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Search indexed NASA NTRS and DOE OSTI research on propulsion, heat transfer, battery materials and energy systems. Follow report and document links to the original sources.

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At least 199 records · Page 11
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NASA NTRS1977

The supernova trigger for formation of the solar system

It is suggested that the explosion of a Type II supernova triggered the collapse of a nearby interstellar cloud and led to the formation of the solar system. Estimates of the abundances resulting from nuclear processing of the supernova ejecta are presented. It appears promising that nucleosynthesis in this single supernova event can account for most isotopic anomalies and traces of extinct radioactivities in solar-system material.

Cameron, A. G. W.↗
NASA NTRS1978

Condensation in supernova ejecta and isotopic anomalies in meteorites

An investigation is conducted of the physical and chemical conditions in an expanding supernova envelope, taking into account the likelihood of grain formation and the chemical composition of the grains. An 'onionskin' presupernova model is used to estimate the chemical and isotopic abundance in the various shells of ejected supernova material. Condensation calculations are performed over a range of pressures and chemical compositions for each of these shells in order to determine the type of grains which could be produced in supernova ejecta. Only grains that are stable under the physical conditions encountered in the presolar nebula can survive and retain their anomalous composition. Two regions in the presolar nebula are considered, and the possible surviving grains are deduced from the appropriate condensation sequences.

Lattimer, J. M.↗
NASA NTRS1978

X-ray emission from MSH 14-63 - Probable remnant of the A.D. 185 supernova

Observations during 1972 from an experiment on OSO 7 detected a 2-10-keV X-ray flux of 1.7 by 10 to the -10th power erg/sq cm per sec from a source coincident with MSH 14-63, the most probable candidate for association with the A.D. 185 supernova. Both the present data and those of Naranan et al. (1977) at lower energy can be fitted by a dual-temperature thermal spectrum similar to that observed in other young supernova remnants. Model calculations indicate that a mass in excess of 5 solar masses must have been ejected in the A.D. 185 supernova event.

Winkler, P. F., Jr.↗
NASA NTRS1979

On the origin of a very close similarity between the spectra of the supernova type 1 in NGC 3198 and the absorption of DQ HeR

The type 1 supernova discovered late in 1966 in NGC 3198 has broad minima in its spectrum break down into a number of significantly narrower absorption bands. The broad minima of tau, sigma and mu, which usually show no details in the spectra of type supernovas, contain a number of narrow absorption bands. The reality of most of these absorption bands is demonstrated by comparison of recordings of spectra of the supernova presented for two moments in time. These minima (particularly of tau and mu,) are a result of blending of several broad absorption bands. The minimum of tau should be a blend of intensive and very broad Fe absorption lines, in which the lower level is metastable. The wavelengths of these line are: 5169, 5198, 5235, 5276, 5317, 5363A.

Mustel, E. R.↗
NASA NTRS1980

Soft X-ray observations of the supernova remnants HB 3 and 3C 58

The HEAO 1 A-2 low energy detectors have discovered soft X-ray emission from a source positionally coincident with the supernova remnant HB 3. The flux in the energy range 0.3-2.2 keV is about 6 x 10 to the -11th ergs per sq cm s. The spectral data are fitted to a hydrogen thermal bremsstrahlung model, and the physical parameters of the supernova remnant are estimated. The age derived is about 21,000 years, and the initial blast energy is about 3.1 x 10 to the 50th ergs. Upper limits to the soft X-ray flux and the luminosity of the supernova remnant 3 C 58 are also derived.

Galas, C. M. F.↗
NASA NTRS1980

Supernovae effects on the terrestrial atmosphere

The first effects of a nearby (10 parsec) supernova on the earth's atmosphere will be caused by ultraviolet radiation dissociating molecular oxygen. The event will be of about one month's duration. Several months later nuclear gamma radiation may arrive, causing a decrease in atmospheric ozone. Cosmic radiation from the supernova remnant will not intercept the earth for at least 1000 years at which time ozone will be seriously depleted. Supernova ultraviolet radiation increases column ozone and atomic oxygen. Atmospheric thermal structure is modified with a large temperature increase in the mesosphere and lower thermosphere and a decrease at higher altitudes caused by enhanced heat loss due to atomic oxygen radiation and conduction.

Aikin, A. C.↗
NASA NTRS1980

Supernova radio remnants and the filling factor of the hot interstellar medium

If a hot (temperature of about one-million K), tenuous gas fills about 90% of interstellar space, then the observed number and surface brightness distribution of galactic radio remnants implies a galactic supernova rate of once about every 30 years. This is consistent with estimates based on observations of historical supernovae, pulsars, and supernovae in other spiral galaxies.

