Engineering topics

Gergely, T. E.

Publications and source records attributed to Gergely, T. E..

26 records · Page 2

NASA NTRS1977

The spectrum and position of solar noise storms at decameter wavelengths

Decametric storm radiation during the period July-August 1970 has been observed simultaneously with a high sensitivity spectrograph at Arecibo Observatory and with the log-periodic, swept-frequency array of the Clark Lake Radio Observatory. The observations complement each other; different types of fine structure emissions can be easily identified on the spectrograph records and their position can be determined from the swept-frequency recordings. The relative positions of the different emissions which have been observed during the storms are studied. Four distinct sources appear to be present. The continuum emission, the type I bursts and the flare-related type III's are all emitted at different locations. The storm type III bursts, type IIIb's and drift pairs overlap in position, but appear at different locations than the previously mentioned sources.

De La Noe, J.↗

NASA NTRS1977

A new determination of the gas-to-dust ratio in M31

The mean gas-to-dust ratio in M31 is derived from observations of the H I column density and the color excess in the direction of 121 globular clusters. The angular resolution of the H I observations obtained with the Westerbork Synthesis Radio Telescope is comparable to the angular sizes of individual globular clusters. The mean gas-to-dust ratio turns out to be approximately 33 by 10 to the 20th power atoms/sq cm per magnitude; the value depends on radial distance from the center of the galaxy. Some effects that may influence the determination are discussed.

Bajaja, E.↗

NASA NTRS1977

Determination of the decameter wavelength spectrum of the quiet sun

The Teepee Tee array of the Clark Lake Radio Observatory has been used to compare the flux of the Sun with that of the sidereal sources Tau A and Vir A at several frequencies in the range 109.0-19.0 MHz. Only the two central banks of the E-W arm of the array were used as elements of a phase switched interferometer so that the Sun could be observed as a point source and compared directly to the sidereal sources. The Sun was still partially resolved however, and appropriate corrections for this effect were made. The observations were taken at times when the Sun and either Tau A or Vir A were at the same declination. We have therefore been able to derive the values for the solar flux, without having to resort to a gain vs zenith distance correction. The observations, combined with those available in the literature, allow us to derive an accurate meter and decameter wavelength spectrum of the quiet Sun.

Erickson, W. C.↗

NASA NTRS1977

Observations of the quiet sun at meter and decameter wavelengths

The new TeePee Tee array of the Clark Lake Radio Observatory has been used to observe the quiet sun at 121.5, 73.8 and 26.3 MHz. The equatorial brightness distributions at all three frequencies, and the polar brightness distributions at the two higher ones have been measured. From the observed total fluxes and half-power diameters we have derived the peak brightness temperatures of the solar disk as well as of some sources of the slowly varying component.

Kundu, M. R.↗

NASA NTRS1976

A decameter type II burst associated with a behind-the-limb flare

The characteristics of a decametric type II burst associated with a possible behind-the-limb flare are discussed. The burst source had an unusually high velocity. Assuming that the disturbance propagated as an MHD wave, the magnetic field strength at the 40-MHz plasma level is estimated to be 5.6 gauss.

Gergely, T. E.↗

NASA NTRS1975

Decameter storm radiation. I

A description is given of the evolution of six decametric storms which took place during the period from January to August, 1971. The storms described were observed with a swept frequency interferometer. The array consists of sixteen log-periodic antennas, equally spaced on a two mile east-west baseline. The association of storms with optical activity and photospheric fields is considered along with the relation of decametric storms to coronal magnetic fields and the association of storms with decimeter and meter wavelength activity. It is shown that decametric storms are always associated with storms at the meter and decimeter wavelengths.

Gergely, T. E.↗

NASA NTRS1975

Decameter storm radiation. II

The height, size, directivity, and lifetime of decametric storm sources are investigated. The height of the continuum sources is determined from the rotation rate, and the gradient of electron density for the regions of storm origin is computed by assuming that the radiation originates at the plasma frequency. The mean angular size of the sources is found to be quite large (increasing with decreasing frequency), the storm continuum is strongly directive toward the disk center, and east-west asymmetry is observed at decameter wavelengths. Two distinct classes of type III bursts are observed during storms: 'off-fringe' (displaced in position from the continuum source) and 'on-fringe' (coinciding in position with the continuum). A model of the storm region is proposed in which the 'on-fringe' bursts originate in regions of diverging field lines above closed magnetic loops and the 'off-fringe' bursts are excited by energetic electron streams having access to open field lines at the base of the loops.

Gergely, T. E.↗

NASA NTRS1974

Decameter type IV bursts associated with coronal transients

The characteristics of four moving type IV burst observed with a 65- to 20-MHz swept-frequency interferometer are discussed. All four bursts were associated with depletions in the electron content of the white light corona. Characteristics of the bursts are not unique i.e., they differ in source size, structure, duration, and their association with other radio bursts. Following Smerd and Dulk (1971), it is assumed that a shock wave, moving out from the flare site is responsible for the expansion of a magnetic arch or the ejection of a plasmoid which is observed as the usual type IV burst. Behind the shock wave, the compressed coronal gas moves outward, and as it expands it causes a depletion of electrons in the inner corona. After the passage of the shock wave, sometimes the coronal magnetic field structure is restored to its initial situation, as evidenced by the observation of homologous transients.

Gergely, T. E.↗