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Jurewicz AJG, Rieck KD, Hervig R, Burnett DS, Wadhwa M, Olinger CT, Wiens RC, Laming JM, Guan Y, Huss GR, Reisenfeld DB, Williams P. Magnesium isotopes of the bulk solar wind from Genesis diamond-like carbon films. Meteorit Planet Sci 2020; 55:352-375. [PMID: 32214784 PMCID: PMC7079557 DOI: 10.1111/maps.13439] [Citation(s) in RCA: 1] [Impact Index Per Article: 0.3] [Reference Citation Analysis] [What about the content of this article? (0)] [Affiliation(s)] [Abstract] [Grants] [Track Full Text] [Figures] [Subscribe] [Scholar Register] [Received: 12/09/2018] [Accepted: 12/10/2019] [Indexed: 06/10/2023]
Abstract
NASA's Genesis Mission returned solar wind (SW) to the Earth for analysis to derive the composition of the solar photosphere from solar material. SW analyses control the precision of the derived solar compositions, but their ultimate accuracy is limited by the theoretical or empirical models of fractionation due to SW formation. Mg isotopes are "ground truth" for these models since, except for CAIs, planetary materials have a uniform Mg isotopic composition (within ≤1‰) so any significant isotopic fractionation of SW Mg is primarily that of SW formation and subsequent acceleration through the corona. This study analyzed Mg isotopes in a bulk SW diamond-like carbon (DLC) film on silicon collector returned by the Genesis Mission. A novel data reduction technique was required to account for variable ion yield and instrumental mass fractionation (IMF) in the DLC. The resulting SW Mg fractionation relative to the DSM-3 laboratory standard was (-14.4‰, -30.2‰) ± (4.1‰, 5.5‰), where the uncertainty is 2ơ SE of the data combined with a 2.5‰ (total) error in the IMF determination. Two of the SW fractionation models considered generally agreed with our data. Their possible ramifications are discussed for O isotopes based on the CAI nebular composition of McKeegan et al. (2011).
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Affiliation(s)
- A. J. G. Jurewicz
- Center for Meteorite StudiesArizona State Universitym/c 6004TempeArizona85287USA
| | - K. D. Rieck
- New Mexico Consortium4200 West Jemez Road Suite 200Los AlamosNew Mexico87544USA
| | - R. Hervig
- School of Earth and Space ExplorationArizona State UniversityTempeArizona85287USA
| | - D. S. Burnett
- Department of Geology and Planetary SciencesCalifornia Institute of Technologym/c 100‐23PasadenaCalifornia91125USA
| | - M. Wadhwa
- School of Earth and Space ExplorationArizona State UniversityTempeArizona85287USA
| | - C. T. Olinger
- GET‐NSA, LLC, AU‐6219901 Germantown RdGermantownMaryland20875USA
| | - R. C. Wiens
- Los Alamos National Laboratory (Remote Sensing)ISR‐2, m/s C‐331Los AlamosNew Mexico87545USA
| | - J. M. Laming
- Naval Research LaboratorySpace Science DivisionCode 7684WashingtonDistrict of Columbia20375USA
| | - Y. Guan
- Geological and Planetary SciencesCalifornia Institute of Technologym/c 100‐10PasadenaCalifornia91125USA
| | - G. R. Huss
- Hawaii Institute of Geophysics and PlanetologyUniversity of Hawaii at Manoa1680 East‐West Road, Post 504HonoluluHawaii96822USA
| | - D. B. Reisenfeld
- Los Alamos National Laboratory ISR‐1Los AlamosNew Mexico87545USA
| | - P. Williams
- School of Molecular SciencesArizona State UniversityTempeArizona85287USA
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Seitenzahl IR, Ghavamian P, Laming JM, Vogt FPA. Optical Tomography of Chemical Elements Synthesized in Type Ia Supernovae. Phys Rev Lett 2019; 123:041101. [PMID: 31491236 DOI: 10.1103/physrevlett.123.041101] [Citation(s) in RCA: 0] [Impact Index Per Article: 0] [Reference Citation Analysis] [What about the content of this article? (0)] [Affiliation(s)] [Abstract] [Track Full Text] [Subscribe] [Scholar Register] [Received: 04/17/2019] [Indexed: 06/10/2023]
Abstract
We report the discovery of optical emission from the nonradiative shocked ejecta of three young type Ia supernova remnants (SNRs): SNR 0519-69.0, SNR 0509-67.5, and N103B. Deep integral field spectroscopic observations reveal broad and spatially resolved [Fe XIV] 5303 Å emission. The width of the broad line reveals, for the first time, the reverse shock speeds. For two of the remnants we can constrain the underlying supernova explosions with evolutionary models. SNR 0519-69.0 is well explained by a standard near-Chandrasekhar mass explosion, whereas for SNR 0509-67.5 our analysis suggests an energetic sub-Chandrasekhar mass explosion. With [S XII], [Fe IX], and [Fe XV] also detected, we can uniquely visualize different layers of the explosion. We refer to this new analysis technique as "supernova remnant tomography".
