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  • 1
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    Role of solar flare index in long term modulation of cosmic ray intensity (1985)
    In:  CASI
    Details
    Publication Date: 2019-06-28
    Description: Recently, the importance of the occurrence of solar flares in the long-term modulation of cosmic ray intensity has been re-emphasized. For this purpose, the data of solar flares have been used from various publications, such as Solar Geophysical Data books, U.A.G. reports and Quarterly Bulletin Of Solar Activity. Research very clearly reveals that even the periodic changes in the solar flare observations, obtained from the four different data sources, for the same interval, differ significantly from one another; this is evidenced even on an average basis. Hence, in any study using solar flares, the importance of selecting a single compilation of the solar-flare data for the entire period of investigation is stressed.
    Keywords: SPACE RADIATION
    Type: SH-4.4-12 , 19th Intern. Cosmic Ray Conf - Vol. 5; p 63-66; NASA-CP-2376-VOL-5
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  • 2
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    Pulsed emission of TeV gamma rays from Vela pulsar (1985)
    In:  CASI
    Details
    Publication Date: 2016-06-11
    Description: The Ooty atmospheric Cerenkov array, consisting of 10 parabolic mirrors of 0.9 m diameter and 8 of 1.5 m diameter, was used for observations on the Vela pulsar to see if it emits gamma rays in the TeV energy range. During the winter of 1984-85, the array was split into two parts: (1) consisting wholly of the smaller mirrors, and (2) wholly of the bigger mirrors. The two arrays were operated at two different sites to distinguish a marginally significant genuine pulsar signal from spurious signals produced trivially by chance fluctuations in the background rates. All the mirrors were pointed at the celestial object to track it for durations of the order of 1 to 6 hours during clear moonless nights. The event time data is analyzed to detect a possible pulsed emission of TeV gamma rays using the contemporaneous pulsar elements on the basis of their radio observations on the Vela pulsar. Results from the analyses of observations made during the winters of 1982-83 and 1984-85 on steady pulsed emission and on possible transient emission is presented.
    Keywords: SPACE RADIATION
    Type: 19th Intern. Cosmic Ray Conf - Vol. 1; p 159-160; NASA-CP-2376-VOL-1
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  • 3
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    Search for gamma rays of energy 10(15) eV from Cygnus X-3 (1985)
    In:  CASI
    Details
    Publication Date: 2019-06-28
    Description: Finite flux of excess radiation of energy 10 to the 15th power has been reported by two groups from the direction of Cygnus X-3, with the characteristic periodicity of 4.8 hrs. Samorski and Stamm find that the muon content of the showers generated by this excess radiation is about 77% of that in normal cosmic ray showers, whereas the expectation for gamma ray showers is less than 10%. It is thus difficult to understand the nature of the radiation arriving from the direction of Cygnus X-3. Samorski and Stamm measured the muon densities close to the core (approx. 10 m), where contamination due to other components is severe. Even though this does not explain the high ratio of muon densities, measurements should be carried out away from the core to establish the nature of the radiation. In order to establish the signal from Cygnus X-3 and its muon content with better statistical significance, an extensive air shower array, specifically designed for this purpose was operated at Kolar Gold Fields (longitude: 78 deg .3 E; latitude: + 12 deg .95; atmospheric depth: 920 q/square centimeters) since September, 1984. The details of the array and the accuracy of arrival direction measurements are discussed.
    Keywords: SPACE RADIATION
    Type: OG-2.1-1 , 19th Intern. Cosmic Ray Conf - Vol. 1; p 59-61; NASA-CP-2376-VOL-1
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  • 4
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    Cosmic ray intensity distribution perpendicular to solar equatorial plane at 1 A.U. during 1978-83 (1985)
    In:  CASI
    Details
    Publication Date: 2019-06-28
    Description: The distribution of cosmic ray intensity perpendicular to solar equatorial plane, was investigated by using its yearly variation with respect to the heliolatitudinal position of the Earth, for the two intervals 1978 to 1980 and 1981 to 1983. The monthly mean values of two high latitude stations along with the solar and geomagnetic indices are used to derive the cosmic ray intensity distribution free from the changes due to variation in solar activity. The correction is found to be significant only during the interval 1976 to 1980. The results indicate a significant linear increase in cosmic ray intensity from north to south of solar equator, contrary to that observed during 1973 to 1975. No symmetrical gradients are found during the period of study, in agreement with earlier results.
    Keywords: SPACE RADIATION
    Type: SH-4.3-14 , 19th Intern. Cosmic Ray Conf - Vol. 5; p 23-26; NASA-CP-2376-VOL-5
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  • 5
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    The Figaro experiment for the observation of time marked sources in the low energy gamma-ray range (1985)
    In:  CASI
    Details
    Publication Date: 2019-06-28
    Description: The only two firmly identified galactic gamma-ray sources in the second COS B catalogue are the pulsars PSR 0531+21 (Crab) and PSR 0833-45 (Vela). In the region between 100 keV and 10 MeV the detailed shape of the emission is particularly important, since one expects a turn-off which is related to geometry of the source. A marginal evidence of such a turn-off just below 1 MeV has been reported for the Vela pulsar. In order to study sources with a well marked time signature in this energy band, the FIGARO - French Italian Gamma Ray Observatory was designed. The first version was launched in November 1983 from the Sao Manuel base (Brazil), and was destroyed in a free fall following a balloon burst at an altitude of 50 mbar. A brief description is given of the new improved version of the experiment, FIGARO 2, which is nearly completed and whose launch is scheduled before summer 1986.
