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At least 91 records · Page 5
All sourcesNASA NTRSDOE OSTI
NASA NTRS2013

Direct Measurement of Dust Attenuation in z approx. 1.5 Star-Forming Galaxies from 3D-HST: Implications for Dust Geometry and Star Formation Rates

The nature of dust in distant galaxies is not well understood, and until recently few direct dust measurements have been possible. We investigate dust in distant star-forming galaxies using near-infrared grism spectra of the 3D-HST survey combined with archival multi-wavelength photometry. These data allow us to make a direct comparison between dust towards star-forming regions (measured using Balmer decrements) and the integrated dust properties (derived by comparing spectral energy distributions [SEDs] with stellar population and dust models) for a statistically significant sample of distant galaxies. We select a sample of 163 galaxies between 1.36< or = z< or = 1.5 with H(alpha) SNR > or = 5 and measure Balmer decrements from stacked spectra. First, we stack spectra in bins of integrated stellar dust attenuation, and find that there is extra dust extinction towards star-forming regions (AV,HII is 1.81 times the integrated AV, star), though slightly lower than found for low-redshift starburst galaxies. Next, we stack spectra in bins of specific star formation rate (log sSFR), star formation rate (log SFR), and stellar mass (logM∗). We find that on average AV,HII increases with SFR and mass, but decreases with increasing sSFR. The amount of extra extinction also decreases with increasing sSFR and decreasing stellar mass. Our results are consistent with the two-phase dust model - in which galaxies contain both a diffuse and a stellar birth cloud dust component - as the extra extinction will increase once older stars outside the star-forming regions become more dominant. Finally, using our Balmer decrements we derive dust-corrected H(alpha) SFRs, and find evidence that SED fitting produces incorrect SFRs if very rapidly declining SFHs are included in the explored parameter space. Subject headings: dust, extinction- galaxies: evolution- galaxies: high-redshift

