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Results for “LAMB SHIFT”

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At least 19 records
All sourcesNASA NTRSDOE OSTI
NASA NTRS1965

Lamb shift in

Lamb shift in lithium isotope measured by determining lifetime from photon emission and employing analog formula of Bethe and Salpeter

PHOTON DENSITY↗
NASA NTRS2001

Is the Lamb shift chemically significant?

The contribution of the Lamb shift to the atomization energies of some prototype molecules, BF3, AlF3, and GaF3, is estimated by a perturbation procedure. It is found to be in the range of 3-5% of the one-electron scalar relativistic contribution to the atomization energy. The maximum absolute value is 0.2 kcal/mol for GaF3. These sample calculations indicate that the Lamb shift is probably small enough to be neglected for energetics of molecules containing light atoms if the target accuracy is 1 kcal/mol, but for higher accuracy calculations and for molecules containing heavy elements it must be considered.

Dyall, Kenneth G.↗
NASA NTRS2017

Precise Determination of the 1s Lamb Shift in Hydrogen-Like Lead and Gold Using Microcalorimeters

Quantum electrodynamics in very strong Coulomb fields is one scope which has not yet been tested experimentally with sufficient accuracy to really determine whether the perturbative approach is valid. One sensitive test is the determination of the 1s Lamb shift in highly-charged very heavy ions. The 1s Lamb shift of hydrogen-like lead (Pb81+) and gold (Au78+) has been determined using the novel detector concept of silicon microcalorimeters for the detection of hard x-rays. The results of (260 +/- 53) eV for lead and (211 +/- 42) eV for gold are within the error bars in good agreement with theoretical predictions. To our knowledge, for hydrogen-like lead, this represents the most accurate determination of the 1s Lamb shift.

microcalorimeters for↗
NASA NTRS1967

Lamb shift in the

Energy difference between metastable levels of hydrogen-like atom determined by measuring lifetime in electrostatic field, yielding average Lamb shift in Li ion

STARK EFFECT↗
NASA NTRS1972

Measurement of the Lamb shift in the O-16/7+/ ion.

The energy difference between the 2S(sub 1/2) levels in the O-16(7+) ion has been determined by means of a Stark-quenching experiment to be 2215.6 plus or minus 7.5 GHz. The uncertainty is based on measured quantities only. This result is shown to be in agreement with the results of similar measurements made by other authors.

Lawrence, G. P.↗
NASA NTRS1986

Measurement of wavelengths and lamb shifts for inner-shell transitions in Fe XVIII-XXIV

The wavelengths of inner-shell 1s-2p transitions in the ions Fe XVIII-XXIV have been measured in solar flare spectra recorded by the Naval Research Laboratory crystal spectrometer (SOLFLEX) on the Air Force P78-1 spacecraft. The measurements are compared with previous measurements and with recently calculated wavelengths. It is found that the measured wavelengths are systematically larger than the wavelengths calculated using the Z-expansion method by up to 0.65 mA. For the more highly charged ions, these differences can be attributed to the QED contributions to the transition energies that are not included in the Z-expansion calculations.

Seely, J. F.↗
NASA NTRS1988

Theoretical energies for the n = 1 and 2 states of the helium isoelectronic sequence up to Z = 100

The unified method described previously for combining high-precision nonrelativistic variational calculations with relativistic and quantum electrodynamic corrections is applied to the 1s2 1S0, 1s2s 1S0, 1s2s 1S0, 1s2s 3S1, 1s2p 1P1, and 1s2p 3P(0.1,2) states of helium-like ions. Detailed tabulations are presented for all ions in the range Z = 2-100 and are compared with a wide range of experimental data up to (Kr-34)+. The results for (U-90)+ significantly alter the recent Lamb shift measurement of Munger and Gould (1986) from 70.4 + or - 8.3 to 71.0 + or - 8.3 eV, in comparison with a revised theoretical value of 74.3 + or - 0.4 eV. The improved agreement is due to the inclusion of higher order two-electron corrections in the present work.

