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  • 1
    ISSN: 1573-5036
    Keywords: acetylene reduction ; grain yield ; N difference ; N2 fixation ; 15N-isotope dilution ; nodule ; Rhizobium ; selection parameters ; total N
    Source: Springer Online Journal Archives 1860-2000
    Topics: Agriculture, Forestry, Horticulture, Fishery, Domestic Science, Nutrition
    Notes: Abstract Most of the production of lentil (Lens culinaris) on the Great Plains occurs on soils that are free of indigenous Rhizobium leguminosarum. Inoculation is required to increase yields through N2 fixation. A screening program to evaluate the effectiveness of R. leguminosarum strains for lentil was initially carried out under controlled environments followed by an evaluation under field conditions. In two separate growth room experiments, the effectiveness of 185 and 24 different strains of R. leguminosarum were tested for Laird and Eston lentil. Significant differences between strains in number of nodules, shoot weight and nitrogenase activity (acetylene reduction activity, ARA) were found for lentil grown for 5 weeks. When lentil were grown for 7 weeks, significant differences between strains in number of nodules, total plant weight, total N, and % N were observed. Fourteen strains plus Nitragin ‘C’ inoculant were selected for further field testing on Eston and Laird lentil at two locations in 1986 and one site in 1987. Inoculation increased yield up to 135%. Percent Ndfa and total N2 fixed ranged from 0 to 76 and 0 to 105 kg ha-1, respectively. N2-fixing activity was site specific and higher spring soil NO3-levels resulted in lower N2-fixing activity. Depending on site and growing conditions, strains 99A1 and I-ICAR-SYR-Le20 appeared to be superior to the other strains tested. A good agreement was found between the estimates for N2 fixation based upon the 15N-isotope dilution and the classical N difference methods. Number of nodules, dry weight of nodules and ARA of Eston and Laird lentil grown under growth room conditions failed to show positive correlations with total dry matter production, total N or total N2 fixed of field grown lentil. However, total plant weight and total N of lentil grown under growth room conditions were highly correlated with field parameters, and were the most reliable screening parameters for the selection of superior rhizobial strains.
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  • 2
    ISSN: 1573-5036
    Keywords: acetylene reduction ; grain yield ; N difference ; N2 fixation ; 15N-isotope dilution ; nodule ; Rhizobium ; selection parameters ; total N
    Source: Springer Online Journal Archives 1860-2000
    Topics: Agriculture, Forestry, Horticulture, Fishery, Domestic Science, Nutrition
    Notes: Abstract Most of the production of lentil (Lens culinaris) on the Great Plains occurs on soils that are free of indigenousRhizobium leguminosarum. Inoculation is required to increase yields through N2 fixation. A screening program to evaluate the effectiveness ofR. leguminosarum strains for lentil was initially carried out under controlled environments followed by an evaluation under field conditions. In two separate growth room experiments, the effectiveness of 185 and 24 different strains ofR. leguminosarum were tested for Laird and Eston lentil. Significant differences between strains in number of nodules, shoot weight and nitrogenase activity (acetylene reduction activity, ARA) were found for lentil grown for 5 weeks. When lentil were grown for 7 weeks, significant differences between strains in number of nodules, total plant weight, total N, and % N were observed. Fourteen strains plus Nitragin ‘C’ inoculant were selected for further field testing on Eston and Laird lentil at two locations in 1986 and one site in 1987. Inoculation increased yield up to 135%. Percent Ndfa and total N2 fixed ranged from 0 to 76 and 0 to 105 kg ha-1, respectively. N2-fixing activity was site specific and higher spring soil NO3-levels resulted in lower N2-fixing activity. Depending on site and growing conditions, strains 99A1 and I-ICAR-SYR-Le20 appeared to be superior to the other strains tested. A good agreement was found between the estimates for N2 fixation based upon the15N-isotope dilution and the classical N difference methods. Number of nodules, dry weight of nodules and ARA of Eston and Laird lentil grown under growth room conditions failed to show positive correlations with total dry matter production, total N or total N2 fixed of field grown lentil. However, total plant weight and total N of lentil grown under growth room conditions were highly correlated with field parameters, and were the most reliable screening parameters for the selection of superior rhizobial strains.