Direct↗
DOE OSTI2020

Materials Data on Na26(Ge3Au8)5 by Materials Project

Na26(Au8Ge3)5 is alpha-derived structured and crystallizes in the orthorhombic Imm2 space group. The structure is three-dimensional. there are eleven inequivalent Na sites. In the first Na site, Na is bonded in a 12-coordinate geometry to three Na, nine Au, and three Ge atoms. There are a spread of Na–Na bond distances ranging from 3.06–3.56 Å. There are a spread of Na–Au bond distances ranging from 3.10–3.36 Å. There are a spread of Na–Ge bond distances ranging from 3.27–3.35 Å. In the second Na site, Na is bonded in a 12-coordinate geometry to two Na, nine Au, and three Ge atoms. The Na–Na bond length is 3.46 Å. There are a spread of Na–Au bond distances ranging from 3.09–3.38 Å. There are a spread of Na–Ge bond distances ranging from 3.27–3.38 Å. In the third Na site, Na is bonded in a 10-coordinate geometry to two equivalent Na, ten Au, and three Ge atoms. Both Na–Na bond lengths are 3.06 Å. There are a spread of Na–Au bond distances ranging from 3.10–3.21 Å. There are a spread of Na–Ge bond distances ranging from 3.19–3.27 Å. In the fourth Na site, Na is bonded in a 4-coordinate geometry to nine Au and four Ge atoms. There are a spread of Na–Au bond distances ranging from 3.08–3.27 Å. There are two shorter (3.11 Å) and two longer (3.27 Å) Na–Ge bond lengths. In the fifth Na site, Na is bonded in a 11-coordinate geometry to two equivalent Na, eight Au, and five Ge atoms. Both Na–Na bond lengths are 3.16 Å. There are four shorter (3.10 Å) and four longer (3.17 Å) Na–Au bond lengths. There are a spread of Na–Ge bond distances ranging from 3.10–3.18 Å. In the sixth Na site, Na is bonded in a 11-coordinate geometry to two Na, ten Au, and three Ge atoms. Both Na–Na bond lengths are 3.00 Å. There are a spread of Na–Au bond distances ranging from 3.10–3.33 Å. There are one shorter (3.18 Å) and two longer (3.41 Å) Na–Ge bond lengths. In the seventh Na site, Na is bonded in a 5-coordinate geometry to four Na, nine Au, and three Ge atoms. The Na–Na bond length is 3.31 Å. There are a spread of Na–Au bond distances ranging from 3.13–3.53 Å. There are one shorter (3.26 Å) and two longer (3.35 Å) Na–Ge bond lengths. In the eighth Na site, Na is bonded in a 5-coordinate geometry to one Na, nine Au, and two equivalent Ge atoms. There are a spread of Na–Au bond distances ranging from 3.13–3.50 Å. Both Na–Ge bond lengths are 3.41 Å. In the ninth Na site, Na is bonded in a 5-coordinate geometry to four Na, eight Au, and four Ge atoms. The Na–Na bond length is 3.49 Å. There are a spread of Na–Au bond distances ranging from 3.10–3.49 Å. There are a spread of Na–Ge bond distances ranging from 3.25–3.58 Å. In the tenth Na site, Na is bonded in a 5-coordinate geometry to one Na, seven Au, and three Ge atoms. There are a spread of Na–Au bond distances ranging from 3.08–3.28 Å. There are one shorter (3.27 Å) and two longer (3.37 Å) Na–Ge bond lengths. In the eleventh Na site, Na is bonded in a 7-coordinate geometry to seven Au and three Ge atoms. There are a spread of Na–Au bond distances ranging from 3.09–3.25 Å. There are one shorter (3.36 Å) and two longer (3.37 Å) Na–Ge bond lengths. There are fourteen inequivalent Au sites. In the first Au site, Au is bonded in a 12-coordinate geometry to five Na, one Au, and one Ge atom. The Au–Au bond length is 2.87 Å. The Au–Ge bond length is 2.55 Å. In the second Au site, Au is bonded in a 12-coordinate geometry to five Na, one Au, and one Ge atom. The Au–Au bond length is 2.88 Å. The Au–Ge bond length is 2.56 Å. In the third Au site, Au is bonded in a 1-coordinate geometry to five Na, one Au, and one Ge atom. The Au–Au bond length is 2.88 Å. The Au–Ge bond length is 2.53 Å. In the fourth Au site, Au is bonded in a 12-coordinate geometry to five Na, one Au, and one Ge atom. The Au–Au bond length is 2.90 Å. The Au–Ge bond length is 2.55 Å. In the fifth Au site, Au is bonded in a 1-coordinate geometry to five Na, one Au, and one Ge atom. The Au–Au bond length is 2.92 Å. The Au–Ge bond length is 2.55 Å. In the sixth Au site, Au is bonded to twelve Au atoms to form AuAu12 cuboctahedra that share corners with two equivalent GeNa6Au6 cuboctahedra. In the seventh Au site, Au is bonded in a 12-coordinate geometry to six Na, three Au, and three Ge atoms. There are one shorter (2.82 Å) and two longer (2.89 Å) Au–Au bond lengths. There are a spread of Au–Ge bond distances ranging from 2.61–2.96 Å. In the eighth Au site, Au is bonded in a 12-coordinate geometry to six Na, four Au, and two Ge atoms. There are a spread of Au–Au bond distances ranging from 2.82–3.09 Å. There are one shorter (2.59 Å) and one longer (2.82 Å) Au–Ge bond lengths. In the ninth Au site, Au is bonded in a 12-coordinate geometry to six Na, three Au, and three Ge atoms. There are one shorter (2.90 Å) and one longer (2.91 Å) Au–Au bond lengths. There are a spread of Au–Ge bond distances ranging from 2.59–2.90 Å. In the tenth Au site, Au is bonded in a 12-coordinate geometry to six Na, three Au, and three Ge atoms. There are one shorter (2.91 Å) and one longer (2.95 Å) Au–Au bond lengths. There are a spread of Au–Ge bond distances ranging from 2.60–2.88 Å. In the eleventh Au site, Au is bonded in a 12-coordinate geometry to six Na, four Au, and two Ge atoms. There are one shorter (2.90 Å) and one longer (3.02 Å) Au–Au bond lengths. There are one shorter (2.55 Å) and one longer (2.68 Å) Au–Ge bond lengths. In the twelfth Au site, Au is bonded in a 12-coordinate geometry to six Na, four Au, and two Ge atoms. The Au–Au bond length is 3.08 Å. There are one shorter (2.56 Å) and one longer (2.64 Å) Au–Ge bond lengths. In the thirteenth Au site, Au is bonded in a 3-coordinate geometry to seven Na, five Au, and two Ge atoms. The Au–Au bond length is 2.75 Å. There are one shorter (3.16 Å) and one longer (3.21 Å) Au–Ge bond lengths. In the fourteenth Au site, Au is bonded in a 1-coordinate geometry to seven Na, four equivalent Au, and one Ge atom. The Au–Ge bond length is 2.49 Å. There are seven inequivalent Ge sites. In the first Ge site, Ge is bonded in a 11-coordinate geometry to six Na and five Au atoms. In the second Ge site, Ge is bonded in a 12-coordinate geometry to five Na and five Au atoms. In the third Ge site, Ge is bonded in a 11-coordinate geometry to six Na and five Au atoms. In the fourth Ge site, Ge is bonded in a 12-coordinate geometry to six Na and six Au atoms. In the fifth Ge site, Ge is bonded to six Na and six Au atoms to form distorted GeNa6Au6 cuboctahedra that share a cornercorner with one AuAu12 cuboctahedra and an edgeedge with one GeNa6Au6 cuboctahedra. In the sixth Ge site, Ge is bonded in a 1-coordinate geometry to seven Na and five Au atoms. In the seventh Ge site, Ge is bonded in a 12-coordinate geometry to three Na, four Au, and one Ge atom. The Ge–Ge bond length is 2.70 Å.

