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Results for “lobe power”

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 19 records
All sourcesNASA NTRSDOE OSTI
NASA NTRS1994

Evolution of radio galaxies to z = 1

We report Very Large Array (VLA) A-configuration studies of a sample of 49 radio galaxies at redshift less than 1. These were selected with no prior knowledge of their morphology and were chosen to match the redshift and luminosity distribution of a previously studied sample of radio-loud quasars. We compare the radio galaxies with the quasar sample and also with a sample of 29 radio galaxies selected for steep spectrum and double-lobe structure. We find that the radio galaxies have more luminous lobes and mostly weaker cores, and there is no population of one-sided sources associated with the galaxies. The radio galaxies' lobe length ratios and lobe power ratios differ from quasars. The overall sizes of the two types of sources are similar, but the radio galaxies have a 3 times larger upper envelope. The distribution of bend angles is similar but the radio galaxies have fewer very bent and straight sources. We discuss these and other comparisons in detail and suggest that while quasars appear to be viewed within a cone and radio galaxies outside it, the two types of source also have intrinsic differences, and both have individual growth and evolution scenarios. This is supported by previously observed differences in optical properties between the two source types.

Hutchings, J. B.↗
NASA NTRS1983

X-ray observations of 20 3CR radio galaxies and their environs

X-ray observations of 20 3CR radio galaxies using the Imaging Proportional Counter on the Einstein Observatory are reported. Fourteen of the 18 galaxies, plus two sources without optical identification, are detected with soft X-ray luminosities (Lx) ranging from 10 to the 40.9th to 10 to the 44.4th ergs/s. In four of the galaxies there is evidence for extended X-ray structure. Lx is statistically correlated with the radio power of the core, the lobe radio power (especially below 1 GHz), and the steepness of the lobe radio spectrum at high frequencies. The complex interrelations between X-ray luminosities and radio core, radio lobe, optical nuclei, and galaxy clustering are examined; and it is found that a cluster origin of the X-rays provides the best explanation of these effects. Constraints on synchrotron and inverse Compton production of X-rays in radio lobes and on mechanisms of lobe confinement are also discussed.

Feigelson, E. D.↗
NASA NTRS2012

Coded acoustic wave sensors and system using time diversity

An apparatus and method for distinguishing between sensors that are to be wirelessly detected is provided. An interrogator device uses different, distinct time delays in the sensing signals when interrogating the sensors. The sensors are provided with different distinct pedestal delays. Sensors that have the same pedestal delay as the delay selected by the interrogator are detected by the interrogator whereas other sensors with different pedestal delays are not sensed. Multiple sensors with a given pedestal delay are provided with different codes so as to be distinguished from one another by the interrogator. The interrogator uses a signal that is transmitted to the sensor and returned by the sensor for combination and integration with the reference signal that has been processed by a function. The sensor may be a surface acoustic wave device having a differential impulse response with a power spectral density consisting of lobes. The power spectral density of the differential response is used to determine the value of the sensed parameter or parameters.

Solie, Leland P.↗
NASA NTRS1990

Ultra-low-frequency wave power in the magnetotail lobes. I - Relation to substorm onsets and the auroral electrojet index

Time-series observations of the magnetotail-lobe magnetic field have been Fourier analyzed to compute the frequency-weighted energy density Pfz in the range 1-30 mHz. Pfz is generally observed in the range 0.0001-0.01 gamma-squared Hz with a mean value of 0.0012 during substorm growth phases and 0.001 in the comparison intervals. No strong correlation of Pfz is found with the auroral electrojet index in either set of intervals, but during substorm growth phases Pfz may vary by an order of magnitude over time scales of 30 min, with a tendency for higher power levels to occur later in the growth phase. Increases in Pfz precede by about 10 min localized expansive phase activity observed in individual magnetograms.

Smith, R. A.↗
NASA NTRS1982

A new SPS antenna design to reduce grating lobes

In the Solar Power Satellite system, the antenna's misalignment will produce well defined grating lobes. These gratings lobe peaks occur every 440 km and are potentially hazardous to the environment. One way to suppress these peaks is to phase control every power module. The cost due to the increase in receiving electronics and processors, however, could prove to be prohibitive. A new design of the antenna involving the addition of two broad gaps, one along the x axis and another along the y axis is proposed. The gap distance is exactly one half of the distance between the center of two neighboring subarrays. Calculation of far field radiation patterns shows that the design reduces grating lobe peaks without sacrificing power in the main lobe.