Higdon, J. C.↗
NASA NTRS1981

Accreting white dwarf models for type 1 supernovae. 1: Presupernova evolution and triggering mechanisms

As a plausible explosion model for a Type I supernova, the evolution of carbon-oxygen white dwarfs accreting helium in binary systems was investigated from the onset of accretion up to the point at which a thermonuclear explosion occurs. The relationship between the conditions in the binary system and the triggering mechanism for the supernova explosion is discussed, especially for the cases with relatively slow accretion rate. It is found that the growth of a helium zone on the carbon-oxygen core leads to a supernova explosion which is triggered either by the off-center helium detonation for slow and intermediate accretion rates or by the carbon deflagration for slow and rapid accretion rates. Both helium detonation and carbon deflagration are possible for the case of slow accretion, since in this case the initial mass of the white dwarf is an important parameter for determining the mode of ignition. Finally, various modes of building up the helium zone on the white dwarf, namely, direct transfer of helium from the companion star and the various types and strength of the hydrogen shell flashes are discussed in some detail.

Nomoto, K.↗
NASA NTRS1980

Observations of supernova remnants in the Large Magellanic Cloud with the Einstein Observatory

Consideration is given to the Large Magellanic Cloud (LMC), noting that above 2 keV, the X-ray luminosity of the LMC is dominated by emission from 3-5 point sources similar to the bright sources near the center of our own Galaxy. The imaging proportional counter aboard the Einstein Observatory has been used to locate about 40 X-ray sources in the LMC. Supernova remnants observed in the LMC are presented, noting X-ray position, X-ray counting rate, and radio flux. For the six brightest sources, X-ray spectra have been analyzed to determine temperatures and intrinsic luminosity corrected for the interstellar absorption. These data are compared for parameters for the young galactic remnant of Tycho's supernova. Attention is given to the ratio of X-ray luminosity to radio luminosity, and the data are discussed within the framework of the standard blast-wave theory. The results of applying the model to recorded observations are numerically presented. In addition to providing a sample of objects for investigations of supernova remnants, the data are applicable to studies of galaxies of other morphological types and individual objects, such as N49.

Helfand, D. J.↗
NASA NTRS1981

On the birthrate of galactic supernovae

The birthrate of galactic supernovae is estimated in three different ways. The three ranges overlap, and it is suggested that 70 + or - 35 yr represents a more realistic estimate of the rate than some that have previously been made. The galactic supernova remnants and their observed systematic brightness gradients perpendicular to the galactic plane imply a scale height of about 200 pc for the remnant progenitors and a galactic magnetic field scale height of about 300 pc. Long standing anomalies associated with the young remnant AD 1006, the galactic loops, and faint remnants, are accounted for by the brightness gradient effect. This provides firm, independent evidence for the validity of the remnant method of deducing the birthrate of galactic supernovae.

Lerche, I.↗
NASA NTRS1981

Ultraviolet emission of the Vela supernova remnant and the Cygnus Loop

Ultraviolet emission spectra of several filaments in the Vela supernova remnant and the Cygnus Loop are compared with theoretical models of radiative shocks. Shock velocities range from 85 to 130 km/s. Little or no grain depletion is apparent. Several of the observed filaments deviate from the steady-flow models in the sense that much of the photoionization-recombination zone is absent. It is shown that resonance line scattering within the emitting region can account for the weakness of the C II 1335 and C IV 1550 lines. Evaporation fronts, which are basic to the McKee and Ostriker picture of supernova remnant evolution, do not contribute significantly to the observed emission. Some discrepancies in UV emission predicted by different sets of shock models are traced to differing atomic rates used in the calculations. A fluorescent emission line of H2 may be observable in some supernova remnants.

Raymond, J. C.↗
NASA NTRS1982

Hydrogen two photon emission in the UV spectrum of type 2 supernovae

The continuum emission of Type 2 supernovae demonstrates an ultraviolet (UV) excess when fit by black body emission is attempted. The H two photon emission is advanced as an explanation of the UV excess. A function by which the UV spectra of two Type 2 supernovae (SN 1979c in NGC 4321 and SN 1980k in NGC 6946) are fitted with U,B,V photometric data is presented. The angular velocity of expansion of the supernovae envelope is derived. From this, the linear velocity of expansion and the distances of the parent galaxies are derived. A distance of 17.3 Mpc is obtained for NGC 4321, and a distance of 7.1 Mpc for NGC 6946.