    Keywords: SPACE RADIATION
    Type: OG-9.2-11 , 19th Intern. Cosmic Ray Conf - Vol. 3; p 334-337; NASA-CP-2376-VOL-3
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  • 6
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    Search for TeV gamma rays from extragalactic sources and the Galactic Center (1985)
    In:  CASI
    Details
    Publication Date: 2019-06-28
    Description: The Ooty atmospheric Cerenkov array was used in 1982-83 to see if the galactic center and the extra-galactic sources 3C 273, Centaurus A emit gamma rays at TeV energies. The ON/OFF method was used wherein the source was tracked for 16 minutes and immediately afterwards, a background region in the same zenith angle range was tracked for the next 16 minutes. Data were taken for approx 15 hours (55 scans) on 3C273, approx 7 hours (26 scans) on Cen A and 5 hours (19 scans) on galactic center. A preliminary analysis involving direct comparison of total rates on and off the source shows no significant excess from any of these orbits. Results of detailed analysis using different energy thresholds are presented.
    Keywords: SPACE RADIATION
    Type: OG-2.7-1 , NASA. Goddard Space Flight Center 19th Intern. Cosmic Ray Conf., Vol. 1; p 263
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  • 7
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    All sky Northern Hemisphere 10(15) EV gamma-ray survey (1985)
    In:  CASI
    Details
    Publication Date: 2019-06-28
    Description: Flux limits in the range 10 to the minus 13th power-10 to the minus 12 power/sq cm/s have been obtained by observing Cerenkov flashes from small air showers. During 1983, a 3.5 sigma excess of showers was observed during the phase interval 0.2 to 0.3 of the 4.8h period of Cygnus X-3, but no excess was found in 1984 observations.
    Keywords: SPACE RADIATION
    Type: OG-2.6-3 , 19th Intern. Cosmic Ray Conf - Vol. 1; p 234-237; NASA-CP-2376-VOL-1
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  • 8
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    Observations on TeV gamma rays from Geminga and PSR 0950+08 (1985)
    In:  CASI
    Details
    Publication Date: 2019-06-28
    Description: The Geminga (2 CG 195+04) which exhibits a periodicity with a period of 59 to 60 s in its emission of X-rays, GeV gamma rays and TeV gamma rays was studied. During the winter of 1984 to 1985, this object was observed to see if it emits TeV gamma rays with a periodicity approx 60 s. The observations were carried out at two different sites separated by 11 Km with the Ooty Atmospheric Cerenkov Array split into two parts. Data were collected during clear moonless nights for a total duration of 15.3 hours spread over 2 months. Since the first time derivative of period is believed to be large and uncertain. The total data are subdivided into segments of duration not more than 3 days each to steer clear of the effects of P in the phase analysis. If TeV gamma ray signals are seen in each of these segments, it is possible to derive P from observed data.
    Keywords: SPACE RADIATION
    Type: OG-2.4-6 , 19th Intern. Cosmic Ray Conf - Vol. 1; p 181-182; NASA-CP-2376-VOL-1
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  • 9
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    Secondary periodicities of microbursts of TeV gamma rays from the Crab pulsar (1985)
    In:  CASI
    Details
    Publication Date: 2019-06-28
    Description: Observations were made during the past several years on the Crab pulsar using the Ooty atmospheric Cerenkov array with the aim of detecting possible emission of ultra high energy gamma rays by the pulsar. During the course of these observations, it was found that the Crab pulsar emits TeV gamma rays in bursts of short duration. The microbursts of TeV gamma rays from the Crab pulsar, which were seen in the data of at least three years, also reveal interesting secondary periodicities. It was noticed at first that some bursts could be connected with the others that occurred during the same night or during the next two nights with integral number of cycles of periods 43 + or - 1 minute. Ten possible periods in the vicinity of 43 minutes were determined for all the combinations of bursts for each year. The best values of periods thus obtained were different from year to year. But when, instead of the real time, the number of Crab cycles elapsed between the bursts was used as the unit of time, two values of burst periods - 77460 and 77770 Crab cycles - were found to be significant in the data of at least two years. A Monte Carlo simulation using 1500 trial periods chosen randomly within + or - 5 minutes of the original burst period did not reveal any value of the period as significant.
    Keywords: SPACE RADIATION
    Type: OG-2.3-5 , 19th Intern. Cosmic Ray Conf - Vol. 1; p 144; NASA-CP-2376-VOL-1
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  • 10
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    Limits on deeply penetrating particles in the 10(17) eV cosmic ray flux (1985)
    In:  CASI
    Details
    Publication Date: 2019-06-28
    Description: Deeply penetrating particles in the 10 to the 17th power eV cosmic ray flux were investigated. No such events were found in 8.2 x 10 to the 6th power sec of running time. Limits were set on the following: quark-matter in the primary cosmic ray flux; long-lived, weakly interacting particles produced in p-air collisions; the astrophysical neutrino flux. In particular, the neutrino flux limit at 10 to the 17th power eV implies that z, the red shift of maximum activity is 10 in the model of Hill and Schramm.
    Keywords: SPACE RADIATION
    Type: HE-5.3-1 , 19th Intern. Cosmic Ray Conf - Vol. 8; p 104-107; NASA-CP-2376-VOL-8
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