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  • 3
    Publication Date: 2019-07-17
    Description: The determination of the radial and latitudinal temperature and wind profiles of the solar corona is of great importance in understanding the coronal heating mechanism and the dynamics of coronal expansion. Cram presented the theory for the formation of the K-coronal spectrum and identified two important observations. He observed the existence of temperature sensitive anti-nodes at certain wavelengths in the theoretical K-coronal spectra. The anti-nodes are separated by temperature-insensitive nodes. Remarkably, Cram showed that the wavelengths of the nodes and anti-nodes are almost independent of altitude above the solar limb. Because of these features, Cram suggested that the intensity ratios at two anti-nodes could be used as a diagnostic of the electron temperature in the K-corona. Based on this temperature diagnostic technique prescribed by Cram a slit-based spectroscopic study was performed by Ichimoto et al. on the solar corona in conjunction with the total solar eclipse of 3 Nov 1994 in Putre, Chile to determine the temperature profile of the solar corona. In this thesis Cram's theory has been extended to incorporate the role of the solar wind in the formation of the K-corona, and we have identified both temperature and wind sensitive intensity ratios. The instrument, MACS, for Multi Aperture Coronal Spectrometer, a fiber optic based spectrograph, was designed for global and simultaneous measurement of the thermal electron temperature and the solar wind velocity in the solar corona. The first ever experiment of this nature was conducted in conjunction with the total solar eclipse of 11 Aug 1999 in Elazig, Turkey. In this instrument one end of each of twenty fiber optic tips were positioned in the focal plane of the telescope in such a way that we could observe conditions simultaneously at many different latitudes and two different radial distances in the solar corona. The other ends of the fibers were vertically aligned and placed at the primary focus of the collimating lens of the spectrograph to obtain simultaneous and global spectra on the solar corona. By isolating the K-coronal spectrum from the spectrum recorded by each fiber the temperature and the wind sensitive intensity ratios were calculated to obtain simultaneous and global measurements of the thermal electron temperature and the solar wind velocity. We were successful in obtaining reliable estimates of the coronal temperature at many positions in the corona. This is the first time that simultaneous measurements of coronal temperatures have been obtained at so many points. However due to instrumental scattering encountered during observations, reliable estimates of the wind velocity turned out to be impossible to obtain. Although remedial measures were taken prior to observation, this task proved to be difficult owing to the inability to replicate the conditions expected during an eclipse in the laboratory. The full extent of the instrumental scattering was apparent only when we analyzed the observational sequence. Nevertheless the experience obtained from this very first attempt to simultaneously and globally measure both the wind velocity and the temperature on the solar corona have provided valuable information to conduct any future observations successfully.
    Keywords: Solar Physics
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  • 4
    Publication Date: 2019-08-14
    Description: An experiment was conducted in conjunction with the total solar eclipse on 29 March 2006 in Libya to measure both the electron temperature and its flow speed simultaneously at multiple locations in the low solar corona by measuring the visible K-coronal spectrum. Coronal model spectra incorporating the effects of electron temperature and its flow speed were matched with the measured K-coronal spectra to interpret the observations. Results show electron temperatures of (1.10 +/- 0.05) MK, (0.70 +/- 0.08) MK, and (0.98 +/- 0.12) MK, at 1.1 Solar Radius from Sun center in the solar north, east and west, respectively, and (0.93 +/- 0.12) MK, at 1.2 Solar Radius from Sun center in the solar west. The corresponding outflow speeds obtained from the spectral fit are (103 +/- 92) km/s, (0 + 10) km/s, (0+10) km/s, and (0+10) km/s. Since the observations were taken only at 1.1 Solar Radius and 1.2 Solar Radius from Sun center, these speeds, consistent with zero outflow, are in agreement with expectations and provide additional confirmation that the spectral fitting method is working. The electron temperature at 1.1 Solar Radius from Sun center is larger at the north (polar region) than the east and west (equatorial region).
    Keywords: Solar Physics
    Type: GSFC.JA.00284.2012 , Solar Physics; 270; 235-251
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  • 5
    Publication Date: 2019-08-14
    Description: An experiment to measure the electron temperature and flow speed in the solar corona by observing the visible K-coronal spectrum was conducted during the total solar eclipse on 29 March 2006 in Libya. New corona1 models accounting for the effect of electron temperature and flow on the resulting K-corona spectrum were used to interpret the observations. Results show electron temperatures of 1.10 +/- 0.05, 0.98 +/- 0.12, and 0.70 +/- 0.08 MK, at l.l{\it R)$-{\odot)$ in the solar north, east and west, respectively, and 0.93 +/- 0.12 MK, at 1.2 R(sub sun) in the solar east. The corresponding outflow speeds obtained from the spectral fit are 103 +/- 92, 0 + 10, 0 + 10, and 0 + 10 km/s. Since the observations are taken only at 1.1 and 1.2 R(sub sun) these velocities , consistent with zero outflow, are in agreement with expectations and provide additional confirmation that the spectral fitting method is working.
