Arnault P., Bastiani-Ceccotti S., Blenski T., Dortan F. de Gaufridy de, Gilleron F., Loisel G., Pain J.-C., Porcherot Q., Reverdin C., Silvert V., Thais F., and Turck-Chièze S.

Subjects
Physics, QC1-999
Abstract

The 2p − nd absorption structures in medium Z elements present a valuable benchmark for atomic models since they exhibit a complex dependence on temperature and density. For these transitions lying in the X-ray range, one observes a competition between the spin-orbit splitting and the broadening associated to the excitation of complex structures. Detailed opacity codes based on the HULLAC or FAC suites agree with the statistical code SCO; but in iron computations predict higher peak absorption than measured. An addition procedure on opacities calculated with detailed codes is proposed and successfully tested.

Published
2013
Full Text
View/download PDF

28. Iron and Nickel spectral opacity calculations in conditions relevant for pulsating stellar envelopes and experiments

Author

Gilles D., Turck-Chièze S., Busquet M., Thais F., Loisel G., Piau L., Ducret J.E., Blenski T., Blancard C., Cossé P., Faussurier G., Gilleron F., Pain J.C., Porcherot Q., Guzik J.A., Kilcrease D.P., Magee N.H., Harris J., Bastiani-Ceccotti S., Delahaye F., and Zeippen C.J

Subjects
Physics, QC1-999
Abstract

Seismology of stars is strongly developing. To address this question we have formed an international collaboration, OPAC, to perform specific experimental measurements, compare opacity calculations, and improve the opacity calculations in stellar codes [1]. We consider the following opacity codes: SCO, CASSANDRA, STA, OPAS, LEDCOP, OP, SCO-RCG. Their comparison has shown large differences for Fe and Ni in equivalent conditions of envelopes of type II supernova precursors, temperatures between 15 and 40 eV and densities of a few mg/cm3 [2–4]. LEDCOP, OPAS, SCO-RCG structure codes and STA give similar results and differ from OP ones for the lower temperatures and for spectral interval values [3]. In this work we discuss the role of Configuration Interaction (CI) and the influence of the number of used configurations. We present and include in the opacity code comparisons new HULLAC-v9 calculations [5, 6] that include full CI. To illustrate the importance of this effect we compare different CI approximations (modes) available in HULLAC-v9 [7]. These results are compared to previous predictions and to experimental data. Differences with OP results are discussed.

Published
2013
Full Text
View/download PDF

29. Systematic Study of L -Shell Opacity at Stellar Interior Temperatures

Author

Nagayama, T., primary, Bailey, J. E., additional, Loisel, G. P., additional, Dunham, G. S., additional, Rochau, G. A., additional, Blancard, C., additional, Colgan, J., additional, Cossé, Ph., additional, Faussurier, G., additional, Fontes, C. J., additional, Gilleron, F., additional, Hansen, S. B., additional, Iglesias, C. A., additional, Golovkin, I. E., additional, Kilcrease, D. P., additional, MacFarlane, J. J., additional, Mancini, R. C., additional, More, R. M., additional, Orban, C., additional, Pain, J.-C., additional, Sherrill, M. E., additional, and Wilson, B. G., additional

Published
2019
Full Text
View/download PDF

32. A 7.2 keV spherical x-ray crystal backlighter for two-frame, two-color backlighting at Sandia’s Z Pulsed Power Facility

Author

Schollmeier, M. S., primary, Knapp, P. F., additional, Ampleford, D. J., additional, Harding, E. C., additional, Jennings, C. A., additional, Lamppa, D. C., additional, Loisel, G. P., additional, Martin, M. R., additional, Robertson, G. K., additional, Shores, J. E., additional, Smith, I. C., additional, Speas, C. S., additional, Weis, M. R., additional, Porter, J. L., additional, and McBride, R. D., additional

Published
2017
Full Text
View/download PDF

35. Direct measurement of the inertial confinement time in a magnetically driven implosion

Author

Knapp, P. F., primary, Martin, M. R., additional, Dolan, D. H., additional, Cochrane, K., additional, Dalton, D., additional, Davis, J.-P., additional, Jennings, C. A., additional, Loisel, G. P., additional, Romero, D. H., additional, Smith, I. C., additional, Yu, E. P., additional, Weis, M. R., additional, Mattsson, T. R., additional, McBride, R. D., additional, Peterson, K., additional, Schwarz, J., additional, and Sinars, D. B., additional

Published
2017
Full Text
View/download PDF

39. The differential absorption hard x-ray (DAHX) spectrometer at the Z facility

Author

Bell, K. S., primary, Coverdale, C. A., additional, Ampleford, D. J., additional, Bailey, J. E., additional, Loisel, G., additional, Harper-Slaboszewicz, V., additional, Schwarz, J., additional, Christener, E., additional, Turner, C., additional, McPherson, L. A., additional, Bourdon, C., additional, Kernaghan, M., additional, Sullivan, M., additional, Kirtley, C., additional, and Cuneo, M. E., additional

Published
2016
Full Text
View/download PDF

45. A higher-than-predicted measurement of iron opacity at solar interior temperatures

Author

Bailey, J. E., primary, Nagayama, T., additional, Loisel, G. P., additional, Rochau, G. A., additional, Blancard, C., additional, Colgan, J., additional, Cosse, Ph., additional, Faussurier, G., additional, Fontes, C. J., additional, Gilleron, F., additional, Golovkin, I., additional, Hansen, S. B., additional, Iglesias, C. A., additional, Kilcrease, D. P., additional, MacFarlane, J. J., additional, Mancini, R. C., additional, Nahar, S. N., additional, Orban, C., additional, Pain, J.-C., additional, Pradhan, A. K., additional, Sherrill, M., additional, and Wilson, B. G., additional

Published
2014
Full Text
View/download PDF

50. ZAPP: The Z Astrophysical Plasma Properties collaboration

Author

Rochau, G. A., primary, Bailey, J. E., additional, Falcon, R. E., additional, Loisel, G. P., additional, Nagayama, T., additional, Mancini, R. C., additional, Hall, I., additional, Winget, D. E., additional, Montgomery, M. H., additional, and Liedahl, D. A., additional

Published
2014
Full Text
View/download PDF

Catalog

Books, media, physical & digital resources
See catalog results