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At least 397 records · Page 22
All sourcesNASA NTRSDOE OSTI
NASA NTRS1979

Degenerate dwarfs in future hard X-ray experiments

The hard X-ray characteristics of weak sources (dwarf novae and AM Her-like), and strong steady sources, are discussed. HEAO A2 light curves for the greater than 2 keV flux from SS Cygni are presented, along with the pulse height spectrum and inferred incident spectrum. With regard to the high luminosity degenerate dwarf candidates, it is noted that only for Sco X-1 and Cyg X-2 has even optical evidence for binary periodicity been seen. The attributes of suitable X-ray experiments are reviewed, concerning the simultaneous observation of low energy X-rays, a large area for studying short flares, low background, and the need for both broad band spectral response and high resolution.

Swank, J. H.↗
NASA NTRS1981

Coal/rock interface detection by sensitized pick, part A

In order to increase the operating margins of the detector for safe, reliable operation under difficult in-mine conditions the transmitted signal strength was increased to provide additional signal margin for in-mine conditions and the transmitter section was redesigned to reduce frequency pulling of the transmitter frequency with variations in antenna load. The linearity of the pick load SCO signal with true pick load was increased, and hysteresis effects were minimized. The sensitized pick hardware was ruggedized for rough inmine use. The sensitized pick and telemetry system provided excellent, high quality signals proportional to cutting load under all conditions experienced during testing.

Wu, P. T. K.↗
NASA NTRS1980

X-ray observations of the OAO1653-40 field

The region of sky containing OAO1653-40 have been observed simultaneously with the Einstein and Copernicus satellites in 1979 August. A best position of RA = 254.318 degrees, Dec = -41.577 degrees (1950) and a period of 38.019 + or - 0.009 sec were obtained for the X-ray pulsar discovered by White and Pravdo. The X-ray spectrum shows considerable photoelectric absorption with an equivalent hydrogen column density of 2.3 x 10 to the 23rd atom per sq cm. An upper limit to any 0.5-3.0 keV flux from V861 Sco of (4 + or - 1) x 10 to the -13th erg /sq cm/sec was also obtained.

Parmar, A. N.↗
NASA NTRS1981

A note on the statistics of early-type close binaries

A degree of contact index (I sub c) is defined, and its frequency diagram is given for 16 early-type close binaries. The objective is to determine whether the numbers of such systems are continuous or discontinuous across marginal contact. Data for four of the systems (TU Mus, V499 Sco, Delta Pic, and SZ Cam) derive from new photometric analyses, the results of which are also given. Present results indicate that there is continuity in frequency across marginal contact, although it would be desirable to include more binaries as further observations become available. It is noted that the only two systems in the bin of largest I sub c are known to be in the rapid phase of mass transfer.

Wilson, R. E.↗
NASA NTRS1981

Two young stars in L 43

Optical and infrared photometry has been obtained for the two stars (RNO 90 and RNO 91) illuminating reflection nebulae in the small, filamentary dust cloud L 43. Spectrograms of RNO 90 in the blue and red have also been obtained, which show that it is a T Tauri star. Both stars have strong infrared excesses, placing them firmly in the 'dust' position of the H - K, K - L diagram. The absorption reversals superimposed on the Balmer lines from H-alpha to H-delta in RNO 90 display an interesting effect. They appear to move progressively redward from a position near the blue edge of the emission line at H-alpha to a nearly central location at H-delta. L 43 is located near the star-forming end of the Sco OB2 association, but is relatively isolated from the major center of activity, the Rho Oph cloud. There are a large number of similar-looking small clouds in its vicinity, only one of which is known to have an associated T Tauri star (AS 209). The complexity of this, the nearest star-forming region in an OB association, is illustrated.

Herbst, W.↗
NASA NTRS1980

Data reduction and analysis for the graphite crystal X-ray spectrometer and polarimeter experiment flown aboard OSO-8 spacecraft

The documentation and software programs developed for the reception, initial processing (quickbook), and production analysis of data obtained by solar X-ray spectroscopy, stellar spectroscopy, and X-ray polarimetry experiments on OSO-8 are listed. The effectiveness and sensitivity of the Bragg crystal scattering instruments used are assessed. The polarization data polarimetric data obtained shows that some X-ray sources are polarized and that a larger polarimeter of this type is required to perform the measurements necessary to fully understand the physics of X-ray sources. The scanning Bragg crystal spectrometer was ideally suited for studying rapidly changing solar conditions. Observations of the Crab Nebula and pulsar, Cyg X-1, Cyg X-2, Cyg X-3, Sco X-1, Cen X-3, and Her X-1 are discussed as well as of 4U1656-53 and 4U1820-30. Evidence was obtained for iron line emission from Cyg X-3.