    Keywords: Solar Physics
    Type: American Geophysical Union Meeting; Dec 14, 2008 - Dec 17, 2008; San Francisco, CA; United States
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  • 6
    Publication Date: 2019-07-13
    Description: We examine the uncertainties in two plasma parameters from their true values in a simulated asymmetric corona. We use the Corona Heliosphere (CORHEL) and Magnetohydrodynamics Around the Sphere (MAS) models in the Community Coordinated Modeling Center (CCMC) to investigate the differences between an assumed symmetric corona and a more realistic, asymmetric one. We were able to predict the electron temperatures and electron bulk flow speeds to within +/-0.5 MK and +/-100 km s(exp1), respectively, over coronal heights up to 5.0 R from Sun center.We believe that this technique could be incorporated in next-generation white-light coronagraphs to determine these electron plasma parameters in the low solar corona. We have conducted experiments in the past during total solar eclipses to measure the thermal electron temperature and the electron bulk flow speed in the radial direction in the low solar corona. These measurements were made at different altitudes and latitudes in the low solar corona by measuring the shape of the K-coronal spectra between 350 nm and 450 nm and two brightness ratios through filters centered at 385.0 nm/410.0 nm and 398.7 nm/423.3 nm with a bandwidth of is approximately equal to 4 nm. Based on symmetric coronal models used for these measurements, the two measured plasma parameters were expected to represent those values at the points where the lines of sight intersected the plane of the solar limb.
    Keywords: Solar Physics
    Type: GSFC-E-DAA-TN22852 , Solar Physics; 289; 6; 2021-2039
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  • 7
    Publication Date: 2019-07-13
    Description: We conducted an experiment in conjunction with the total solar eclipse of 1 August 2008 in China to determine the thermal electron temperature in the low solar corona close to the solar limb. The instrument, Imaging Spectrograph of Coronal Electrons (ISCORE), consisted of an 8 inch f/10 Schmidt Cassegrain telescope with a thermoelectrically cooled CCD camera at the focal plane. Results are electron temperatures of 1 MK at 1.08 R(solar system) and 1.13 R(solar system) from the Sun center in the polar and equatorial regions, respectively. This experiment confirms the results of an earlier experiment conducted in conjunction with the total eclipse of 29 March 2006 in Libya, and results are that at a given coronal height the electron temperature in the polar region is larger than at the equatorial region. In this paper we show the importance of using the correct photospheric spectrum pertinent to the solar activity phase at the time of the experiment, which is a required parameter for modeling the underlying theoretical concept for temperature interpretation of the measured intensity ratios using color filters.
    Keywords: Solar Physics
    Type: GSFC-E-DAA-TN53822 , Journal of Geophysical Research: Space Physics (ISSN 2169-9380) (e-ISSN 2169-9402); 122; 6; 5856-5869
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  • 8
    Publication Date: 2019-07-13
    Description: Three-dimensional electron density distributions in the solar corona are reconstructed for 100 Carrington rotations (CR 2054 - 2153) during 2007/03 - 2014/08 using the spherically symmetric method from polarized white-light observations with the inner coronagraph (COR1) onboard the twin Solar Terrestrial Relations Observatory (STEREO). These three-dimensional electron density distributions are validated by comparison with similar density models derived using other methods such as tomography and a magnetohydrodynamics (MHD) model as well as using data from the Solar and Heliospheric Observatory (SOHO)/Large Angle and Spectrometric Coronagraph (LASCO)-C2. Uncertainties in the estimated total mass of the global corona are analyzed based on differences between the density distributions for COR1-A and -B. Long-term variations of coronal activity in terms of the global and hemispheric average electron densities (equivalent to the total coronal mass) reveal a hemispheric asymmetry during the rising phase of Solar Cycle 24, with the northern hemisphere leading the southern hemisphere by a phase shift of 7 - 9 months. Using 14 CR (approx. equal to 13-month) running averages, the amplitudes of the variation in average electron density between Cycle 24 maximum and Cycle 23/24 minimum (called the modulation factors) are found to be in the range of 1.6 - 4.3. These modulation factors are latitudinally dependent, being largest in polar regions and smallest in the equatorial region. These modulation factors also show a hemispheric asymmetry: they are somewhat larger in the southern hemisphere. The wavelet analysis shows that the short-term quasi-periodic oscillations during the rising and maximum phases of Cycle 24 have a dominant period of 7 - 8 months. In addition, it is found that the radial distribution of the mean electron density for streamers at Cycle 24 maximum is only slightly larger (by approx. equal to 30%) than at cycle minimum.
    Keywords: Solar Physics
    Type: GSFC-E-DAA-TN50924 , Solar Physics (ISSN 0038-0938) (e-ISSN 1573-093X); 292; 97
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