Drake, G. W.↗
NASA NTRS1988

Electronic Neural Networks

Memory based on neural network models content-addressable and fault-tolerant. System includes electronic equivalent of synaptic network; particular, matrix of programmable binary switching elements over which data distributed. Switches programmed in parallel by outputs of serial-input/parallel-output shift registers. Input and output terminals of bank of high-gain nonlinear amplifiers connected in nonlinear-feedback configuration by switches and by memory-prompting shift registers.

Lambe, John↗
NASA NTRS1994

Oscillatory Dynamics of Single Bubbles and Agglomeration in a Sound Field in Microgravity

A dual-frequency acoustic levitator containing water was developed for studying bubble and drop dynamics in low gravity. It was flown on USML-1 where it was used in the Glovebox facility. High frequency (21 or 63 kHz) ultrasonic waves were modulated by low frequencies to excite shape oscillations on bubbles and oil drops ultrasonically trapped in the water. Bubble diameters were typically close to 1 cm or larger. When such large bubbles are acoustically trapped on the Earth, the acoustic radiation pressure needed to overcome buoyancy tends to shift the natural frequency for quadrupole (n = 2) oscillations above the prediction of Lamb's equation. In low gravity, a much weaker trapping force was used and measurements of n = 2 and 3 mode frequencies were closer to the ideal case. Other video observations in low gravity include: (i) the transient reappearance of a bulge where a small bubble has coalesced with a large one, (ii) observations of the dynamics of bubbles coated by oil indicating that shape oscillations can shift a coated bubble away from the oil-water interface of the coating giving a centering of the core, and (iii) the agglomeration of bubbles induced by the sound field.

Marston, Philip L.↗
NASA NTRS1994

Search for gamma-ray emission lines from SS 433: 2: 1980-1989

We have searched through the Solar Maximum Mission satellite gamma-ray spectrometer database for evidence of red and blue Doppler-shifted 1.37 MeV (24)Mg* nuclear lines. The data were obtained between 1980 and 1989 and span a total of 720 days when SS 433 was in the field of view. No evidence of Doppler-shifted line emission was found in any of our spectra. The range of 3 sigma upper limits for individual 9 day integration periods was (0.8-2.4) x 10(exp -3) photons/sq cm/s for the blue beam, encompassing the approximately 1.5 MeV feature reported by Lamb et al., and (0.2-2.1) x 10(exp -3) photons/sq cm/s for the red beam, encompassing the reported approximately 1.2 MeV feature. The average 3 sigma upper limit in each beam for shifted 1.37 MeV was 1.5 x 10(exp -3) photons/sq cm/s for single 9 day integration. The 3 sigma upper limits over 56 9 day integration intervals (504 days) for the red beam and 69 intervals (621 days) for the blue beam are 1.2 x 10(exp -4) photons/sq cm/s. The new limits can be reconciled with the HEAO 3 results only if SS 433 emits gamma rays at or above the SMM sensitivity limit on rare occasions due to variable physical conditions in the system.

Geldzahler, B. J.↗
NASA NTRS1983

Gamma-ray line emission from SS433

Preliminary evidence for gamma ray line emission from the region of SS433 using the spectrometer aboard the HEAO 3 satellite is reported. One of the line features, located at an energy of 1.5 MeV, has a statistical significance of about six sigmas during a particular 18-day interval. Another feature appears near 1.2 MeV. Both features exhibit fractional linewidths of about one percent. The intensity of the 1.5 MeV feature is variable by a factor of about three on a time scale of days, and the 1.2 MeV feature is similarly variable. The combined power of the lines is about 2 x 10 to the 27th ergs/s, assuming isotropic emission. The observed energies can be interpreted in terms of a kinematic model published elsewhere as blue and red-shifted components of the 1.369 MeV line from a nuclear transition of Mg-24 from its first excited state to its ground state.

Lamb, R. C.↗