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Affiliation(s)
- I R Seitenzahl
- School of Science, University of New South Wales, Australian Defence Force Academy, Canberra, ACT 2600, Australia
| | - P Ghavamian
- Department of Physics, Astronomy and Geosciences, Towson University, Towson, Maryland 21252, USA
| | - J M Laming
- Space Science Division Code 7684, Naval Research Laboratory, Washington, D.C. 20375, USA
| | - F P A Vogt
- European Southern Observatory, Av. Alonso de Córdova 3107, 763 0355 Vitacura, Santiago, Chile
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Moses JD, Ko YK, Laming JM, Provornikova EA, Strachan L, Beltran ST. Ultraviolet and extreme ultraviolet spectroscopy of the solar corona at the Naval Research Laboratory. Appl Opt 2015; 54:F222-F231. [PMID: 26560611 DOI: 10.1364/ao.54.00f222] [Citation(s) in RCA: 0] [Impact Index Per Article: 0] [Reference Citation Analysis] [What about the content of this article? (0)] [Abstract] [Track Full Text] [Subscribe] [Scholar Register] [Indexed: 06/05/2023]
Abstract
We review the history of ultraviolet and extreme ultraviolet spectroscopy with a specific focus on such activities at the Naval Research Laboratory and on studies of the extended solar corona and solar-wind source regions. We describe the problem of forecasting solar energetic particle events and discuss an observational technique designed to solve this problem by detecting supra-thermal seed particles as extended wings on spectral lines. Such seed particles are believed to be a necessary prerequisite for particle acceleration by heliospheric shock waves driven by a coronal mass ejection.
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Chen GX, Kirby K, Silver E, Brickhouse NS, Gillaspy JD, Tan JN, Pomeroy JM, Laming JM. The 3C/3D line ratio in Ni XIX: New Ab Initio theory and experimental results. Phys Rev Lett 2006; 97:143201. [PMID: 17155246 DOI: 10.1103/physrevlett.97.143201] [Citation(s) in RCA: 0] [Impact Index Per Article: 0] [Reference Citation Analysis] [What about the content of this article? (0)] [Affiliation(s)] [Abstract] [Track Full Text] [Subscribe] [Scholar Register] [Received: 03/21/2006] [Indexed: 05/12/2023]
Abstract
We report a fully relativistic close-coupling calculation of the electron impact excitation of Ni xix to derive the 3C/3D line intensity ratio, with an uncertainty of 5%. Convergence of the calculation with respect to both channel coupling effects and the many interacting Rydberg series of resonances has been achieved. New measurements in an electron beam ion trap agree with our calculation. We show that the 3C/3D x-ray line ratio depends sensitively on both electron energy and beamwidth in an optically thin plasma. Accounting for this dependence improves the accuracy of the Ni abundance determination in astrophysical sources.
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Affiliation(s)
- G X Chen
- ITAMP, Harvard-Smithsonian Center for Astrophysics, 60 Garden Street, Cambridge, MA 02138, USA
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Seely JF, Goray LI, Kjornrattanawanich B, Laming JM, Holland GE, Flanagan KA, Heilmann RK, Chang CH, Schattenburg ML, Rasmussen AP. Efficiency of a grazing-incidence off-plane grating in the soft-x-ray region. Appl Opt 2006; 45:1680-7. [PMID: 16572682 DOI: 10.1364/ao.45.001680] [Citation(s) in RCA: 2] [Impact Index Per Article: 0.1] [Reference Citation Analysis] [What about the content of this article? (0)] [Affiliation(s)] [Abstract] [Track Full Text] [Subscribe] [Scholar Register] [Indexed: 05/08/2023]
Abstract
Efficiency measurements of a grazing-incidence diffraction grating in the off-plane mount were performed using polarized synchrotron radiation. The grating had 5000 grooves/mm, an effective blaze angle of 14 degrees, and was gold coated. The efficiencies in the two polarization orientations (TM and TE) were measured in the 1.5-5.0 nm wavelength range and were compared with the efficiencies calculated using the PCGrate-SX code. The TM and TE efficiencies differ, offering the possibility of performing unique science studies of astrophysical, solar, and laboratory sources by exploiting the polarization sensitivity of the off-plane grating.
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Affiliation(s)
- J F Seely
- Space Science Division, U.S. Naval Research Laboratory, Washington, D.C. 20375, USA.