36 MATERIALS SCIENCE↗
DOE OSTI2019

Materials Data on Ti4(FeSb)5 by Materials Project

Ti4(FeSb)5 is alpha-derived structured and crystallizes in the trigonal R3m space group. The structure is three-dimensional. there are four inequivalent Ti sites. In the first Ti site, Ti is bonded to three equivalent Fe and three equivalent Sb atoms to form distorted TiFe3Sb3 octahedra that share corners with six equivalent FeSb6 octahedra, edges with six equivalent TiFe3Sb3 octahedra, and a faceface with one FeSb6 octahedra. The corner-sharing octahedral tilt angles are 41°. All Ti–Fe bond lengths are 2.49 Å. All Ti–Sb bond lengths are 2.91 Å. In the second Ti site, Ti is bonded in a 6-coordinate geometry to three equivalent Fe and three equivalent Sb atoms. All Ti–Fe bond lengths are 2.49 Å. All Ti–Sb bond lengths are 2.92 Å. In the third Ti site, Ti is bonded in a 6-coordinate geometry to three equivalent Fe and three equivalent Sb atoms. All Ti–Fe bond lengths are 2.51 Å. All Ti–Sb bond lengths are 2.92 Å. In the fourth Ti site, Ti is bonded to three equivalent Fe and three equivalent Sb atoms to form distorted edge-sharing TiFe3Sb3 octahedra. All Ti–Fe bond lengths are 2.49 Å. All Ti–Sb bond lengths are 2.89 Å. There are five inequivalent Fe sites. In the first Fe site, Fe is bonded to six Sb atoms to form distorted FeSb6 octahedra that share corners with six equivalent TiFe3Sb3 octahedra, edges with six equivalent FeSb6 octahedra, and a faceface with one TiFe3Sb3 octahedra. The corner-sharing octahedral tilt angles are 41°. There are three shorter (2.60 Å) and three longer (2.67 Å) Fe–Sb bond lengths. In the second Fe site, Fe is bonded in a 6-coordinate geometry to three equivalent Ti and three equivalent Sb atoms. All Fe–Sb bond lengths are 2.61 Å. In the third Fe site, Fe is bonded to three equivalent Ti and three equivalent Sb atoms to form distorted edge-sharing FeTi3Sb3 pentagonal pyramids. All Fe–Sb bond lengths are 2.60 Å. In the fourth Fe site, Fe is bonded in a 6-coordinate geometry to three equivalent Ti and three equivalent Sb atoms. All Fe–Sb bond lengths are 2.61 Å. In the fifth Fe site, Fe is bonded in a 6-coordinate geometry to three equivalent Ti and three equivalent Sb atoms. All Fe–Sb bond lengths are 2.68 Å. There are five inequivalent Sb sites. In the first Sb site, Sb is bonded in a 6-coordinate geometry to six Fe atoms. In the second Sb site, Sb is bonded in a 6-coordinate geometry to three equivalent Ti and three equivalent Fe atoms. In the third Sb site, Sb is bonded in a 6-coordinate geometry to three equivalent Ti and three equivalent Fe atoms. In the fourth Sb site, Sb is bonded in a 6-coordinate geometry to three equivalent Ti and three equivalent Fe atoms. In the fifth Sb site, Sb is bonded in a 6-coordinate geometry to three equivalent Ti and three equivalent Fe atoms.

