Engineering topics

Stiening, R. F.

Publications and source records attributed to Stiening, R. F..

9 records

NASA NTRS1995

The pulsation index, effective temperature, and thickness of the hydrogen layer in the pulsating DA white dwarf G117-B15A

We have measured the amplitude of the 215 s pulsation of the pulsating DA white dwarf, or ZZ Ceti star, G117-B15A in six passbands with effective wavelengths from 1570 to 6730 A. We find that the index of the pulsation is l = 1 with a high degree of confidence, the first unambiguous determination of l for a pulsation of a ZZ Ceti star. We also find that log g and T(sub eff) are tightly correlated for model atmospheres that fit the data, such that at log g = 7.5 the temperature is 11,750 K and at log g = 8.0 the temperature is 12,375 K. Adopting log g = 7.97 +/- 0.06 from published observations of the optical spectrum of G117-B15A, the correlation yields T(sub eff) = 12,375 +/- 125 K. This temperature is free of flux calibration errors and should be substantially more reliable than temperatures derived for IUE spectra. Since G117-B15A is thought to lie close to the blue edge of the ZZ Ceti instability strip, this low temperature also implies a low temperature for the blue edge. Using pulsation models calculated by Fontaine et al. (1992) and Bradley (1994), we find that the mass of the hydrogen layer in G117-B15A lies between 1.0 x 10(exp -6) solar mass (for k = 1) and 8 x 10(exp -5) solar mass (for k = 2). This range of masses is (barely) consistent with the masses predicted by recent models for the ejection of planetary nebulae, (8-13) x 10(exp -5) solar mass. The mass is too large to be consistent with models invoking thin hydrogen layers to explain the spectral evolution of white dwarfs.

Robinson, E. L.↗

NASA NTRS1982

Observations of the rapid oscillations of EM Cygni

High-speed two-color photometric observations have been made of the dwarf nova EM Cyg and rapid coherent oscillations with periods between 14.6 and 16.5 sec have been found. The minimum period is less than the period of a Keplerian orbit at the surface of a carbon white dwarf. The color temperature of the oscillating component is much higher than that of the constant component of the luminosity. These results suggest that the source of the oscillations is the white dwarf or the inner part of the accretion disk.

Stiening, R. F.↗

NASA NTRS1981

The color of the fast oscillations of AH Herculis

The color of the fast coherent oscillations of AH Herculis is measured by comparing simultaneous records of the photon arrival rate in two wavelength bands, 355 + or - 30 nm and 795 + or - 80 nm. It is found that the color temperature of the coherent oscillation detected in these two wavelength bands is between 28,000 and 73,000 K. The color temperature of the nonoscillating luminosity is much lower. The arrival times of photons in these two bands have also been correlated, and it is found that the time interval between the long-wavelength coherent signal and the ultraviolet coherent signal is 0.26 + or - 0.5 sec. These results suggest that it is the surface of the white dwarf or the hot inner portion of the accretion disk which is emitting the coherent signal. The oscillations become detectably incoherent at the approach to minimum light after the outburst, as would be expected if the oscillating medium becomes more dissipative as it cools, or if there were increased modulation by clouds of obscuring material.

Hildebrand, R. H.↗

NASA NTRS1981

Observations of fast oscillations in SS Cygni

High-speed photometric observations of the dwarf nova SS Cygni have been made using an ultraviolet and blue sensitive photomultiplier. Rapid oscillations were detected over an interval of 7 days. The period of the oscillations passed through a minimum of 7.29 s, the shortest period yet observed in a dwarf nova. The signal was spread in frequency by an amount larger than required by the slow evolution of the period. The data are considered from the viewpoint of several models.

Hildebrand, R. H.↗

NASA NTRS1980

The evolution of rapid oscillations in an outburst of a dwarf nova

High-speed photometric observations of the dwarf nova AH Her on nine consecutive days during an outburst have been made, and rapid coherent oscillations on every day except two near maximum light have been detected. The period, amplitude, and luminosity for each day is presented and the progression of the periods is discussed.

Hildebrand, R. H.↗

NASA NTRS1979

Changes in the rapid oscillations of AH Herculis during an outburst

High-speed photometric observations of the dwarf nova AH Her were made during the period June 5-12, 1978 at the NASA/University of Arizona 152-cm telescope of the Mount Lemmon Observatory. Observations have shown rapid oscillations beginning after the maximum of an outburst and remaining detectable for five consecutive days. Measurements of the period and amplitude of the oscillations and the intensity of the outburst are presented for each day.

Stiening, R. F.↗

NASA NTRS1978

Submillimeter observations of the galactic center

A 15 by 15 arcmin region surrounding Sgr A has been mapped at a mean wavelength of 540 microns. The principal feature is a ridge about 10 arcmin long running parallel to the galactic equator and approximately centered on Sgr A but with no peak at that point. The ridge coincides with the 25- and 55-km/s clouds seen in molecular line observations. The mass of the clouds is estimated, and their positions with respect to the galactic center are discussed.

Hildebrand, R. H.↗

NASA NTRS1977

Submillimeter photometry of extragalactic objects

Submillimeter flux densities from five extragalactic objects have been measured, and upper limits set for three others. The galaxies NGC 253 and NGC 1068 have submillimeter spectra steeper than the cube of frequency. Of several source mechanisms considered for the far-infrared and submillimeter flux from NGC 1068, only thermal emission from dust at about 30 K is consistent with the data. The source of that flux, if thermal, must have a diameter of at least 5 arcsec. If one assumes radiation from dust, the masses of interstellar material derived for the central 80-arcsec diameter regions of NGC 253, NGC 1068, and NGC 5236 are, respectively, 800 million, 10 billion, and 3 billion solar masses. Measurements of submillimeter flux densities for 3C 273, BL Lac, NGC 1275, and NGC 5128 show no excess above values obtained by interpolation between radio and mid-infrared data.

Hildebrand, R. H.↗

NASA NTRS1977

Far-infrared and submillimeter observations of the planets

Broadband observations in several passbands between 30 and 500 microns of Mercury, Venus, Mars, Jupiter, Saturn, and Uranus are presented. The best agreement between the data and various thermal models of Mars, Jupiter, and Uranus is obtained with a slightly cooler absolute temperature scale than that previously adopted by Armstrong et al. (1972). The effective temperature of Uranus is 58 + or - 2 K, which is in agreement with its solar equilibrium temperature. The existence of an internal energy source for Saturn has been reconfirmed; its output must lie within the range of 0.9 to 3.2 times the absorbed solar flux. A depression exists in the spectra of Jupiter, Saturn, and Uranus between 80 and 300 microns, which may be a result of NH3 opacity.

Loewenstein, R. F.↗