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Back CA, Grun J, Decker C, Suter LJ, Davis J, Landen OL, Wallace R, Hsing WW, Laming JM, Feldman U, Miller MC, Wuest C. Efficient multi-keV underdense laser-produced plasma radiators. Phys Rev Lett 2001; 87:275003. [PMID: 11800887 DOI: 10.1103/physrevlett.87.275003] [Citation(s) in RCA: 3] [Impact Index Per Article: 0.1] [Reference Citation Analysis] [What about the content of this article? (0)] [Affiliation(s)] [Abstract] [Track Full Text] [Subscribe] [Scholar Register] [Received: 06/02/2000] [Indexed: 05/23/2023]
Abstract
Novel, efficient x-ray sources have been created by supersonically heating a large volume of Xe gas. A laser-induced bleaching wave quickly ionizes the high- Z gas, and the resulting plasma emits x rays. This method significantly improves the production of hard x rays because less energy is lost to kinetic energy and sub-keV x rays. The conversion efficiency of laser energy into L-shell radiation between 4-7 keV is measured at approximately 10%, an order of magnitude higher than efficiencies measured from solid disk targets. This higher flux enables material testing and backlighting in new regimes and scales well to future high-powered lasers.
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Affiliation(s)
- C A Back
- Lawrence Livermore National Laboratory, L-21, P.O. Box 808, Livermore, California 94551, USA
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Kink I, Laming JM, Takács E, Porto JV, Gillaspy JD, Silver E, Schnopper H, Bandler SR, Barbera M, Brickhouse N, Murray S, Madden N, Landis D, Beeman J, Haller EE. Analysis of broadband x-ray spectra of highly charged krypton from a microcalorimeter detector of an electron-beam ion trap. Phys Rev E Stat Nonlin Soft Matter Phys 2001; 63:046409. [PMID: 11308958 DOI: 10.1103/physreve.63.046409] [Citation(s) in RCA: 1] [Impact Index Per Article: 0.0] [Reference Citation Analysis] [What about the content of this article? (0)] [Affiliation(s)] [Abstract] [Track Full Text] [Subscribe] [Scholar Register] [Received: 06/13/2000] [Indexed: 05/23/2023]
Abstract
Spectra of highly charged Kr ions, produced in an electron-beam ion trap (EBIT), have been recorded in a broad x-ray energy band (0.3 keV to 4 keV) with a microcalorimeter detector. Most of the spectral lines have been identified as transitions of B- to Al-like Kr. The transition energies have been determined with 0.2% uncertainty. A semi-empirical EBIT plasma model has been created to calculate a synthetic spectrum of highly charged Kr and to determine a charge state distribution of Kr ions inside the EBIT.
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Affiliation(s)
- I Kink
- National Institute of Standards and Technology, Gaithersburg, MD 20899, USA
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Takács E, Meyer ES, Gillaspy JD, Roberts JR, Chantler CT, Hudson LT, Deslattes RD, Brown CM, Laming JM, Dubau J, Inal MK. Polarization measurements on a magnetic quadrupole line in Ne-like barium. Phys Rev A 1996; 54:1342-1350. [PMID: 9913599 DOI: 10.1103/physreva.54.1342] [Citation(s) in RCA: 8] [Impact Index Per Article: 0.3] [Reference Citation Analysis] [What about the content of this article? (0)] [Track Full Text] [Subscribe] [Scholar Register] [Indexed: 05/22/2023]
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Drake JJ, Laming JM, Widing KG, Schmitt JH, Haisch B, Bowyer S. The Elemental Composition of the Corona of Procyon: Evidence for the Absence of the FIP Effect. Science 1995; 267:1470-3. [PMID: 17743544 DOI: 10.1126/science.267.5203.1470] [Citation(s) in RCA: 18] [Impact Index Per Article: 0.6] [Reference Citation Analysis] [What about the content of this article? (0)] [Abstract] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/02/2022]
Abstract
The chemical composition of the solar corona is not the same as that of the underlying photosphere. In the corona, elements with a first ionization potential (FIP) of </=10 electron volts (for example, iron, magnesium, silicon, and calcium) are overabundant relative to those with an FIP of >/=10 electron volts (for example, oxygen, neon, and sulfur) by factors of 3 to 10 with respect to the photosphere. The origin of this FIP effect is unknown. The launch of the Extreme Ultraviolet Explorer Satellite (EUVE) opened up the spectroscopic capability required to determine elemental abundances in the coronae of other stars. Spectroscopic observations of the corona of the nearby F5 IV star Procyon obtained with EUVE have yielded estimates of the relative abundances of high- and low-FIP species. The results provide evidence that Procyon, unlike the sun, does not exhibit the FIP effect. Whether the sun or Procyon is more typical of the general late-type stellar population is of fundamental interest to the physics of stellar outer atmospheres and has a bearing on the origin of cosmic rays.
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Silver JD, McClelland AF, Laming JM, Rosner SD, Chandler GC, Dietrich DD, Egan PO. Simultaneous observation of Lyman- alpha and Balmer- beta transitions in hydrogenic iron, Fe25+: A novel technique for 1s Lamb-shift measurement. Phys Rev A Gen Phys 1987; 36:1515-1518. [PMID: 9899028 DOI: 10.1103/physreva.36.1515] [Citation(s) in RCA: 3] [Impact Index Per Article: 0.1] [Reference Citation Analysis] [What about the content of this article? (0)] [Track Full Text] [Subscribe] [Scholar Register] [Indexed: 05/22/2023]
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