In 1842, Julius Robert Mayer discovered The law of conservation of Energy. It its most compact form, it it now called The first law of Thermodynamics
Energy can neither be created nor destroyed, it can only be changed to another form of energy.
We need to directly measure the spectral type in order to determine the surface temperature of a star.
<h3>How do you find the properties of a star?</h3>
Astronomers can determine the temperature of a star by looking at its color and spectrum. The apparent brightness of a star describes how luminous it looks to us. The brightness of a star tells us how bright it really is. The luminance can be determined using both the perceived brightness and the distance.
A star's luminosity, or the total amount of energy it emits each second, is determined by two factors: The stellar photosphere's "Effective Temperature," T. the star's total surface area, which is influenced by its radius, R.
Because it controls how much fuel a star has and how quickly it burns it, a star's mass is its most fundamental characteristic. The majority of a star's life is spent burning hydrogen into helium in its core, which generates energy. The star needs to achieve a balance between gravity and outward pressure in order to continue to be "alive."
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Wind acts as an agent of Erosion and deposition because it can erode the sediments from the rock etc then deposit it someplace else
Answer:
initial velocity =starting velocity
final velocity=last velocity
keep in mind the fact that velocity is a vector quantity it also has a direction
Answer:
The ocean is 6485.6m deep when measured from the vessel
Explanation:
v=1474m/s
t=8.88s
let d represent distance from the vessel to the ocean bottom.
an echo travels a distance equivalent to 2d, that is to and fro after it reflects from the obstacle.
d= 6485.6m
