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Neupert, W. M.

Publications and source records attributed to Neupert, W. M..

At least 19 records
All sourcesNASA NTRSDOE OSTI
NASA NTRS1994

Evidence of mass outflow in the low corona over a large sunspot

An extreme ultraviolet (EUV) imaging spectrograph designed for sounding rocket flight has been used to search for velocity fields in the low solar corona. During a flight in May, 1989, we obtained emission line profile measurements along a chord through an active region on the Sun. Relative Doppler velocities were measured in emission lines of Mg IX, Fe XV, and Fe XVI with a sensitivity of 2-3 km/s at 350 A. The only Doppler shift appreciably greater than this level was observed in the line of Mg IX at 368.1 A over the umbra of the large sunspot. The maximum shift measured at that location corresponded to a velocity toward the observer of 14 plus or minus 3 km/s relative to the mean of measurements in that emission line made elsewhere over the active region. The magnetic field in the low corona was aligned to within 10 deg of the line of sight at the location of maximum Doppler shift. Depending on the magnetic field geometry, this mass outflow could either re-appear as a downflow of material in distant footprints of closed coronal loops or, if along open field lines, could contribute to the solar wind. The site of the sunspot was near a major photospheric magnetic field boundary. Such boundaries have been associated with low-speed solar winds as observed in interplanetary plasmas.

Neupert, W. M.↗
NASA NTRS1994

Abundance determination in solar active region

An improved method has been developed to evaluate element abundances from emission line intensities of thin plasmas, depending on the differential emission measure (DEM) of the source. Observations made by the Solar EUV Rocket Telescope and Spectrograph (SERTS) Rocket EUV Spectrograph are used to perform a detailed analysis of the DEM distribution for temperatures larger than 10(exp 5) K in a solar active region. Comparison of the DEM distributions obtained by means of lines from different elements allows the verification of relative abundances for the most common elements of the solar corona, and gives an abundance estimates for the minor components, such as Na, Al, Ar, Cr, Mn and Zn.

Monsignori Fossi, B. C.↗
NASA NTRS1994

Mg IX emission lines in an active region spectrum obtained with the Solar EUV Rocket Telescope and Spectrograph (SERTS)

Theoretical electron-temperature-sensitive Mg IX emission line ratios are presented for R(sub 1) = I(443.96 A)/I(368.06 A), R(sub 2) = I(439.17 A)/I(368.06 A), R(sub 3) = I(443.37 A)/I(368.06 A), R(sub 4) = I(441.22 A)/I(368.06 A), and R(sub 5) = I(448.28 A)/I(368.06 A). A comparison of these with observational data for a solar active region, obtained during a rocket flight by the Solar EUV Rocket Telescope and Spectrograph (SERTS), reveals excellent agreement between theory and observation for R(sub 1) through R(sub 4), with discrepancies that average only 9%. This provides experimental support for the accuracy of the atomic data adopted in the line ratio calculations, and also resolves discrepancies found previously when the theoretical results were compared with solar data from the S082A instrument on board Skylab. However in the case of R(sub 5), the theoretical and observed ratios differ by almost a factor of 2. This may be due to the measured intensity of the 448.28 A line being seriously affected by instrumental effects, as it lies very close to the long wavelength edge of the SERTS spectral coverage (235.46-448.76 A).

Keenan, F. P.↗
NASA NTRS1993

Correlation of He II Lyman alpha with He I 10830 A, and with chromospheric and EUV coronal emission

This paper describes the results of comparing Solar EUV Rocket Telescope and Spectrograph (SERTS-3) images obtained in the transition region line of He II 304 A with chromospheric He I 10830 A absorption; with strong coronal lines of Mg IX 368 A, Fe XV 284 A and 417 A, and Fe XVI 335 A and 31 A; with H-alpha; with Ca II 8542 A; and with magnetograms in Fe I 8688H-alpha. All of the images are illustrated, and the image reconstruction techniques used are described and evaluated. The high correlation of the He II 304 A and He I 10830 A images, originally found by Harvey and Sheeley (1977), is confirmed and is put on a quantitative basis. We find that the supergranulation network has greater contrast, and that filaments appear darker, in 10830 A than in 304 A. In active regions, the 304 A line follows more closely the behavior of H-alpha and Ca II 8542 A than the 10830 A line.

