排序方式： 共有19条查询结果，搜索用时 31 毫秒
1.
The purpose of this paper is to find correlation between OI 6300 Å line intensity with solar and ionospheric parameters. A critical study have been made and the following important results are obtained:
相似文献
| (i) | Solar flare index plays more important role for the emissions of 6300 Å line than other solar parameters. |
| (ii) | Intensity of 6300 Å line increases linearly with the increase of solar flare index. |
| (iii) | Virtual height plays more important role than critical frequency for the emission of 6300 Å line-intensity. |
| (iv) | Possible explanation of this type of variation is also presented. |
2.
The paper presents the effect of O3 depletion on different night airglow emission lines. Calculations based on chemical kinetics show that the airglow intensity of Na5893Å, O5577Å and OH band emissions will also be affected due to the depletion of O3 concentration. Intensity of Na5893Å is calculated theoretically for Halley Bay (76° S,27° W), British Antarctic Survey Station, during the period 1973 to 1984. It is concluded from the covariation of different emission lines that O5577Å and OH emissions also follow the same trend of variation. A study has been made to find the correlation between the depletion of O3 concentration and total solar flare numbers. Important results are as follows:
相似文献
| (i) | Depletion of O3 is oscillatory upto 7932 solar flare numbers. The average trend of variation of O3 concentration is downward, i.e., O3 is depleted with the increase of total solar flare numbers. |
| (ii) | Afterwards, it follows a upward trend. Possible explanation of such type variation is also presented. |
3.
Evening and morning twilight enhancements of 5577 Å and 5893 Å lines were observed by Dunn-Manring type photometer at Calcutta during the period 1983–1985 and that of 5577 Å have been collected from Allahabad observatory. The following paper presents the correlation between the enhanced intensity of airglow lines (A
G
) and solar flare index (I
f
) which is calculated considering all the flares which occurred 24 hr before the times of occurrence of enhancements. It is observed that the intensity of airglow lines varies with the flare index in an oscillatory manner upto a certain limiting value ofI
f
. Afterwards intensity of both lines increases with the increase ofI
f
. The nature of variation is the same for both sunspot maximum and minimum periods. A possible explanation of such type of variation has also been invoked. 相似文献
4.
The paper presents the nature of the variation of refractive index of atmospheric medium with time and altitude before, during and after the onset of thunderstorms over Gangetic West Bengal during the pre-monsoon period. A critical analysis shows that sharp depletion of the refractive index takes place before the onset of Nor??westers and possible explanations are also offered for the said occurrence. 相似文献
5.
D. Bhaumik J. N. Chakravorty S. K. Midya S. Chakraborty 《Earth, Moon, and Planets》1996,74(2):115-121
Evening twilight airglow emissions of OH (7,2) band and Li 6708 Å are observed by Dunn-Manring type photometer and following important results are obtained.
- Intensity of OH (7,2) and Li (6708 Å) decrease exponentially during evening twilight period.
- OH (7,2) band covaries with Li (6708 Å) during evening twilight period.
- Empirical equations of OH (7,2) band with time is obtained.
- Possible explanations of such type of variations is also presented.
6.
The paper presents the relations between different solar and ionospheric parameters. Variation of 5577 line intensity with the variation of solar and ionospheric parametersis also discussed. A study have been made and following important results are obtained:(i) Virtual height ofF layer is decreased exponentially with the increase of solar flare numbers, sunspot number and 10.7 cm solar flux.(ii) Linear relations between critical frequency ofF layer and different solar parameters are obtained.(iii) Empirical relations between ionospheric and solar parameters are established.(iv) It is concluded that airglow intensity will also be affected with the variation of different solar and ionospheric parameters.(v) It is concluded that airglow intensity is mainly affected by 10.7 cm solar flux among different solar parameters and virtual height plays important role than critical frequency ofF layer. 相似文献
7.
The paper presents the seasonal variation of 6300 Å line intensity at Calcutta with relative sunspot number, solar flare number and variable component of 10.7 cm solar flux. A study has been made and important results have been obtained which are as follows. (i) Intensity of 6300 Å line shows periodic variation with relative sunspot number, solar flare number and variable component of 10.7 cm solar flux during the period 1984–1986 which is the secondary peak of the descending phase of 21st solar cycle. (ii) 6300 Å line intensity at Cachoeira Paulista station, taken by Sahai et al. (1988), also shows periodic variation with solar parameters during the period 1978–1980 which is the peak phase of the solar cycle. (iii) A possible explanation of such a type of variation is also presented. 相似文献
8.
Variation of the total ozone column during tropical cyclones over the Bay of Bengal and the Arabian Sea 总被引：1，自引：0，他引：1
The variation of the total ozone column (TOC) before, during, and after tropical cyclones occurring in the pre-monsoon and post-monsoon periods over the Bay of Bengal and the Arabian Sea for the period 1997–2009 is presented. From the analysis, it is concluded that TOC decreases steadily before and during the formation of a cyclone, followed by a more or less increasing trend after dissipation of the cyclone. It is also observed that, when the cyclone reaches its peak intensity indicated by its maximum wind speed, there is a sudden fall in TOC over those regions where the cyclone has intensified. The observed variation of TOC is consistent with existing chemical and dynamical theories. 相似文献
9.
The purpose of this paper is to present the correlation of seasonal variation of 5893 Å line intensity with relative sunspot numbers, solar flare numbers and the variable component of 10.7 cm solar flux. A study has been made and the following important results have been obtained.
- The intensity of 5893 Å line at Calcutta shows periodic variation with different solar parameters during descending part of secondary peak of 21st solar cycle (1984–1985).
- 5893 Å line intensity of Mt. Abu also shows periodic variation with solar parameters during the period 1965–1968 when there was a peak phase of 20th solar cycle.
- A possible explanation for such type of variation is also presented.
10.
The paper presents the seasonal variations of OI 6300 Å line night airglow emission at Calcutta and other stations. Their covariations with OI 5577 Å line are also offered. Explanation for the variation is also provided. 相似文献