36 MATERIALS SCIENCE↗
DOE OSTI2023

Systematic evaluation of fast neutron sensing with Cesium Hafnium Chloride

Cesium Hafnium Chloride (CHC) is a promising new scintillator for dual mode sensing of both neutrons and gamma-rays. The high chlorine content allows for both 35 Cl(n,p) 35 S and 35 Cl(n,α) 32 P reaction channels leading to reliable detection of fast neutrons. By utilizing pulse shape discrimination (PSD), these neutron interactions may be reliably separated from gamma-ray signals with a high figure-of-merit (FOM) after optimization of the PSD algorithm. Here, in this study, the PSD algorithm settings for CHC were systematically investigated using a bare 252 Cf and a lead shielded plutonium beryllium neutron source. It was found that the PSD algorithm settings affects both the FOM and the neutron detection efficiency, but a FOM as high as 4.5 for alpha particles was observed in one data processing scenario. Further, an intrinsic 5 parts per million alpha emitting contamination was observed in the sample, which we attribute to natural uranium.

46 INSTRUMENTATION RELATED TO NUCLEAR SCIENCE AND ↗
DOE OSTI2018

Semiconducting lithium indium diselenide: Charge-carrier properties and the impacts of high flux thermal neutron irradiation

Here, we report on the charge carrier properties of several lithium indium diselenide (LISe) semiconductors. It was found that the charge collection efficiency of LISe was improved after high flux thermal neutron irradiation including the presence of a typically unobservable alpha peak from hole-only collection. Charge carrier trap energies of the irradiated sample were measured using photo-induced current transient spectroscopy. Compared to previous studies of this material, no significant differences in trap energies were observed. Through trap-filled limited voltage measurements, neutron irradiation was found to increase the density of trap states within the bulk of the semiconductor, which created a polarization effect under alpha exposure but not neutron exposure. Further, the charge collection efficiency of the irradiated sample was higher (14–15 fC) than that of alpha particles (3–5 fC), indicating that an increase in hole signal contribution resulted from the neutron irradiation. Finally, it was observed that significant charge loss takes place near the point of generation, producing a significant scintillation response and artificially inflating the W-value of all semiconducting LISe crystals.

36 MATERIALS SCIENCE↗
DOE OSTI2015

RCS2 J232727.6-020437: An efficient cosmic telescope at z = 0.6986

We present a detailed gravitational lens model of the galaxy cluster RCS2 J232727.6-020437. Due to cosmological dimming of cluster members and intra-cluster light, its high redshift (z = 0.6986) makes it ideal for studying high-redshift background galaxies. Using new Advanced Camera for Surveys and WFC3/IR Hubble Space Telescope data, we identify 16 new multiple images belonging to 6 distinct source galaxies. From Multi-object Spectrometer for Infrared Exploration (MOSFIRE) follow-up, we identify a strong emission line in the spectrum of one multiple image, measuring the redshift of that system to z = 2.083. With a highly magnified (μ ≳ 3) source plane area of ∼0.9 arcmin{sup 2} at z = 7, RCS2 J232727.6-020437 has a lensing efficiency comparable to the Hubble Frontier Fields clusters. We discover four highly magnified z ∼ 7 candidate Lyman-break galaxies behind the cluster. Correcting for magnification, we find that all four galaxies are fainter than 0.5L{sub ⋆}. One candidate is detected at >10σ in both Spitzer/IRAC [3.6] and [4.5] channels. A spectroscopic follow-up with MOSFIRE does not result in the detection of the Lyα emission line from any of the four candidates. From the MOSFIRE spectra, we place median upper limits on the Lyα flux of (3−11)×10{sup −19} erg s{sup −1} cm{sup −2} (5σ).

79 ASTRONOMY AND ASTROPHYSICS↗
DOE OSTI2015

Timing gamma-ray pulsars with the Fermi large area telescope: Timing noise and astrometry

