Hysteresis Loop Effect on Coronal Index and Solar Flare Index During Solar Cycles 22 and 23

The hysteresis loop effect on the solar activity as coronal index (CI) and solar flare index (SFI) over cosmic ray intensity (CRI) at the low cut-off rigidities neutron monitoring station Oulu on the monthly basis data for the period January 1, 1986 to December 31, 2008 has been studied. It is observed that the shape of the hysteresis loops is varying from solar cycle 22 to 23. The hysteresis loops for solar cycle 23 are broad ovals whereas for solar cycle 22 are nearly flat. A complementary feature of the cosmic ray intensity decreases more rapidly as the increase in solar activity (coronal index and solar flare index). The positive solar polar magnetic parameter (A>0) and negative solar polar magnetic parameter (A<0) is representing the hysteresis loops

Solar plasma related to Geomagnetic Disturbance storm time during Solar Cycles 22 & 23

A correlative and comparative study has been carried out between the peak values of Geomagnetic Disturbance storm time (Dst) corresponding to Interplanetary Magnetic Field (IMF), and solar plasma parameters during solar cycles 22 and 23. For this purpose, we have identified 86 Geomagnetic Disturbance storm time index from -150nT to -589nT.This study has shown that the Bz component is a significant factor in the description of geomagnetic storms. A linear relationship has been established between Dst and corresponding to IMF and solar plasma parameters. Our study has suggested that geomagnetic storms only occur when the value of solar wind velocity exceeds ~350 km/sec. We have observed that the strong solar wind and interplanetary magnetic field were responsible for an intense geomagnetic storm. Moreover, the phase of IMF and Dst is strongly related during occurring of geomagnetic storms for solar cycles 22 and 23

Growth and Yield of Wheat (Triticum aestivum L.) as Affected by Bio-Fertilizer and Seaweed Extract

The field experiment was conducted at crop research farm (CRF) during Rabi season 2021- 22 Department of Agronomy, SHUATS, Prayagraj (U.P), to evaluate the influence of bio-fertiliser and seaweed extract on growth and yield of wheat. The 9 treatments consisting of Seed inoculation with Azotobacter (ASI) 20g/kg seed and 0% application of seaweed extract (SWE) (T1), ASI 20g/kg seed and 5% application of SWE (T2), ASI 20g/kg seed and 7.5% application of SWE (T3), Seed inoculation with PSB 20g/kg seed and 0% application of SWE (T4), Seed inoculation with PSB 20g/kg seed and 5% application of SWE (T5), Seed inoculation with PSB 20g/kg seed and 7.5% application of SWE (T6), Seed inoculation with both Azotobacter and PSB 10+10g/kg seed and foliar application of 0% SWE (T7), Seed inoculation with both Azotobacter and PSB 10+10g/kg seed and foliar application of 5% SWE (T8), Seed inoculation with both Azotobacter and PSB 10+10g/kg seed and foliar application of 7.5% SWE (T9), were carried in Randomized Block Design and replicated thrice. The results showed that seed inoculation with both Azotobacter and PSB 10+10g/kg seed and foliar application of 7.5% SWE at 30 and 60 days after sowing (DAS) (T9) had superior values of growth parameters i.e., plant height  (35.39, 82.58, 84.59 cm) and dry weight (6.19, 16.61, 22.85 g) at 60, 90 days after sowing (DAS) and harvest, respectively, and found more productive as it attained higher values of spikes/m2 (391.67), grains/spike (53.79), test weight (40.00), as well as grain (6.68 t/ha) and straw yields (10.68 t/ha) and proved statistically superior over other treatments but found at par to seed inoculation with both Azotobacter and PSB 10+10 g/kg seed and foliar application of 5% seaweed extract (T8)

Hysteresis Loop Effect on Coronal Index and Solar Flare Index During Solar Cycles 22 and 23

83-85The hysteresis loop effect on the solar activity as coronal index (CI) and solar flare index (SFI) over cosmic ray intensity (CRI) at the low cut-off rigidities neutron monitoring station Oulu on the monthly basis data for the period January 1, 1986 to December 31, 2008 has been studied. It is observed that the shape of the hysteresis loops is varying from solar cycle 22 to 23. The hysteresis loops for solar cycle 23 are broad ovals whereas for solar cycle 22 are nearly flat. A complementary feature of the cosmic ray intensity decreases more rapidly as the increase in solar activity (coronal index and solar flare index). The positive solar polar magnetic parameter (A>0) and negative solar polar magnetic parameter (A<0) is representing the hysteresis loops