Chan, C. H.↗
NASA NTRS1994

Search for inverse Compton x-rays from the lobes of Fornax A x-rays from radio galaxies straddling the Fanaroff-Riley transition

Two related studies of radio galaxies are covered in this report. The first is a search for inverse Compton x-rays from the lobes of Fornax A. In this study, a ROSAT position sensitive proportional counter image of Fornax A (NGC 1316) is presented, and after image processing, it was observed that the x-ray emission closely mimicked the radio emission. A second study involved x-rays from radio galaxies straddling the Fanaroff-Riley transition which divides radio galaxies into two broad morphological groups based on whether the lobe radio power is greater or less than a critical value. ROSAT HRI observations were obtained from four bright radio galaxies around the transition to search for x-ray indications of either nuclear engine or ambient medium differences.

Feigelson, Eric D.↗
NASA NTRS1982

Grating lobe characteristics and associated impacts upon the solar power satellite microwave system

The object of this investigation is to determine the grating lobe characteristics for the SPS (solar power satellite) microwave power beam. Using techniques of Fourier array decomposition, equations, and numerical results are given for the complete SPS microwave antenna pattern (main beam plus grating lobes). In order to ensure the grating lobe peaks are below the environmental guideline of 0.01 mW/sq cm, constraints are defined for the mechanical alignment (tilt) of the SPS antenna and the satellite attitude control system. Two conditions, phase control to the subarray level and to the power module (tube) level, are analyzed as to their effects upon grating lobes.

Kerwin, E. M.↗
NASA NTRS1988

Low-noise interferometer for microwave radiometry

An interferometer for precision measurements in microwave radiometry is proposed which uses two low-noise heterodyne receivers based on SIS tunnel junction mixers in the 40-50-GHz band. The antenna interference pattern has lobes which lead to positive output signals and lobes which give negative output, and the radiometer measures the difference in the power from these lobes without beam switching or instrument motion. The present system cancels instrumental signals, has a very low 1/f noise in the output, and has a zero outpus signal when viewing a uniform source. It is noted that application of the interferometer may be limited to radiometry with relatively large beams.

Timbie, P. T.↗
NASA NTRS1992

Ultralow frequency waves in the magnetotails of the earth and the outer planets

Ultralow frequency waves with periods greater than two minutes are characteristic features of planetary magnetotails. At Jupiter, changes in the wave characteristics across the boundary between the plasma sheet and the lobe have been used to identify this important plasma boundary. In the terrestrial lobes the wave amplitude can be relatively large, especially during intervals of intense geomagnetic activity. The wave power seen in the lobes of the magnetotails of the earth, Jupiter, Saturn and Uranus is evaluated to evaluate a proposal by Smith et al. that the propagating waves generated by the Kelvin-Helmholtz instability on the magnetopause can heat the plasma through a resonant absorption of these waves. The results indicate that the wave power in the lobes is generally small and can be easily understood in the framework of coupled MHD waves generated in the plasma sheet.

Khurana, Krishan K.↗
NASA NTRS1989

Phase-front measurements of an injection-locked AlGaAs laser-diode array

The phase-front quality of the primary spatial lobe emitted from an injection-locked gain-guided AlGaAs laser-diode array is measured by using an equal-path, phase-shifting Mach-Zehnder interferometer. Root-mean-square phase errors of 0.037 + or - 0.003 wave are measured for the single spatial lobe, which contained 240-mW cw output power in a single longitudinal mode. This phase-front quality corresponds to a Strehl ratio of S = 0.947, which results in a 0.23-dB power loss from the single lobe's ideal diffraction-limited power. These values are comparable with those measured for single-stripe index-guided AlGaAs lasers.

Cornwell, Donald M., Jr.↗
NASA NTRS1993

Development of simplified external control techniques for broad area semiconductor lasers

The goal of this project was to injection lock a 500 mW broad area laser diode (BAL) with a single mode low power laser diode with injection beam delivery through a single mode optical fiber (SMF). This task was completed successfully with the following significant accomplishments: (1) injection locking of a BAL through a single-mode fiber using a master oscillator and integrated miniature optics; (2) generation of a single-lobed, high-power far-field pattern from the injection-locked BAL that steers with drive current; and (3) a comprehensive theoretical analysis of a model that describes the observed behavior of the injection locked oscillator.

Davis, Christopher C.↗
NASA NTRS1989

Radio emission and the hot interstellar medium of early-type galaxies

The results of an analysis of a sample of 84 elliptical and S0 galaxies, observed in X-rays with the Einstein Observatory and in radio continuum at 5 GHz, are reported. Radio flux densities result in some of the lowest radio powers yet reported for early-type galaxies. Radio structures extending beyond the optical radius are found only in galaxies with 5 GHz radio power greater than about 10 exp 29.5 ergs/s/Hz. Radio and X-ray luminosities are correlated, although with large intrinsic scatter, suggesting that more than one mechanism may be involved. A correlation between core radio power and the X-ray-to-optical ratio suggests a connection between the hot ISM and nuclear radio sources and points to accreting cooling flows as the fuel for the radio sources. For the same radio core power, extended radio lobes tend to be associated with galaxies with relatively smaller X-ray-to-optical ratios, pointing to the importance of the hot ISM in disrupting the radio jets and confining extended radio structures.

