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NASA NTRS1982

Ultraviolet spectra of Herbig-Haro objects and of the environment of the Cohen-Schwartz star

Observations in both spectral regions were used in order to determine the continuous energy distribution and the emission line fluxes for H-H 2. The continuous spectrum is similar to that in H-H 1 and F lambda increases rapidly towards shorter wavelengths. This statement is found to be qualitatively correct for all obvious choices of the ultraviolet extinction curve if we use the E(B-V) value determined by the use of the S II method. The origin of the continuum remains enigmatic. The emission line spectrum of H-H 2 shows an even somewhat higher degree of ionization than the spectrum of H-H 1, indicating an even larger discrepancy between ionization information from optical data and that contained in the UV spectra. The immediate environment of the Cohen-Schwartz star emits a continuous spectrum similar to that of a H-H-object but increasing even more steeply towards shorter wavelengths.

Boehm, K. H.↗

NASA NTRS1982

IUE spectroscopy, visible-band polarimetry, and radiometry of V641 Mon

This hot, double line, ellipsoidal variable member of NGC 2264 has been shown previously to be either a semi-detached or contact close binary. Low-resolution IUE spectra are best fitted to a Kurucz model atmosphere for very small (approximately 0.08 mag) E(B-V). The familiar interstellar absorption dip near lambda 2200 is apparently absent. A suitable model atmosphere can be fitted to the IUE fluxes, but flux excesses (compared to the model) appear for all the published U through L magnitudes. The spectrum of the B through L excess appears to follow a .0001 lambda dependence. It is shown that this cannot be interpreted as arising from another star fortuitously observed in the visible band or IR. Ground based polarization measures indicate V641 Mon to be a polarization variable. Previous and new V light curves show the amplitude of light variability itself to be variable by about a factor of 2. It is suggested that all these observed characteristics are best explained by postulating "third light" and identifying part of it with Rayleigh scattered starlight very near to the stars. From this same region there arise circumstellar absorptions which give rise to nontheoretical strengths for Si II and Si III lines.

Koch, R. H.↗

NASA NTRS1982

Ultraviolet observations of nova Aquila, 1982

A bright nova in Aquila was discovered with a visual magnitude of 6 to 7. A number LWR and SWP spectra of the object were obtained with the IUE. The nova has a heavily reddened spectrum, E(B-V)= 0.55 + or - 0.15, and a complex shot wavelength spectrum with both narrow emission features and broad absorption troughs, indicating terminal velocities as high as 10,000 km/s. Both the continuum flux and the absorption line profiles changed between two observations. Short period variations were also observed.

Snijders, M. A. J.↗

NASA NTRS1981

Ultraviolet interstellar extinction toward stars in the Orion Nebula and toward HD 147889

The International Ultraviolet Explorer (IUE) was used to obtain low resolution absolute ultraviolet energy distributions for the four Trapezium stars Theta(1) Orionis A, B, C, and D, Theta(2) Orionis A and B, HD 147889, and several unreddened standard stars. The observations for Theta(1) Orionis B reveal a peculiar extended object. The measurements for the rest of the stars were used to derive UV extinction curves. The derived curves are very different from the average galactic curve. The curves for the Orion stars all exhibit smaller than normal middle and far-UV extinctions. Although a 2175 A feature is present, its strength, when normalized to E(B-V), is smaller than in the average galactic curve. In contrast, the curve for HD 147889 has a pronounced 2175 A feature followed by smaller than normal extinction for an inverse wavelength between 5 and 7 per micron.

Bohlin, R. C.↗

NASA NTRS1982

Further photometric observations of 2A 0311-227

Simultaneous V, B, and U photometry is presented for the AM Herculis type system 2A 0311-227. A Fourier analysis has failed to detect the 6 minute quasi-periodic oscillation reported earlier. It has, however, revealed the presence of oscillations at 20.2 and 13.7 minutes. These are interpreted in terms of a nonsinusoidal light curve. U, B, and V light curves are given and discussed in terms of current models for AM Her systems. B-V and U-B color curves are also presented, as is the behavior of the system in the color-color plane.

Williams, G.↗

NASA NTRS1982

ANS spectrophotometry - The bright X-ray binaries Hercules X-1 /HZ Herculis/ and Cygnus X-1 /HDE 226868/

Complete ultraviolet light curves for HZ Her immediately after a well-defined X-ray turn-on in 1975 are obtained. The features of the curve are found to correspond well with features seen in the optical. The absolute level of emission at maximum light at 1550 A is in good agreement with the calculations of the X-ray reflection effect of Milgrom and Salpeter (1975). It is found that at 1550 A approximately 20% of the light at maximum comes from the accretion disk. Similar observations of Cyg X-1 make it possible to determine the degree of reddening, equivalent to E(B-V) = 0.95 + or - 0.07, from the strength of the 2200 A interstellar absorption feature. The distance inferred from this amount of reddening requires that the optical star be luminous and, therefore, massive. Observations obtained during the May 1975 X-ray transition show ultraviolet excess when compared with the data obtained six months later.

