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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 73 records · Page 4
All sourcesNASA NTRSDOE OSTI
NASA NTRS1988

Varves and solar physics

The relationship between varves (visibly striated rocks deposited by glacial run-off) and solar radiation is discussed, proposing that the thickness of any given varve represents the mean annual sunspot number for the year in which the varve was laid down. The solar cycle may entail a deep torsional oscillator whose influence reaches the surface by wave propagation. Several observed features suggest a wave link between the source of solar activity and its surface manifestations. It is suggested that the cause of varve modulation is solar UV and X-ray radiation, which exerts solar cycle influence in the ozonosphere and ionosphere. The undulations and cycles of the Elatina varve bed formation in South Australia are related to solar phenomena. The varve mechanism is significant for the build-up of the protective shield of biogenic oxygen in the palaeoatmosphere.

Bracewell, R. N.↗
NASA NTRS2012

Small Pitch Transition-Edge Sensors with Broadband High Spectral Resolution for Solar Physics

We are developing small pitch transition-edge sensor (TES) X-ray detectors optimized for solar astronomy. These devices are fabricated on thick Si substrates with embedded Cu heat-sink layer. We use 35 x 35 square micrometers Mo/Au TESs with 4.5 micrometer thick Au absorbers. We have tested devices with different geometric absorber stem contact areas with the TES and surrounding substrate area. This allows us to investigate the loss of athermal phonons to the substrate. Results show a correlation between thc stem contact area and a broadening in the spectral line shape indicative of athermal phonon loss. When the contact area is minimized we have obtained exceptional broadband spectral resolution of 1.28 plus or minus 0.03 eV at an energy of 1.5 keV, 1.58 plus or minus 0.07 eV at 5.9 keV and 1.96 plus or minus 0.08 eV at 8 keV. The linearity in the measured gain scale is understood in the context of the longitudinal proximity effect from the electrical bias leads resulting in transition characteristics that are strongly dependent upon TES size.

Smith, S. J.↗
NASA NTRS1988

Gamma-ray, neutron, and hard X-ray studies and requirements for a high-energy solar physics facility

The requirements for future high-resolution spatial, spectral, and temporal observation of hard X-rays, gamma rays and neutrons from solar flares are discussed in the context of current high-energy flare observations. There is much promise from these observations for achieving a deep understanding of processes of energy release, particle acceleration and particle transport in a complicated environment such as the turbulent and highly magnetized atmosphere of the active sun.

Ramaty, R.↗
NASA NTRS1984

Research in solar physics: Some techniques for analyzing data from the ultraviolet spectrometer and polarimeter

Useful information for certain aspects of the analysis of data obtained by the Ultraviolet Spectrometer and Polarimeter (UVSP) on the Solar Maximum Mission (SMM) are contained. The meaning of the UVSPCO-ordinate system and the SMM roll, pitch, and yaw are described and the process for overlaying UVSP images is explained. The various computer programs that calculate the line of sight component of the SMM spacecraft velocity from the spacecraft to the Sun is described. The spacecraft velocity is used to correct or interpret the signal observed in USVP dopplergrams. A method of using the spacecraft velocity to calibrate UVSP dopplergrams and magnetograms, i.e., determine the width of the observed emission line is applied. The UVSP polarization analysis procedures are described and the expressions for the statistical uncertainties in various quantities obtained from UVSP measurements are given.

Henze, W., Jr.↗
NASA NTRS1972

Observing programs in solar physics during the 1973 ATM Skylab program.

Description of the Apollo Telescope Mount (ATM), a set of spaceborne X-ray, ultraviolet, and visible-light telescopes intended to implement the extensive series of solar observations representing one of the major tasks assigned to the three-man crews who will perform three (respectively 28-, 56-, and 56-day long) manned orbital flights in mid-1973, known collectively as the Skylab mission. The ATM capabilities, its principal scientific goals, and planned observing program are reviewed, along with the methods to be used for coordinating the observations with ground-based and other kinds of solar observations.

Reeves, E. M.↗
NASA NTRS1977

Research in Solar Physics: Analysis of Skylab/ATM S-056 X-Ray Data

Data obtained by the X-ray event analyzer are described as well as methods used for film calibration. Topics discussed include analyses of the 15 June 1973 flare, oscillations in the solar soft X-ray flux, and deconvolution of X-ray images of the 5 September 1973 flare.

Henze, W., Jr.↗
NASA NTRS1989

Infrared solar physics from the South Pole

Infrared (IR) observations of the sun could greatly benefit from the quality of the South Pole as an IR site, and the potential for multi-day sequences of uninterrupted observations. A nearly continuous picture of the evolution of the magnetic field in solar active regions could be obtained using vector magnetographs, especially vector magnetographs which incorporate IR array detectors. Observations of the sun over a range of wavelengths in the IR continuum could also be used to study the vertical propagation characteristics of the solar p-mode oscillations.

Deming, Drake↗
NASA NTRS1973

Background of the completed research; relevances to solar physics

Research activities reported consider the atomic structures of highly stripped heavy ions and their modes of formation and destruction in collisions. The lifetime of the metastable 2 3p1 state of the two electron ion F-7(+) was determined by measuring the radiative decay of an excited helium-like fluorine beam, Metastable state quenching measurements were performed on a helium-like ion to obtain the 1 1S0 to 2 3p2 transition probability. Exponential exchange state dependence of X-ray production cross sections was studied in heavy target atoms during collisions with light charged particles.

Sellin, I. A.↗
NASA NTRS1985

Solar physics applications of computer graphics and image processing

Computer graphics devices coupled with computers and carefully developed software provide new opportunities to achieve insight into the geometry and time evolution of scalar, vector, and tensor fields and to extract more information quickly and cheaply from the same image data. Two or more different fields which overlay in space can be calculated from the data (and the physics), then displayed from any perspective, and compared visually. The maximum regions of one field can be compared with the gradients of another. Time changing fields can also be compared. Images can be added, subtracted, transformed, noise filtered, frequency filtered, contrast enhanced, color coded, enlarged, compressed, parameterized, and histogrammed, in whole or section by section. Today it is possible to process multiple digital images to reveal spatial and temporal correlations and cross correlations. Data from different observatories taken at different times can be processed, interpolated, and transformed to a common coordinate system.

Altschuler, M. D.↗
NASA NTRS2005

Laboratory Studies in UV and EUV Solar Physics

A new 5 GHZ Electron Cyclotron Resonance (ECR) ion source for SAO's Ion Beam Experiment was designed, built and tested. Absolute cross sections were measured for electron impact excitation (EIE) in C(2+) (2s2p (3)P(sup o) - 2p(sup 2) (3)P), and empirical EIE rate coefficients were derived. The absolute cross section for EIE in Si(2+) (3s3p (3)P(sup o) - 3s3p (1)P(sup o)) was measured, and our experimental values for absolute cross sections for EIE in C(3+) (2s (2)S - 2p (2)P(sup o)) were reanalyzed and compared to values obtained by other experimental methods and by theory. In addition, a paper was published. The development and testing of the new ion source, the Si(2+) EIE measurements, and the reevaluation of the cross sections for C(3+) resulted from the Ph.D. research of Paul H. Janzen who completed the degree requirements for the Harvard University Department of Physics in 2002. John Kohl served as the Ph.D.Thesis Advisor. Because of delays in bringing the new ion source on line, the measurements of EIE in C(2+) (2s2p (3)P(sup o) - (2)p(sup 2) (3)P) were not completed until 2004. Preparations for measurements of EIE in C(2+) (1s(sup 2) (1)S - 2s2p (1)P(sup o)) are currently underway.

Wagner, William J.↗