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        <rdf:li rdf:resource="http://hdl.handle.net/2248/6044" />
        <rdf:li rdf:resource="http://hdl.handle.net/2248/6043" />
        <rdf:li rdf:resource="http://hdl.handle.net/2248/6042" />
        <rdf:li rdf:resource="http://hdl.handle.net/2248/6041" />
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    <dc:date>2026-04-15T15:48:54Z</dc:date>
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  <item rdf:about="http://hdl.handle.net/2248/6044">
    <title>Effect of the solar eclipse on some atmospheric parameter</title>
    <link>http://hdl.handle.net/2248/6044</link>
    <description>Title: Effect of the solar eclipse on some atmospheric parameter
Authors: Rai, J; Rai, A; Kumar, A; Singh, A. K; Singh, M. P; Nigam, M. J
Abstract: To study the solar terrestrial atmospheric parameters such as positive conductivity, negative conductivity, aerosols measurement for forward and backward scattering and atmospheric temperature were recorded at Roorkee during the solar eclipse of October 24, 1995 where the eclipse was about 90%. These observations were taken for about fifteen days spanning both before and after the eclipse.</description>
    <dc:date>1997-01-01T00:00:00Z</dc:date>
  </item>
  <item rdf:about="http://hdl.handle.net/2248/6043">
    <title>Record of extended corona using colour video</title>
    <link>http://hdl.handle.net/2248/6043</link>
    <description>Title: Record of extended corona using colour video
Authors: Saxena, A. K; Samson, J. P. A; Lancelot, J. P
Abstract: The entire event of the total solar eclipse of October 24 1995 was vediographed at our Kalpi camp. We have used SONY handy cam Video 8 Model No. CCD FX 280E PAL attached with 12x variable zoom lens. Partial eclipse was video graphed using neutral density filters. During totality no filters were employed. The sky was very clear with good transparency. Beautiful extended corona even beyond 2Ro has been recorded. The records so obtained are of reasonably high quality and could be used for certain scientific investigations. Few selected frames showing different stages during totality are given in Figure 1.</description>
    <dc:date>1997-01-01T00:00:00Z</dc:date>
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  <item rdf:about="http://hdl.handle.net/2248/6042">
    <title>Response of the small-scale dynamics of lower F-region plasma over Kodaikanal to the total solar eclipse of October 24, 1995</title>
    <link>http://hdl.handle.net/2248/6042</link>
    <description>Title: Response of the small-scale dynamics of lower F-region plasma over Kodaikanal to the total solar eclipse of October 24, 1995
Authors: Visweswara Rao, J. V. S; Sastri, J. H
Abstract: Continuous and high-time resolution recording of the changes in phase path (Doppler frequency shift) of lower F-region reflections over Kodaikanal were made in the forenoon on October 24, 1995 and on several days prior to and after that date. The Doppler data will be used to assess the changes in the small scale dynamics of the lower F-region plasma brought about by the eclipse conditions in the penumbral zone.</description>
    <dc:date>1997-01-01T00:00:00Z</dc:date>
  </item>
  <item rdf:about="http://hdl.handle.net/2248/6041">
    <title>F-region oscillations observed during October 24, 1995 solar eclipse at Waltair</title>
    <link>http://hdl.handle.net/2248/6041</link>
    <description>Title: F-region oscillations observed during October 24, 1995 solar eclipse at Waltair
Authors: Rao, B. M; Anhjaneyulu, P
Abstract: Measurements of changes in phase path/Doppler of HF signals on 5.5 MHz from F-region of the ionosphere are carried-out using coherent pulsed Doppler radar. Preliminary analysis of the data show large deviations in phase path centered around the time of maximum phase of the eclipse on the eclipse day when compared to the control days. These deviations in phase path exhibit a long period oscillatory pattern comparable to the duration of the eclipse with the maximum aptitude during the eclipse interval. The same is severely damped during post eclipse intervals. Enveloped with this long period damped oscillation a systematic short period oscillatory pattern is observed in phase path after the last contact. The periodicity of these short period components are of the order of atmospheric gravity waves with pronounced periods of about 12 minutes followed by 17 and 30 minutes, immediately after the last contact.</description>
    <dc:date>1997-01-01T00:00:00Z</dc:date>
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