Novick, R.↗
NASA NTRS1982

Solar analogs in the 2600 to 3200 A region

No criteria for the selection of solar analogs are found. At low dispersion, the spectra of 16 Cyg A, 16 Cyg B, 18 Sco and alpha Cen A look identical to each other and to sunlight reflected from Galilean satellites with the possible exception of Mg II lambda 2800 being stronger in the stars. The use of alpha Cen A or 16 Cyg B as solar substitutes for planetary photometry is expected to be far superior to using published solar irradiances.

Hardorp, J.↗
NASA NTRS1982

The peculiar UV extinction of Herschel 36

The differential extinction curve of Herschel 36 was determined from International Ultraviolet Explorer data. It is quite unusual, characterized by a distinct 2200 A peak with a very low far blue end at 5 to 7 mu to the -1 power. The star appears to be an extreme member of the group Savage drew attention to, previously consisting only of theta Ori, NU Ori, sigma Sco, and rho Oph. It appears that multiple scattering effects are needed to explain the observations.

Hecht, J.↗
NASA NTRS1982

A model for the 1979 outburst of the recurrent nova U Scorpii

A series of ultraviolet spectra were obtained of the recurrent nova U Sco during its recent outburst with the IUE satellite. These spectra were analyzed and found to consist primarily of emission lines although broad resonance absorption is present during the first week. These data, in combination with the optical data, show that the nova ejecta is very depleted in hydrogen relative to helium and is rich in nitrogen. An optical spectrum, obtained nine months after the outburst, shows predominantly He II emission lines, indicating that the gas being transferred from the secondary is very helium rich and that the secondary is highly evolved. These data are interpreted to imply that the outburst is associated with the accretion of helium rich material by a massive white dwarf in a close binary system. Neither the observational data nor the theoretical calculations, permit differentiation between a thermonuclear runway or an accretion event as the cause of the outburst. In both cases, an equal amount of material is ejected at equal speeds.

Starrfield, S.↗
NASA NTRS1981

Relativistic astrophysics - The view from Texas in Baltimore /Review/

Recent observational and theoretical work presented at the Tenth Texas Symposium on Relativistic Astrophysics held in Baltimore, Maryland from December 15-19, 1980, is outlined. Areas covered include the theoretical foundations of relativistic astrophysics in general relativity, quantum gravitational theory and the association of grand unification with astronomical and cosmological issues, the cosmic microwave, X-ray, gamma-ray, UV, cosmic ray and gravitational wave backgrounds, the current expansion rate and average mass-energy density of the universe, and mechanisms of galaxy formation. Also discussed are the characteristics of active galaxies and clusters emitting in the gamma-ray and X-ray regions, and compact objects formed from supernova explosions, including pulsars, X-ray-emitting neutron stars, Sco X-1 and SS 433, gamma-ray sources, and X-ray and gamma-ray bursters.

Trimble, V. L.↗
NASA NTRS1982

Ultraviolet observations of four symbiotic stars

Observations were obtained with the International Ultraviolet Explorer (IUE) of four symbiotic stars. The UV spectra of YY Her, SY Mus, CL Sco, and BX Mon are characterized by varying degrees of thermal excitation. These low resolution spectra have been analyzed in terms of line-blanketed model atmospheres of early A, B, and F type stars in order to identify the nature of the hot companion in these systems. The expected emission from early main sequence stars does not fully explain the observed distribution of UV continuum energy over the entire IUE spectral range (1200-3200 A). More likely the observed continuum may be originating from an accretion disk and/or hot subdwarf that photoionizes circumstellar material, and gives rise to the high excitation lines that have been detected. The Bowen fluorescent excited lines of O III in SY Mus exhibit slightly broadened profiles that suggest possible turbulent motions in an extended circumstellar cloud with characteristic velocities of approximately 300 km/s.

Michalitsianos, A. G.↗
NASA NTRS1982

The local interstellar medium

Analysis of the velocities of optical interstellar lines shows that the sun is immersed in a coherently moving local interstellar medium whose velocity vector agrees with that of the interstellar wind observed through backscatter of solar H Ly-alpha and He lambda 584 photons. The local interstellar medium consists of both cool clouds and warm intercloud medium gas, has a mass of perhaps approximately 30 solar masses, does not have severe depletion of trace elements from the gas phase, and appears to be material which has been shocked and accelerated by stellar winds and supernovae associated with the Sco-Oph OB association.