We have constructed timing solutions for 81 γ-ray pulsars covering more than five years of Fermi data. The sample includes 37 radio-quiet or radio-faint pulsars which cannot be timed with other telescopes. These timing solutions and the corresponding pulse times of arrival are prerequisites for further study, e.g., phase-resolved spectroscopy or searches for mode switches. Many γ-ray pulsars are strongly affected by timing noise (TN), and we present a new method for characterizing the noise process and mitigating its effects on other facets of the timing model. We present an analysis of TN over the population using a new metric for characterizing its strength and spectral shape, namely, its time-domain correlation. The dependence of the strength on ν and ν-dot is in good agreement with previous studies. We find that noise process power spectra S(f) for unrecycled pulsars are steep, with strong correlations over our entire data set and spectral indices S(f)∝f{sup −α} of α ∼ 5–9. One possible explanation for these results is the occurrence of unmodeled, episodic “microglitches.” Finally, we show that our treatment of TN results in robust parameter estimation, and in particular we measure a precise timing position for each pulsar. We extensively validate our results with multi-wavelength astrometry, and using our updated position, we firmly identify the X-ray counterpart of PSR J1418−6058.

79 ASTRONOMY AND ASTROPHYSICS↗
DOE OSTI2021

Atomic forces from Dirac-Kohn-Sham equations: Implementation in flexible (APW+lo/LAPW)+LO basis set

The atomic forces formulation based on the Dirac-Kohn-Sham equation and the flexible (APW+lo/LAPW)+LO basis set is presented here. The formulation was implemented in the code FlapwMBPT and allows a user to easily switch between different basis functions of the augmentation type (APW or LAPW) and between different kind of local orbitals. Similar to the work (Phys.Rev.B 91 (2015) 035105), the implementation takes into account small discontinuities of the wave functions, density, and potential at the muffin-tin sphere boundaries. Applications to the materials with strong relativistic effects, such as $\alpha$-Uranium, PuCoGa$_{5}$, and FePt, demonstrate robustness of the method. The comparison of the calculated forces with the ones obtained by numerical differentiation of free energy shows close agreement with deviations about 0.1% or less.

75 CONDENSED MATTER PHYSICS, SUPERCONDUCTIVITY AND↗
DOE OSTI2013

Crystallization and preliminary X-ray analysis of a phosphopentomutase from Bacillus cereus

Phosphopentomutases (PPMs) interconvert D-ribose 5-phosphate and {alpha}-D-ribose 1-phosphate to link glucose and nucleotide metabolism. PPM from Bacillus cereus was overexpressed in Escherichia coli, purified to homogeneity and crystallized. Bacterial PPMs are predicted to contain a di-metal reaction center, but the catalytically relevant metal has not previously been identified. Sparse-matrix crystallization screening was performed in the presence or absence of 50 mM MnCl{sub 2}. This strategy resulted in the formation of two crystal forms from two chemically distinct conditions. The crystals that formed with 50 mM MnCl{sub 2} were more easily manipulated and diffracted to higher resolution. These results suggest that even if the catalytically relevant metal is not known, the crystallization of putative metalloproteins may still benefit from supplementation of the crystallization screens with potential catalytic metals.

59 BASIC BIOLOGICAL SCIENCES↗
NASA NTRS1973

Analysis and synthesis of coronal and interplanetary energetic particle, plasma, and magnetic field observations over three solar rotations.

In a previous paper (Krimigis et al., 1971), simultaneous observations in 1967 of solar particle events at low (less than 1 MeV) energies were presented. In the present paper, the full complement of simultaneous plasma, magnetic field, and energetic particle data is combined, and a complete analysis is made of all the events discussed in the original paper. The essential concept of 'collimated convection' is introduced, whereby the bulk velocity along the field lines of low-energy solar particles is independent of solar local plasma velocity, and the particles are strongly collimated along the field line with no transverse velocity component other than that of the field line itself. Collimated convection effects are shown to exist in small-scale convection and large-scale evolution of particle fluxes; the particle fluxes are, in turn, used to delineate the small-scale and large-scale evolution of the interplanetary magnetic field. Use of collimated convection is made in demonstrating a technique whereby energetic particle intensity profiles in the interplanetary medium can be related to equatorial high coronal magnetic field structures, by using the instantaneous solar wind velocity. This technique is applied in mapping particle intensities from Mariner 5 onto H alpha synoptic charts of chromospheric magnetic field structures for Carrington rotations 1523 to 1525.

Roelof, E. C.↗
NASA NTRS1980

The electric potential of particles in interstellar space released from a nuclear waste payload

Mechanisms for charging a grain in the interplanetary medium include: (1) capture of solar wind electrons; (2) capture of solar wind protons; (3) ejection of electrons through the photoelectric effect due to the solar radiation; (4) escape of beta particles from beta emitters in the grain; and (5) escape of alpha particles from alpha emitters in the grain. The potentials on both nonradioactive and radioactive grains are considered with relation to particle size and time, and the distance from the Sun. Numerical results are presented where the waste mix is assumed to be PW-4b.