Thompson, W. T.↗
NASA NTRS1993

Solar coronal observations and formation of the He II 304 A line

Although a large body of recent work supports the formation of the He II 304 A resonance line by collisional excitation in the quiet sun, the formation mechanism is less clear in strong coronal active regions and flares. The 1989 May 5 flight of the Goddard Solar Extreme Ultraviolet Rocket Telescope and Spectrograph (SERTS-3) provided a data set that is well suited to addressing this question. This paper develops a method of assessment of the line formation mechanism that is based on simple non-LTE theory and is applied to these data. The results support the conclusion of other authors that the 304 A line is formed by collisional excitation in the quiet sun, but that photoionization-recombination (p-r) may play a significant role in coronal active regions, and that p-r is important, and may even be predominant, in many flares.

Jordan, S. D.↗
NASA NTRS1993

A comparison of theoretical CIV emission line strengths with active region observations obtained with the solar EUV rocket telescope and spectrograph (SERTS)

Theoretical line ratios involving 2s 2S - 3p 2P, 2p 2p - 3s 2S, and 2p 2S - 3d 2D transitions in C IV between 312 and 420 A are presented. A comparison of these with solar active region observational data obtained during a rocket flight by the Solar EUV Rocket Telescope and Spectrograph (SERTS) reveals good agreement between theory and experiment, with discrepancies that average only 22 percent. This provides experimental support for the accuracy of the atomic data adopted in the line ratio calculations, and also resolves discrepancies found previously when the theoretical results were compared with solar data from the S082A instrument on board Skylab. The potential usefulness of the C IV line ratios as electron temperature diagnostics for the solar transition region is briefly discussed.

Keenan, F. P.↗
NASA NTRS1991

Coordinated observations with high resolution spectrographs (HRTS, SERTS, MSDP)

Some of the advantages of coordinated observations with ground-based and space instrumentation in research on prominences are examined. The dynamical behavior of a prominence in transition zone lines (HRTS) and the coronal environment of a filament (SERTS) are discussed. Fe XIV and Si X line ratios were found to be important for NE diagnostic.

Schmieder, B.↗
NASA NTRS1989

The extreme ultraviolet imaging telescope on board SOHO

The design of the multibandpass Extreme-Ultraviolet Imaging Telescope designed for 1996 launch on board the Solar Heliospheric Observatory is described. The telescope will observe simultaneously distinct temperature ranges in the solar corona, defined by well chosen emission lines. Images in four narrow bandpasses at wavelengths ranging from 17 to 31 nm will be obtained using normal-incidence multilayered optics deposited on quadrants of a Ritchey-Chretien telescope. Results are presented on the performances measured on a 2/3 scale mock-up. The bandpasses could be adjusted to better than 1 percent in wavelength.

Delaboudiniere, J. P.↗
NASA NTRS1985

Space Station Spartan study

The required extension, enhancement, and upgrading of the present Spartan concept are described to conduct operations from the space station using the station's unique facilities and operational features. The space station Spartan (3S), the free flyer will be deployed from and returned to the space station and will conduct scientific missions of much longer duration than possible with the current Spartan. The potential benefits of a space station Spartan are enumerated. The objectives of the study are: (1) to develop a credible concept for a space station Spartan; and (2) to determine the associated requirements and interfaces with the space station to help ensure that the 3S can be properly accommodated.

Lane, J. H.↗
NASA NTRS1984

Diagnostic application of highly ionized iron lines in the XUV spectrum of a solar flare

Recent atomic data have been used to analyze a solar flare spectrum obtained with the Goddard Space Flight Center's grating spectrometer on the OSO-5 satellite. There exist in the wavelength region 90-200 A strong lines from each of the ions Fe XVIII-Fe XXIV. The Fe XXI lines can be used as an electron density diagnostic for the 10 to the 7th K plasma. From an analysis of a particular flare, a steep positive slope in the emission measure between 10 to the 6.5th and 10 to the 7.2th K and an electron density of about 4 x 10 to the 11th per cu cm at 10 to the 7th K is found. The need is emphasized for high spectral and spatial resolution observations of solar flares in this wavelength region, which has to date been largely neglected.

Mason, H. E.↗
NASA NTRS1984

Effects of shuttle bay environment on UV sensitive photographic film results of measurements aboard STS-7 and STS-8

Schumann emulsions, having low gelatin content and no protective gelatin overcoating, are extremely sensitive to environmental conditions and handling. Experiments using this emulsion are to be flown on the space shuttle within the cargo-bay. Because the environment of the cargo-bay is unknown, a Get-Away-Special payload was designed to expose Kodak-type SO 652 Schumann emulsion to the residual atmosphere of the cargo-bay. The experiment was programmed to make exposures for various time periods to determine the maximum length of time the film could be exposed in making a measurement and what precautions would be required to preserve the film during ascent into orbit and reentry. The results of the STS-7 and STS-8 flights indicated that long exposures in the shuttle bay do not produce high fog levels in orbit. Observations of severe bleaching of the latent image makes protection of the emulsion during reentry manditory and increase of fog levels with time set a limit of four weeks (preferably less than three) between installation and recovery of the emulsion for processing.