Wu, C.-C.↗

NASA NTRS1982

Ultraviolet, visual, and infrared observations of the WC7 variable HD 193793

Low-resolution IUE data are used to explore the ultraviolet extinction toward the Wolf-Rayet star HD 193793 and to search for ultraviolet variability that might relate to the infrared variability. High-dispersion IUE observations are used to investigate the nature of the stellar wind of the star and to search for anomalies in the interstellar line spectrum that might be expected to be found toward a star that has recently formed a dust shell. Finally, the ultraviolet and new visual and infrared data are combined to investigate the full energy distribution of this unusual source. The energy distribution is found to extend from 0.12 to 12.5 microns, and the ultraviolet data suggest a normal WC-7 type star. A wind terminal speed of about 3000 km/s is implied by the data, as well as an E(B-V) value of 0.85. The dereddened ultraviolet to visual energy distribution is consistent with a star having effective temperature of about 43,000 K.

Fitzpatrick, E. L.↗

NASA NTRS1981

Results from the central Hyades survey

Results of a soft X-ray survey of the central 5 deg of the Hyades star cluster made with the Einstein Observatory Imaging Proportional Counter are presented. Virtually all of the late F and early G stars in the cluster were detected at an X-ray luminosity of greater than 10 to the 28.5 erg/sec, although only about 50% of the stars in the cluster as a whole were detected. Plots of X-ray luminosity against B-V index indicate that the typical solar-type star in the Hyades is emitting soft X-rays at a level approximately 30 times that of the active sun. Histograms of the X-ray to bolometric luminosity ratio reveal a gradual distinction between late A-early F stars, which are expected to possess little or no convective envelope, and solar-type (F8-G5) stars, with convective outer atmospheres. Results confirm the dependence of stellar coronal activity on rotation, and establish the prevalence of stellar coronae throughout the main sequence and the giant regions of the H-R diagram.

Stern, R. A.↗

NASA NTRS1982

The eight-color asteroid survey - Standard stars

Compositionally diagnostic information regarding the spectral reflectance of faint asteroids and planetary satellites, obtained using a photometric system, is presented. Standard UBV and range in effective wavelength from 0.34 to 1.04 microns are among the eight broadband filters relative to the study. An InGaAsP photomultiplier of high quantum efficiencies employed for longer wavelengths, allows work to magnitude 17 and fainter when used in conjunction with a 2 m telescope. Magnitudes and color indices with mean uncertainty + or - 0.006 mag for 50 standard stars are presented, and by setting the mean colors of four of these stars to zero, the zero point of the system is established. Sun color implications resulting from the study are U-B = 0.20 + or - 0.02, and B-V = 0.67 + or - 0.02.

Tedesco, E. F.↗

NASA NTRS1982

The IUE spectrum of BD + 39 deg 4926

IUE spectra of the A- or F-type supergiant BD + 39 deg 4926 have been combined with existing optical data. Comparison with model atmospheres yields an effective temperature of 7750 K, gravity log g of 0.5, and a reddening corresponding to E(B-V) of 0.15. The Mg II wavelength 2800 feature was used to estimate the abundance of Mg(+), and the value of log (epsilon (Mg(+)/epsilon (Ca(+)) was found to be about 2.7.

Saha, A.↗

NASA NTRS1982

Photoelectric photometry of asteroids 33 Polyhymnia and 386 Siegena

The photometric parameters of 33 Polyhymnia and 386 Siegena were determined in the course of an international campaign performed during August 15-September 14, 1980 at Table Mountain Observatory, European Southern Observatory, and Catania Astrophysical Observatory. The rotational periods and amplitudes were determined, and the multiple-scattering factor was found to be 0.15 plus or minus 0.06 for 386 and 0.26 plus or minus 0.33 for 33, implying higher albedos in each case than expected according to their taxonomic classes, C and S, respectively. The color indices B-V and U-B were measured and found to differ significantly from those given by Bowell et al. (1979).

Zappala, V.↗

NASA NTRS1983

Time-resolved ultraviolet and optical spectroscopy of the pulsating X-ray source H2252-035

UV spectrophotometry and and optical spectroscopy of H2252-035, a close binary featuring a spinning, magnetized star, were carried out with instrumentation on the IUE satellite, in addition to ground-based observations from the Lick Observatory. An excess reddening was determined, with E(B-V) equal to 0.10. The spectrum from 1200-22,000 A was decomposed into a blackbody with a temperature of 13,400 K and a power law wavelength component, where the exponent is 2.74, which fits the excess UV and IR excesses. The exponent value is noted to be amenable to a disk model with a slight curvature because of its finite extent. The emission-line intensities were found to vary by a factor of two, with some of the variations accountable by a modulation in-phase with the optical continuum binary modulation.

