explain with the help of a diagram the part played by the inclination of Earth's axis in causing day and night of wearing duration except at the equator
Answers
Explain with the help of diagram the part played by the inclination of earth's axis in causing day and night of duration accept at the equator
Answer:
the Earth is tilted at 23.5 degress. Due to this inclination, there is variation in length of day and night with the change in seasons with the rotation of the earth around the sun. This is better explained in the following pictures. Circle of Illumination: It is the line which delineates day and night on earth.
Explanation:
As the earth rotates on its axis and the causes us to experience the phenomenon of the day and the night and is measured between the earth's equatorial plane and the plane in which orbits around the sun.
The rays of the sun that falls over the earth and this angle shows the measure of the solar radiation and the impact of the temperatures over the surface of the earth and when the rays of the sun strikes at the equator that gets most of the percent of the isolation as ts direct as the solar radiation is concentrated over this region.
They have a low angle of the incoming solar radiation and have a low angle of the income solar radiation at the 60 degrees north and the south. This affects the equinox and the soloistic on earth.
Know more about the role played by the angle of inclination with the earth axis in causing the day and night of duration.
Answer:
B Eclipsing Binary Light Curves
The orbital plane of eclipsing stars lies perpendicular to the plane of the sky. Depending on the relative sizes of the stars, the orbital inclination over which eclipses can occur is considerable, but in general only a small fraction of the known binary systems will be seen to undergo eclipses. The variation in light serves two purposes. It permits a determination of the relative radii of the stars, since the duration of ingress and the duration of eclipse depend on the difference in the sizes of the stars. That is, if Δt1 is the total time between first and last contact, and Δt2 is the duration of totality, assuming that the eclipse is annular or total, then,
(5)
Δt1
Δt2
=
rg+rs
rg-rs
where rs is the smaller and rg is the greater radius, respectively. The diminution in light from the system depends on the relative surface brightness of the stars, which in turn depends on the surface (effective) temperature, Teff. Eclipses will not be total if the two stars are not precisely in the line of sight, unless they differ considerably in radius, so that the mark of totality is that the light does not vary during the minimum in brightness.