Satellite Communication - Orbital Perturbations

This video lecture is about the Orbital Perturbations . Forces pertaining to Orbit perturbations are: Gravitational forces of Sun and Moon, Effect of Earth’s Oblateness, Solar and Lunar Eclipse, Solar radiation pressure, Atmospheric Drag, Aerodynamic Drag, Doppler Effect etc., which have been discussed in detail.
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[@pankilchhabra5584]

Madam please upload the ppt of this video

[@anirudhm187]

At 16:34 , there should be a 2 in denominator , t = (360/2pi) sin-1(8.7/23.5)
In the video just pi is mentioned

[@ECMaddy]

😮

[@anuragghosh328]

The formula using
𝑡
=
365
𝜋
t=
π
365
​
calculates the 21 days required for the eclipse to reach the equinox.
However, this occurs twice a year (once before and once after the equinox).
Therefore, the total eclipse effect duration is:
𝑡
total
=
21
×
2
=
42
days per year
.
t
total
​
=21×2=42 days per year.
The use of
𝜋
π instead of
2
𝜋
2π seems correct here, as it describes a half-cycle (from the start of the eclipse to the equinox). If it were a full cycle (
2
𝜋
2π), it would describe a complete orbital period, not just the eclipse phase.

[@anirudhm187]

Jo bhi hai, Dekhle bhai 😅. Main toh pass hogya aur job bhi lag gyi. Tu padhle. 😂