Crutcher, R. M.↗
NASA NTRS1982

IUE observations of the X-ray burst source 4U/MXB 1735-44

The ultraviolet (1250-1950 A) energy distribution of the X-ray burst source 4U/MXB 1735-44 has been observed with the International Ultraviolet Explorer. The source was detected with an average flux of 1.1 x 10 to the -15th ergs/sq cm per sec per A. The similarity of the optical energy distribution of this source to that of Sco X-1 extends into the far-ultraviolet. Assuming that the optical and ultraviolet emission of MXB 1735-44 is due to reprocessing of X-rays in an accretion disk, the ratio of X-ray to bolometric (optical + ultraviolet) flux has been used to make an estimate of the thickness of the disk. For an assumed X-ray albedo of 0.5, it is found that the disk extends to less than approximately 6 deg from the orbital plane.

Hammerschlag-Hensberge, G.↗
NASA NTRS1983

Spectrophotometric observations of symbiotic stars and related objects

Calibrated optical spectrophotometric observations of 16 symbiotic and symbiotic-like objects are presented. The objects observed include Z And, T CrB, CH Cyg, CI Cyg, V1016 Cyg, V1329 Cyg, AG Dra, YY Her, RS Oph, XX Oph, AG Peg, AX Per, CL Sco, HM Sge, AS 289, and M1-2. Integrated emission-line intensities are tabulated for comparison with ultraviolet and infrared data, as well as with previous optical studies. The reddening to each of the objects is derived by assuming that Balmer lines are emitted in their case B recombination ratios. However, the values so derived are often systematically higher than reddening estimates from the ultraviolet 2200 A feature. Comparisons with the available data from other wavelength ranges are noted.

Blair, W. P.↗
NASA NTRS1983

First detection of winds in red giants by microwave continuum techniques

Eight red giants and supergiants have been observed at 4885 MHz (6 cm) with the Very Large Array in an attempt to detect continuum emission. The bright giant Alpha-1 Her (M5 II) was detected at an average flux density of 0.9 + or - 0.13 mJy. Since the likely source of this emission is an ionized, optically thick component of a stellar wind, this detection implies a mass loss rate of 2 x 10 to the -9th solar masses per yr for the ionized gas. The fraction of the outflow in Alpha-1 Her that is ionized (0.002-0.02) seems to be similar to that previously found for Alpha Ori and Alpha Sco A. Alpha Boo (K2 IIIp) and Beta Gem (K0 III) are probable and definite detections, respectively. The derived ionized mass loss rates for these two stars are about 1 x 10 to the -10th solar masses per yr, implying in the case of Alpha Boo that the wind is largely ionized.

Drake, S. A.↗
NASA NTRS1984

Polarization of Comptonized photons

The polarization of Comptonized X-rays as a function of energy and emission angle is obtained. The geometry utilized is that of the semi-infinite plane with the source photons located on a plane at a finite optical depth below the surface. It is further shown what information is obtainable from polarization measurements at only two different energies. The observed values for the X-ray sources Cyg X-1 and Sco X-1 are used to illustrate the calculations.

Williams, A. C.↗
NASA NTRS1983

A mercuric iodide detector system for X-ray astronomy. I - Design considerations and predictions of background and sensitivity

Since the discovery of Sco X-1 initiated X-ray astronomy in 1962, this science has progressed in connection with the placement of X-ray photon detectors above the atmosphere by means of rockets, balloons, and satellites. In the last few years, studies have been conducted regarding the use of mercuric iodide (HgI2) as room temperature X-ray detector for applications in hard X-ray astronomy. These detectors combine a high quantum efficiency with good energy resolution. The sensitivity of an astronomical X-ray telescope is discussed, and a description is presented of a specific design accepted for the HDXT to be flown on Spacelab. Attention is given to predictions of the background counting rate of the detector assembly in this design, taking into account the results of a Monte Carlo simulation of the detector assembly in the radiation environment at balloon altitudes (40 km).

Ricker, G. R.↗
NASA NTRS1984

Do the Arching HI Filaments Show in Local Reddening Data?

Probable dust counterparts of arching structures are investigated in two cases: (1) the Eridanus expanding shell; and (2) the extended Sco-Cen feature. Color excess data may be used to derive distance and dimension estimates of these structures. Color excesses from two areas SA 121 and SA 144 situated on the position of the 3.2 to 6.3 km/s velocity-slice are applied. Some stratification of the color excesses is noticed for both areas but extreme patchiness typifies particularly the dust in the SA 144 region.

Knude, J.↗