Answer:
1.3.
Explanation:
From the question given above, the following data were obtained:
Sine of incident angle (Sine i) = 0.217
Sine of refracted angle (Sine r) = 0.173
Refractive index (n) =?
From snell's law, the Refractive index is simply defined as the ratio of the sine of the incident angle to sine of the refracted angle. Mathematically, it is expressed as:
Refractive index = Sine of incident angle / sine of refracted angle
n = Sine i / Sine r
With the above formula, we can obtain index of refraction as shown below:
Sine of incident angle (Sine i) = 0.217
Sine of refracted angle (Sine r) = 0.173
Refractive index (n) =?
n = Sine i / Sine r
n = 0.217 / 0.173
n = 1.3
Thus, the index of refraction is 1.3.
Answer:
Scientists who study the Sun usually divide it up into three main regions: the Sun's interior, the solar atmosphere, and the visible "surface" of the Sun which lies between the interior and the atmosphere. There are three main parts to the Sun's interior: the core, the radiative zone, and the convective zone.
Explanation:
Hopefully this helps :)
B. their distances from the sun.
Explanation:
Absolute Magnitude:
Astronomers defines the absolute magnitude of a stars brightness in terms of how bright a star appears from a standard distance of 10 parsecs. Parsec is a unit of distance in astronomy. 10 parsecs is equal to 32.6 light years.
Apparent Magnitude:
Apparent magnitude of a star refers to how bright the star appears at its distance from the Earth.
If two stars have the same absolute magnitude but their apparent magnitude differs, the reason is that the distance of both the stars from the Earth varies. Hence their brightness differs when measured from Earth. The farther a star is from the Earth, the fainter its brightness.
Keywords: star, brightness, parsec, light years, apparent magnitude, absolute magnitude
Learn more about stars and absolute magnitude from:
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Kepler noticed an imaginary line drawn from a planet to the Sun and this line swept out an equal area of space in equal times, If we then draw a triangle out from the Sun to a planet’s position at one point in time, it is notice that the area doesn't change even after the planet has left the original position say like after 2 to 3days or 2hours. So to have same area of triangle means that the the planet move faster when that are closer to the sun and slowly when they are far from the sun.
This led to Kepler's law of orbital motion.
First Law: Planetary orbits are elliptical with the sun at a focus.
Second Law: The radius vector from the sun to a planet sweeps equal areas in equal times.
Third Law: The ratio of the square of the period of revolution and the cube of the ellipse semi-major axis is the same for all planets.
It is this Kepler's law that makes Newton to come up with his own laws on how planet moves the way they do.
Answer:
North of west
Explanation:
Given
Plane wishes to fly in west
but wind with speed 33.9 km/h towards south obstructing its path
so plane must fly at an angle of \theta w.r.t west such that it final velocity is towards west
Plane absolute speed=195 km/h
To fly towards west velocity in Y direction should be zero
thus 
so Plane should head towards 
North of west in order to fly in west.
So plane
actual velocity is