Williams, A. C.↗
NASA NTRS1986

A three-dimensional model of the nucleus of Comet Halley

The nucleus of comet Halley was observed by the Halley Multicolor Camera (HMC) during the last minutes of the flyby sequence before reaching the point of closest approach. The phase angle change during the observational period was less than 17 deg, so HMC data can only define a two-dimensional contour of the nucleus at a certain time. The overall geometry during the HMC observations is outlined and the findings are related to information available from other sources at different times. The nucleus of the comet is described as a triaxial ellipsoid with major axes of 16, 10, and 9 km. The rotation axis is directed towards delta 1950 = -(40 + or - 5) deg and alpha 1950 = (50 + or - 10) deg. The rotation with a period of P = (54 + or - 1) is in a prograde sense with respect to the orbital motion.

Wilhelm, K.↗
NASA NTRS1990

Reactions of SiC with H2/H2O/Ar mixtures at 1300 C

Thermochemical modeling anticipates the existence of three reaction regions for the case of a sintered alpha-SiC with 5 percent H2/H2O/Ar at 1300 C, depending on the initial water vapor or, equivalently, oxygen, content of the gas stream. While a high oxygen content leads to SiC-protecting SiO2 surface film formation and limits consumption of the SiC through passive oxidation, intermediate oxygen contents lead to SiO and CO formation and rapid SiC consumption. In this intermediate region, reaction rates appear to be controlled by H2O gas-phase transport to the sample; reacted microstructures exhibit extensive grain-boundary attack in this region. Very low oxygen content is predicted to selectively remove carbon, with free silicon formation.

Jacobson, Nathan S.↗
NASA NTRS1992

Nonlinear stability and control study of highly maneuverable high performance aircraft, phase 2

This research should lead to the development of new nonlinear methodologies for the adaptive control and stability analysis of high angle-of-attack aircraft such as the F18 (HARV). The emphasis has been on nonlinear adaptive control, but associated model development, system identification, stability analysis and simulation is performed in some detail as well. Various models under investigation for different purposes are summarized in tabular form. Models and simulation for the longitudinal dynamics have been developed for all types except the nonlinear ordinary differential equation model. Briefly, studies completed indicate that nonlinear adaptive control can outperform linear adaptive control for rapid maneuvers with large changes in alpha. The transient responses are compared where the desired alpha varies from 5 degrees to 60 degrees to 30 degrees and back to 5 degrees in all about 16 sec. Here, the horizontal stabilator is the only control used with an assumed first-order linear actuator with a 1/30 sec time constant.

Mohler, R. R.↗
NASA NTRS1961

Fast Interplanetary Missions with Low-Thrust Propulsion Systems

A simple family of indirect-transfer trajectories between circular orbits is used to evaluate the mass ratio required to complete round-trip interplanetary missions using low-thrust propulsion systems. These trajectories, although not optimum, yielded very substantial reductions in total round-trip time for Mars missions with moderate increases in initial weight. For a powerplant specific weight a of 10 pounds per kilowatt of jet power, trip times were reduced from 1200 to 600 days, for a typical manned mission, with an initial weight increase of a factor of two. Comparison with a nuclear rocket with 1000-second specific impulse indicated that the electric-propulsion system required less initial weight for trip times as low as 550 days with alpha equal to 10 and as low as 400 days with alpha equal to 5 pounds per kilowatt. Further weight reductions would be expected with more nearly optimum trajectories.

Moeckel, W. E.↗
NASA NTRS2001

FUSE Observations of Galactic and LMC Novae in Outburst

This document is a collection of five abstracts from papers written on the 'FUSE Observations of Galactic and LMC Novae in Outburst'. The titles are the following: (1) Analyzing FUSE Observations of Galactic and LMC Novae; (2) Detailed NLTE Model Atmospheres for Novae during Outburst: Modeling Optical and Ultraviolet Observations for Nova LMC 1988; (3) Numerical Solution of the Expanding Stellar Atmosphere Problem; (4) A Non-LTE Line-Blanketed Expanding Atmosphere Model for A-supergiant Alpha Cygni; and (5) Non-LTE Model Atmosphere Analysis of the Early Ultraviolet Spectra of Nova Andromedae 1986. A list of journal publications is also included.

Huschildt, P. H.↗