Cordova, F. A.↗

NASA NTRS1983

IUE observations of E1405-451 - A new AM Herculis type cataclysmic variable

International Ultraviolet Explorer observations of the recently discovered AM Herculis type cataclysmic variable E1405-451 reveal a UV spectrum (1000-3000 A) similar to the other members of the type. The continuum flux distribution rises steeply at short wavelength and shows the effects of interstellar extinction. Best fit parameters for a blackbody spectrum are T = 25,500 + or - 2300 K with E(B-V) = 0.13 + or - 0.05. Many strong emission lines appear in the spectrum with similar intensities to those in AM Her. C IV 1550 and He II 1640 show some sign of a P Cygni profile. If these profiles are truly P Cygni, they indicate the intriguing possibility of a magnetically confined, radiatively driven wind present in all AM Her systems but only observable in a subset with an orientation like E1405-451.

Nousek, J. A.↗

NASA NTRS1983

Worldwide photometry and lightcurve observations of 16 Psyche during the 1975-1976 apparition

Twenty-six lightcurves of Psyche are presented together with UBV photometry and phase functions from 1975 and 1976. Combining photometric data from this opposition with those from previous apparitions resulted in a mean phase coefficient in V of 0.026 + or - 0.002 mag/deg. No significant phase-dependent variation in the U-B color could be determined from the data; the B-V color, however, displayed a reddening with phase of 0.0010 + or - 0.0004 mag/deg. It is concluded that compositional variations over Psyche's surface are minor, and that Psyche's opposition effect is typical of that for other well-observed asteroids. Psyche's behavior is accounted for if, to the first order, its shape is that of a triaxial ellipsoid with axial ratios near 5:4:3.

Tedesco, E. F.↗

NASA NTRS1983

Ultraviolet observations of the transient X-ray sources A0535 + 26 and A0620-00

Observations of A0535+26 (HDE 245770) by the ANS in September 1975 and March 1976 when it was at the X-ray low state are discussed. Also observed were 58 early-type stars lying within 10 deg of HDE 245770; these stars are used to derive a localized extinction curve. On the basis of the depth of the 2200 A interstellar absorption feature observed in the ANS flux distribution of HDE 245770 and the shape of the localized extinction curve, an E(B-V) = 0.72 is derived for HDE 245770. Observations were made of this system during its X-ray flare-up (October 1980) and quiescent (November 1981) states by the IUE. It is noted that the fine error sensor on board the IUE detected an increase in the optical brightness of HDE 245770 during the X-ray outburst. This greatly corroborates the identification of HDE 245770 as the optical counterpart of A0535+26. No significant change in the absorption-line profiles during the X-ray high and low periods is found, indicating that there was no significant increase in the stellar wind density when the X-ray flare-up occurred. The UV continuum level increased by less than 6 percent when it was near peak X-ray luminosity. The UV spectrum of HDE 245770 suggests that it is a B0 V or a B0 III star with its dereddened continuum slope slightly in favor of being a giant.

Wu, C.-C.↗

NASA NTRS1983

RW Tauri as a weak W Serpentis star

Observations of the short-period eclipsing binary RW Tau made with the LWR and SWP cameras of the IUE satellite and with the ITS scanner at the 3-m Shane telescope of the Lick Observatory in August and October, 1982, are reported and analyzed. At total eclipse, weak excess continuous radiation in the LWR range and emission lines at Si IV (1), C IV (1), Al III (1), Fe III (34), and Mg II (1) in the SWP range were detected. These findings are similar to those for W Ser-type binaries such as U Cep. The parameters of the system are estimated using a bilinearly interpolated atmospheric model of the type developed by Kurucz (1979): primary-star T(eff) = 11,750 K, log g = 4.2, cool-component spectral type = K0 III, E(B-V) color excess = 0.14 mag, system distance = 270 pc. The implications of these findings for proposed models of the W Ser binaries are discussed, and the observation of a possible distant optical companion star 45 arcsec from RW Tau is reported.

Plavec, M. J.↗

NASA NTRS1983

The rotation, color, phase coefficient, and diameter of 1915 Quetzalcoatl

Photoelectric observations of 1915 Quetzalcoatl on March 2, 1981 show that this asteroid has a rotational period of 4.9 + or - 0.3 hr and a lightcurve amplitude of 0.26 magnitudes. B-V and U-B colors are found to be 0.83 + or - 0.04 and 0.43 + or - 0.03, respectively, consistent with Quetzalcoatl being an S-type asteroid. Additional observations from March 31, 1981, give a linear phase coefficient of 0.033 mag/deg and a mean B(1,0) magnitude of 20.10. The resulting estimated mean diameter for Quetzalcoatl is only 0.37 km, making it one of the smallest asteroids for which physical observations have yet been made.

Binzel, R. P.↗

NASA NTRS1983

Ultraviolet observations of M1-2 (= VV 8)

First IUE spectrograms of the peculiar emission-line object M1-2 (= VV 8) are presented. In the wavelength region 1150-3200 A this object is characterized by emission lines superposed on a moderately strong continuum. Some ultraviolet and optical properties of M1-2 are discussed in the context of symbiotic stars and protoplanetary and planetary nebulae. An E(B-V) extinction of 0.37 mag is obtained from the ratio of the He II flux at 1640 and 4686 A and is compared with values derived from other parameters. The ultraviolet observations suggest that M1-2 is a young, high-density planetary nebula of excitation class 5 or 6 with characteristics similar to IC 4997.

Feibelman, W. A.↗