Kreplin, R. W.↗
NASA NTRS1984

Effects of Shuttle bay environment on UV sensitive photographic film - Instrumentation for Get-Away-Special

An account is given of a Get-Away-Special experiment flown on Space Shuttles 7 and 8 investigating the effect of the space environment on Shumann emulsions. Shumann emulsions, having low gelatin content and no protective gelatin overcoating, are useful detectors of ultraviolet radiation shorter than 2200 angstroms but are extremely sensitive to environmental conditions and handling. The instrument required no interface with the Shuttle. It was turned on by an aneroid switch at an altitude of 50,000 feet. After that, its operation was controlled completely by a CMOS digital controller. Each hour, two temperatures and one voltage were read and stored in a CMOS programmable read only memory. At intervals, valves were opened and closed to expose SO 652 film strips of three sensitivities to the cargo bay environment for various time periods. The design and operation of the instrument package is described.

Kreplin, R. W.↗
NASA NTRS1983

A spectroscopic method for calibration of solar extreme ultraviolet instrumentation

A method of calibrating solar extreme ultraviolet spectrographs in space using coronal emission lines of known relative intensity is presented and demonstrated. This approach is useful for recalibrating orbiting instruments that may be subject to degradation during extended periods of operation. The calibration results are insensitive to the physical distribution of emitting plasma in any likely solar coronal source. It is suggested that this technique may be useful for calibration of spectrographs used in the study of laboratory plasmas.

Neupert, W. M.↗
NASA NTRS1983

OSS-1 - A pathfinder mission for space science on Shuttle

On the third Shuttle flight (STS-3), the Orbiter carried a payload of nine scientific instruments. The payload was designated OSS-1 because the program was originaly managed by the Office of Space Science. The OSS-1 objectives are discussed, taking into account the Plasma Diagnostics Package, a study concerned with vehicle charging and potential, the Thermal Canister Experiment, the Solar Flare X-ray Polarimeter, the Solar Ultraviolet Spectral Irradiance Monitor, the study of the influence of weightlessness on lignification in developing plant seedlings, the Microabrasion Foil Experiment, the Contamination Monitor Package, and a study of the characteristics of the Shuttle/Spacelab induced atmosphere. The OSS-1 payload was launched on STS-3 on March 22, 1982.

Neupert, W. M.↗
NASA NTRS1982

Science on the Space Shuttle

On the Space Shuttle's third flight, scientific instruments will study the electromagnetic environment with charging and electron beams. Beam plasma discharge will be studied. The plasma diagnostics package contains electromagnetic and particle sensors to study the ionosphere. An attempt will be made to establish a more accurate base of solar UV irradiance measurements with an absolute error of 10 percent or less over the wavelength region 120-400 nm. The solar flare X-ray polarimeter will observe flare X-rays emitted between 5 and 30 keV and measure their polarization as a function of time and photon energy. A photopolarimeter will help study zodiacal light, and interplanetary dust will be sampled by a section of thick aluminum foil. Plant seedlings will be grown to research the effect of near-zero gravity on lignification. A thermal canister experiment will help determine whether instruments can be maintained at a fixed temperature under varying thermal loads.

Neupert, W. M.↗
NASA NTRS1981

A solar extreme ultraviolet telescope and spectrograph for Shuttle/Spacelab

An instrument for advanced studies of the solar corona is described. Its optical system provides nearly stigmatic imaging of selected portions of the sun over the spectral range from 22.5 to 44.0 nm. Both spectroheliograms and emission line profiles of coronal features will be obtained over a wide range of coronal temperatures.

Neupert, W. M.↗
NASA NTRS1979

The high-temperature corona associated with a loop prominence system

Flare-associated coronal loops were observed on the SE limb of the sun of 1972 February 9 by the Goddard X-ray and EUV spectroheliograph on board OSO 7. The loop structure is clearly visible in the lines of Mg VIII and Mg IX, whereas little or no detail is observed in Fe XV and Fe XVI. A looplike structure with a cloud of emission at the top is observed in soft X-rays. The temperature structure in the region has been calculated from the ratio Fe XVI/Fe XV. The isothermal contour plot is strikingly similar to the isointensity contour plots of the soft X-ray spectroheliograms. With these temperatures and the Fe XV intensity calculated from a calibration scheme developed by Chapman and Neupert, the emission measure has been estimated in the loops. Calculated energy losses suggest that continued deposition of energy is required over the observing period.

Chapman, R. D.↗