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At least 685 records · Page 38
All sourcesNASA NTRSDOE OSTI
NASA NTRS1974

The 90-day report for SL4 experiment S019: UV stellar astronomy

The use of Experiment S019 to obtain moderate dispersion stellar spectra extending down to 1300A with sufficient spectral resolution to permit the study of ultraviolet (UV) line spectra and of spectral energy distributions of early-type stars is studied. Data obtained from this experiment should be of sufficient accuracy to permit detailed physical analysis of individual stars and nebulae, but an even more basic consideration is the expectation of obtaining spectra of a sufficient number of stars so that a statistically meaningful survey may be made of the UV spectra of a wide variety of star types. These should include all luminosity classes of spectral types O, B and A, as well as peculiar stars such as Wolf-Rayet stars and Ap or Am stars. An attempt was also made to obtain, in the no-prism mode, low dispersion UV spectra in a number of Milky Way star fields and in nearby galaxies.

Source record↗
NASA NTRS1973

Laboratory simulation of graphite formation in stellar envelopes

A technique has been developed which permits laboratory simulation of graphite condensation in the envelopes of cool, late sequence stars. Processes in the stellar envelope were simulated by allowing hydrogen-carbon mixtures of typical circumstellar composition and temperature to expand freely into vacuum, cooling and supersaturating the vapor. Expansion products were determined mass spectrometrically through the use of molecular beam techniques. The results of laboratory expansions were scaled to those occurring near M and N stars by comparing the number of collisional events in each case. Kinetic considerations indicate that the important rate process in rarefied envelopes will be C2 formation; consequently scaling by termolecular collisions was employed. Results of this study imply that envelope expansions near M giants contribute at most .01 of the observed interstellar grain density. In the case of pulsating N stars, on the other hand, the results are not inconsistent with previous predictions of essentially complete carbon condensation.

Dorfeld, W. G.↗
NASA NTRS1973

Stellar flux calibration at 10 and 20 microns using Mariner 6, 7, and 9 results

The stellar flux calibrations at 10 and 20 microns have been obtained by comparing observations of alpha Orionis and alpha Scorpii with observations of the central area of Mars. The flux from Mars, in turn, has been inferred from data of the Mariner 6, 7, and 9 infrared radiometers. If the 10- and 20-micron broadband magnitudes of alpha Ori are set equal to -5.18 and -5.70, the flux of a zero magnitude star has been determined to be 1.3 plus or minus 0.2 times 10 to the -16th power and 8.1 plus or minus 1.5 times 10 to the -18th power W/sq cm/micron at 10.0 and 20.0 microns.

Becklin, E. E.↗
NASA NTRS1974

Is the present stellar birthrate really determined by gas density

The assumption that the present star formation rate is determined primarily by the gas density is examined with respect to its consistency with the results of recent studies of supernovae rates in Sb and Sc galaxies and mean H I space densities in the disks of these galaxies. A recent reexamination of the mean gas density in the Sb and Sc galaxies is shown to imply that, if the 'clumpiness' of gas in the disks of these galaxies is similar, the gas density is not the primary factor in determining the overall present stellar birthrate.

Black, D. C.↗
NASA NTRS1974

Stellar and solar X-ray polarimetry

Astronomical stellar and solar studies involving X-ray polarimetry are discussed along with the statistical limitations inherent in polarimeter measurements and the design principles of a number of polarimeter types. Attention is given to photoelectric polarimeters, secondary fluorescence X-ray polarimeters, Borrmann-effect polarimeters, circular polarization analyzers, gamma-ray polarimeters, and multilayer reflection polarimeters. Bragg crystal polarimeters are considered, taking into account the theory of the polarimeter operation, aspects of instrument design, and the occurrence of systematic errors. The design and the performance of a rocket and a satellite Thomson-scattering polarimeter are also examined.

Novick, R.↗
NASA NTRS1974

Studies of hydrodynamic events in stellar evolution. III Ejection of planetary nebulae

Investigation of the dynamic behavior of the hydrogen-rich envelope (0.101 solar mass) of an evolved star (1.1 solar mass) as the luminosity rises to 19,000 solar luminosities during the second ascent of the red-giant branch. For luminosities in the range 3100 less than L less than 19,000 solar luminosities the H-rich envelope pulsates like a long-period variable (LPV) with periods of the order of a year. As L reaches 19,000 solar luminosities, the entire H-rich envelope is ejected as a shell with speeds of a few times 10 km sec. The ejection occurs on a time scale of a few LPV pulsation periods. This ejection is shown to be related to the formation of a planetary nebula. The computations are based on an implicit hydrodynamic computer code. Tand rho-dependent opacities and excitation and ionization energies are included. As the H-rich envelope is accelerated off the stellar core, the gap between envelope and core is approximated by a vacuum filled with radiation.

Kutter, G. S.↗
NASA NTRS1974

The stellar and solar tracking system of the Geneva Observatory gondola

Sun and star trackers have been added to the latest version of the Geneva Observatory gondola. They perform an image motion compensation with an accuracy of plus or minus 1 minute of arc. The structure is held in the vertical position by gravity; the azimuth is controlled by a torque motor in the suspension bearing using solar or geomagnetic references. The image motion compensation is performed by a flat mirror, located in front of the telescope, controlled by pitch and yaw servo-loops. Offset pointing is possible within the solar disc and in a 3 degree by 3 degree stellar field. A T.V. camera facilitates the star identification and acquisition.