Benvenuti, P.↗
NASA NTRS1981

Stellar clustering as induced by a supernova

A possible mechanism for the fragmentation of the expanding shock wave from a supernova to form stellar clusters is considered. A model of supernova shell expansion is constructed in which the ratio of magnetic field intensity to gas density remains constant during the one-dimensional compression of the interstellar medium by the shock, and the gas and field adjust to a quasi-equilibrium within the shell following shock passage. It is shown that the quasi-equilibrium, which may be considered as an isothermal atmosphere, is unstable to a hydromagnetic instability representing a form of the Parker instability, which results in a clumping of gas at intervals on the order of parsecs. The length and time scales of the instability are consistent with the clustering of newly formed stars observed in Canis Major R1, where there is evidence for supernova-induced star formation.

Baierlein, R.↗
NASA NTRS1982

The cosmic distance scale - Methods for determining the distance to supernovae

It is established by an analysis of alternative methods for the determination of absolute distances to supernovae that there exists a kinematic method, superior to that of Baade (1926), which is illustrated for the case of the Type I supernova 1975a in NGC 2207. In addition, a dynamical method is developed which employs the recently-discovered analytic solutions for Type I supernovae. The requirement that the paradigm invoked in the present study be able to reproduce both fast and slow light curves has implied a dispersion in intrinsic brightness, whose size is approximately that observed in the Virgo and Coma clusters.

Arnett, W. D.↗
NASA NTRS1982

Supernovae, young remnants, and nucleosynthesis

Chemical abundance data from extragalactic supernovae and from supernova remnants (SNR) less than 1000 yrs old are employed to show that nuclear burning beyond helium synthesis actually occurs. Supernova (SN) are classified into types I or II, having no hydrogen lines or featuring hydrogen lines, respectively. The SN I's have been observed as having a preponderance of Fe lines, and emitting from a source at around 12,000 K with a center continuum of approximately 10 AU. Decay chains which could account for detected luminosities and spectra are presented, noting a good fit of Fe II spectrum with observed SN spectra. SNR pass through younger and older stages, going from the outpouring of material to diffusion in the interstellar medium. Expanding flocculi from young SNR show oxygen abundances as well as lines from sulfur, calcium, and argon, with a corresponding necessity of an explosive source of 15 solar masses.

Kirshner, R. P.↗
NASA NTRS1982

The interstellar spectrum of the supernova 1980k in NGC 6946

Bright supernovae in external galaxies offer a rare opportunity to probe the intervening interstellar media over very extended path-lengths, including the disk and halo of the Galaxy and the parent galaxy of the supernova. SN 1980k was discovered in NGC 6946 on 1980 October 29. In the first month after discovery, high resolution optical and ultraviolet observations were obtained to exploit the supernova as a probe of the intervening interstellar media. The obtained data are discussed. In the spectra, absorption lines were observed of Mg I, Mg II, Fe II, Mn II, Ca II and Na I. The absorption lines are attributed to the intervening interstellar media distributed over the very extended line of sight sampled, of order 7 Mpc. These lines are wider and stronger than any previously measured in the quiescent interstellar gas in the halo and disk of the Milky Way and of external galaxies

Pettini, M.↗
NASA NTRS1980

X-ray spectroscopy of supernova remnants

The information which can be obtained from X-ray spectroscopy of supernova remnants is considerd. The fitting of X-ray detector counts to models of the incident spectrum is discussed, and the types of thermal emission models generally employed are presented, including the power law, black body, and thermal bremsstrahlung models of the continua and models of the emission of a hot, optically thin plasma in collisional equilibrium. Observations of 12 supernova remnants made with the Solid State Spectrometer on board the Einstein Observatory are reported, and metal abundances inferred from the lines of the eight remnants showing thermal spectra are summarized. Questions raised by the failure to observe the overabundance of Fe predicted by stellar evolution and hydrodynamic modeling are discussed, and the need to develop more detailed models of the conditions in a supernova remnant in order to interpret the X-ray spectra is noted.

Szymkowiak, A. E.↗
NASA NTRS1982

Supernovae and the origin of the solar system

A review is presented of the astrophysical reasoning that links supernovae to the origin of the solar system. Topics examined concerning the supernova connections include the abundances of the nuclides at the time the solar system formed, the collapse of a solar cloud by supernova triggering, the origins of isotopic anomalies in solar system samples, and the sputtering of interstellar dust with the attendant chemical and isotopic evolution of the interstellar medium. The controversies surrounding each of these topics are critically examined, focusing on the issues arising from the discovery of the isotopic anomalies in meteorites.

Clayton, D. D.↗