Fabbiano, G.↗
NASA NTRS1991

The dust enshrouded quasar in the ultraluminous galaxy Markarian 463 - Radio, near-infrared, and optical imaging

New imaging data are presented at radio, near-infrared, and optical wavelengths to elucidate the processes associated with the ongoing merger and nuclear activity in Mrk 463. Imaging at 20 cm reveals previously unknown components 4 arcsec north and 18 arcsec south of Mrk 463E, and a source 10 arcsec to the northwest which is believed to be linked to the nuclear region. The western nucleus, Mrk 463W, was detected at 6 and 20 cm; it has a radio luminosity comparable to that of a moderately luminous Seyfert galaxy or a highly luminous starburst galaxy. Near-infrared images at wavelengths less than 2.3 microns show the two nuclei; only Mrk 463E has been detected at 3.7 microns. Brightness profiles of Mrk 463E are unresolved at K and L-prime, but extended at J. It is inferred from the fact that radio continuum components 4-18 kpc from the nucleus are aligned with previously known 0.05-1.5 kpc radio structure and extended conical O-III forbidden omission lines that Mrk 463E is powering weak radio lobes and therefore exemplifies a transition between the confined linear sources in Seyfert galaxies and the extended lobes in classical quasars and radio galaxies.

Mazzarella, J. M.↗
NASA NTRS1992

Choice of antenna geometry for microwave power transmission from solar power satellites

A comparison is made between square and circular transmitting antennas for solar power satellite microwave power transmission. It is seen that the exclusion zone around the rectenna needed to protect populations from microwaves is smaller for a circular antenna operating at 2.45 GHz than it is for a square antenna at that frequency. If the frequency is increased, the exclusion zone size remains the same for a square antenna, but becomes even smaller for a circular antenna. Peak beam intensity is the same for both antennas if the frequency and antenna area are equal. The circular antenna puts a somewhat greater amount of power in the main lobe and somewhat less in the side lobes. Since rain attenuation and atmospheric heating remain problems above 10 GHz, it is recommended that future solar power satellite work concentrate on circular transmitting antennas at frequencies of roughly 10 GHz.

Potter, Seth D.↗
NASA NTRS2018

Simultaneous Optical and Dual-Frequency Radar Observations of Small Mass Meteors at Arecibo

We present simultaneous optical and radar observations of meteors observed over the Arecibo radar in Puerto Rico. These observations were obtained during ~24 h of radar time over 3 different nights in May 2012. The radar was operating in a dual-frequency mode at 430 MHz (UHF) and 46.8 MHz (VHF). The optical observations were made at 41 frames per second with an Andor Electron Multiplying CCD camera with a field of view of ~6, enabling the determination of accurate horizontal meteor velocities and optical light curves. There are varying detection sensitivities of the 3 different techniques (2 radar, 1 optical). The UHF radar is the most sensitive, resulting in a total of 8710 detected meteors during that period, while the VHF radar is significantly less sensitive— resulting in only 278 detected meteors. The optical observations are the least sensitive, resulting in a total of 178 detections. Of all of these meteors, only 19 were simultaneously detected by the 3 instruments. This paper focuses on the analysis of these 19 common events. The meteoroid masses determined from the optical light curves were found to be in the range of 20 μg to 1.2 mg and did not correlate with the maximum Signal-to-Noise Ratio (SNR) of either radar. In addition, the UHF radar detected 5 out of these 19 meteors with far side-lobes, beyond the main-beam and first side-lobe. This indicates that a significant fraction of events detected by the UHF radar could be in far side lobes and therefore have significantly underestimated Radar Cross Sections (RCS), given the smaller backscattered powers received in the side lobes.

Arecibo Observatory↗
NASA NTRS1993

Coherent summation of saturated AlGaAs amplifiers

Coherent summation of the output of two saturated traveling-wave amplifiers, each injected from a common semiconductor laser and all operated CW, has resulted in a single diffraction-limited beam containing 93 percent of the power originally contained in the two individual amplified beams. The 372 mW of power in a single diffraction-limited lobe is a 1.5-fold enhancement over the power available from a single amplifier.

Schuster, Gregory L.↗
NASA NTRS1980

System performance conclusions

The advantages and disadvantages of reducing power levels and using antennas with diameters smaller than 1 Km were evaluated if rectenna costs and land usage requirements become major factors, operating at 5800 megahertz should be considered. Three sequences (random, incoherent phasing, and concentric rings - center to edge) provided satisfactory performance in that the resultant sidelobe levels during startup/ shutdown were lower than the steady-state levels present during normal operations. Grating lobe peaks and scattered power levels were used to determine the array/subarray mechanical alignment requirements. The antenna alignment requirement is 1 min or 3 min depending on phase control configuration. System error parameters were defined to minimize scattered microwave power.

Arndt, G. D.↗