Huguenin, D.↗
NASA NTRS1974

Stellar content of the nuclei of elliptical galaxies determined from 2.3 micron CO band strengths

Observations of the luminosity sensitive CO absorption band at 2.3 micron are presented for the nuclei of 16 epsilon and SO galaxies. Preliminary data on the radial variation of the CO index in 6 galaxies are also given. The data show that the 2-u radiation from the nuclei is dominated by high luminosity stars of integrated spectral type later than K5. There is only a small variation in the CO absorption from galaxy to galaxy, and only a slight variation with measuring aperture size from 17.5 in. to 59 in. The data can be used to synthesize stellar populations for elliptical galaxy nuclei.

Frogel, J. A.↗
NASA NTRS1974

The interaction of interstellar gas with stellar density wave packets

We have numerically studied the interaction between interstellar gas and a gravitational perturbation produced by a fluctuation in the stellar mass distribution. For a simple equation of state, shock waves develop even if the gravitational perturbation is aperiodic and transient. In a medium which can change thermal phase, shocks do not form and the gas makes a transition directly to the cold, dense phase. The cold material has an anomalous velocity imparted to it by the gravitational perturbation and it becomes an accretion front moving through the hot gas and capturing it. The accretion fronts trigger thermal phase change on a large scale and can reproduce the extent of observed cold clouds. Furthermore their high mass is favorable to gravitational instability and subsequent star formation.

Baker, P. L.↗
NASA NTRS1975

Formation of molecular lines in stellar atmospheres

Statistical equilibrium of electronic states of diatomic molecules in stellar atmospheres is examined. Atmospheres discussed are representative of the sun, Arcturus (K-giant) and Betelgeuse (M-supergiant). A comparison of the relative collisional and radiative contributions to the equilibrium of the ground electronic state shows that this state is collisionally controlled and that the line source function for vibration-rotation transitions within this state is equivalent to the Planck function. Examination of the equilibrium for excited electronic states demonstrates that the exchange between these states and the ground electronic state is most probably determined by radiative excitation. This result implies that scattering rather than pure absorption is the appropriate mechanism for the formation of lines belonging to these electronic transitions. The scattering hypothesis is given a preliminary check against solar observations. Areas for future investigations are outlined.

Hinkle, K. H.↗
NASA NTRS1975

Skylab ultraviolet stellar spectra - Variation of intensity and structure of strong lines with temperature and luminosity

Objective-prism spectra at ultraviolet wavelengths extending to 1300 A were photographed during the three Skylab missions in a survey covering 9 percent of the sky. Several spectral features, notably resonance lines of C IV and Si IV, show striking variations with stellar temperature and luminosity. Marked P Cygni profiles in C IV and Si IV, indicative of significant outflow of mass, appear in the spectra of all stars with bolometric magnitude brighter than -8.4.

Henize, K. G.↗
NASA NTRS1975

Stellar winds driven by Alfven waves

Properties are analyzed of stellar winds in which Alfven waves propagating outward along radial magnetic-field lines drive the dynamic expansion of the corona. It is shown that the constants of motion of these winds may be simply expressed in terms of reference-level parameters near the star. The analysis indicates that the streaming velocities at infinity as well as the mass and energy fluxes of winds accelerated solely by Alfven-wave pressures will vary over ranges of values that depend on the initial Alfven-wave energy flux. The dynamics of the acceleration mechanism producing these winds is discussed in detail, and a star similar to the sun is considered for purposes of numerical illustration.

Belcher, J. W.↗
NASA NTRS1975

Stellar refraction - A tool to monitor the height of the tropopause from space

Calculations of stellar refraction for a setting or rising star as viewed from a spacecraft show that the tropopause is a discernible feature in a plot of refraction vs time. The height of the tropopause is easily obtained from such a plot. Since the refraction suffered by the starlight appears to be measurable with some precision from orbital altitudes, this technique is suggested as a method for remotely monitoring the height of the tropopause. Although limited to nighttime measurements, the method is independent of supporting data or model fitting and easily lends itself to on-line data reduction.

Schuerman, D. W.↗
NASA NTRS1975

Numerical techniques for the linear, nonadiabatic stellar pulsation problem

The linear, nonadiabatic eigenvalue problem is formulated using Castor's method for calculating radial pulsations of stellar models. Both left and right eigenvectors are calculated. Initial eigenvalues for the linear, nonadiabatic solutions are obtained from the adiabatic eigenvalues and left and right eigenvectors. The orthogonality relation is obtained. Simple formulas for the Newton method are given. The iteration procedure is constrained to improve convergence. The Newton method is less satisfactory than the secant method for difficult cases. The linear, nonadiabatic solutions are shown to be sensitive to the number of zones with tau smaller than 2/3, and the value of (P/P sub r) surface or tau (surface). Optimum values can be determined for the number of zones and tau (surface). Application of the method to Population II Cepheids is briefly presented.

Bednarek, T. A.↗