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Phillips, E.

Publications and source records attributed to Phillips, E..

9 records
All sourcesNASA NTRSDOE OSTI
NASA NTRS1984

Line width of the solar EUV He I resonance emissions at 584 and 537 A

Instrumentation was carried aloft on a Black Brant rocket in August 1982 to gather spectrometry on the solar He I resonance lines. The payload consisted of a He spectrometer which furnished 11 readings at FWHM of close to 97 and 132 mA for the 584 and 537 a lines, respectively. The results indicated a variation of the solar line width that was inversely correlated with solar activity and with the solar EUV flux. Further studies of the 522 A line are recommended to detect any unidentified first order solar emissions close to or within the absorption profile of the 537 A line that contributed to the observed line width.

Ogawa, H. S.↗
NASA NTRS1984

Absolute measurement of the extreme UV solar flux

A windowless rare-gas ionization chamber has been developed to measure the absolute value of the solar extreme UV flux in the 50-575-A region. Successful results were obtained on a solar-pointing sounding rocket. The ionization chamber, operated in total absorption, is an inherently stable absolute detector of ionizing UV radiation and was designed to be independent of effects from secondary ionization and gas effusion. The net error of the measurement is + or - 7.3 percent, which is primarily due to residual outgassing in the instrument, other errors such as multiple ionization, photoelectron collection, and extrapolation to the zero atmospheric optical depth being small in comparison. For the day of the flight, Aug. 10, 1982, the solar irradiance (50-575 A), normalized to unit solar distance, was found to be 5.71 + or - 0.42 x 10 to the 10th photons per sq cm sec.

Carlson, R. W.↗
NASA NTRS1982

Measurement of the profile of solar He I resonance lines

The analysis of data obtained by a rocket-borne helium-filled spectrometer employing a curve-of-growth technique in 1977 and 1980 is used in an investigation of the 584-A helium resonance line from the full solar disk. Between 6.5 and 13% of the Gaussian core area was found to be missing through self-reversal. Line widths from 1980 and 1977 were 101 + or - 10 mA and 128 + or - 20 mA full width at half maximum, respectively. No consistent relationship is found between the measured widths and solar activity.

Phillips, E.↗
NASA NTRS1979

Lyman-alpha and Balmer-series fluorescence from hydrogen photofragments of H2O vapor

Production cross sections associated with the atomic hydrogen Lyman-alpha and Balmer-series (3-9 to 2) fluorescence observed in H2O photodissociation are measured, and maximum fluorescence production cross sections for the two series are reported. Repulsive potential energy curves corresponding to the respective pseudodiatomic OH-H(n) molecule are constructed according to the Franck-Condon principle, and the efficiencies for converting H(2S) to H(2P) by H2 collisions and by H2O collisions are estimated. The data are considered with reference to cometary photochemistry.

Wu, C. Y. R.↗
NASA NTRS1978

Atomic carbon emission from photodissociation of CO2

Atomic carbon fluorescence, C I 1561, 1657, and 1931 A, has been observed from photodissociation of CO2, and the production cross sections have been measured. A line emission source provided the primary photons at wavelengths from threshold to 420 A. The present results suggest that the excited carbon atoms are produced by total dissociation of CO2 into three atoms. The cross sections for producing the O I 1304-A fluorescence through photodissociation of CO2 are found to be less than 0.01 Mb in the wavelength region from 420 to 835 A. The present data have implications with respect to photochemical processes in the atmospheres of Mars and Venus.

Wu, C. Y. R.↗
NASA NTRS1977

Dispersed fluorescence observations of the CO/A 1Pi to X 1Sigma+/ transitions from photodissociation of CO2

The spectra of vacuum ultraviolet (vuv) fluorescence resulting from the excitation of CO2 by photons from an intense line emission source at 15 wavelengths in the range 449-955 A were obtained. The vibrational population distributions for the v = 0, 1, and 2 levels of the CO(A 1Pi) fragments were obtained at several incident photon wavelengths from 700 to 923 A. At incident photon wavelengths of 901 and 923, the relative intensities of the CO(A to X) bands were determined, permitting examination of the variation of the electronic transition moment with the r centroid.

Phillips, E.↗
NASA NTRS1976

CO/d-3 Delta sub i to X-1 Sigma +/ fluorescence from photodissociation of CO2 by 923 A photons

Measurements of vacuum ultraviolet fluorescence from the photodissociation of CO2 by photons from a N IV line emission source at a wavelength of 923 A have revealed a second CO band system in addition to the expected emission bands. Spectra with time resolution were obtained and the fluorescence lifetime and the dependence of fluorescence intensity on CO2 pressure were measured. An analysis of this data has permitted the second band system to be identified as originating from CO(d-3 Delta sub i to X-1 Sigma +) transitions.

Phillips, E.↗