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Dec 26, 2014 · The same applies to the beams of light above them. The Sun is very far away and the beams are pretty much parallel, but they're pointing towards you, and perspective makes them appear to converge towards the vanishing point - which in this case is the Sun's location in the sky. The technical term for these beams is "crepuscular rays."
0. If you want your eyes to receive 32000~100000lux, you need to stare at the sun in a sunny day.If you stare at the ground in a sun-exposure area, your eyes receives much less than 32000 lux. If you stare at a shedded ground in a sunny day, your eyes receive slight less than 10000lux. human eyes could not tolerate 32000lux more than 5 secounds.
Feb 15, 2011 · Another way of calculating the earth - sun distance is to look at the centrifugal and the gravitational force. This solution assumes that one already knows the mass of the sun, but thats a different problem ;-).
Apr 17, 2015 · If we assume the Sun orbits the Earth, the math says that the Sun should be much less massive than the Earth. If we assume the Earth orbits the Sun, the opposite is true. Either way we can get an estimate of the mass of the Sun. We know from other tests that the Sun is more massive than the Earth, so therefore the Earth orbits the Sun.
Mar 10, 2020 · Now the Sun loses a small amount of mass. The Earth is still traveling at the same velocity, and requires the same centripetal force to maintain the same circular orbit. Unfortunately, the reduced mass of the Sun no longer supplies the required centripetal force. So the Earth is now in a slightly elliptical orbit, passing perihelion.
But in Gerthsen Kneser Vogel there is an exercise where Sherlock Holmes estimated the temperature of the sun only knowing the root of the fraction of D and R. Lets say, he estimated this fraction to 225, so the square root is about 15, how does he come to 6000 K ?
Oct 8, 2013 · A well known story "Two Children arguing about the sun" (From Lie Zi, ca. 500BC): On the way traveling to the east, Confucius saw two children were arguing. One child thought that the sun is nearer to us at daybreak and far away from us at noon, because in the morning it is as big as the canopy of a carriage, but at noon only the size of a ...
May 22, 2018 · So, now you need to simply calculate the total power passing through a sphere whose radius is the same of the Earth's orbit, and this is. P = 4πR2F ≈ 3.8 ×1026W = 3.8 ×1026J/s P = 4 π R 2 F ≈ 3.8 × 10 26 W = 3.8 × 10 26 J / s. Since energy is conserved this number is the amount of power passing through any surface surrounding the Sun ...
May 31, 2015 · Stefan-Boltzmann: J = σT4 J = σ T 4. To lose 1 kW over 1 m 2 requires a temperature of. T = 1000 5.67 ⋅10−8− −−−−−−−−√4 ≈ 364 K T = 1000 5.67 ⋅ 10 − 8 4 ≈ 364 K. This assumes only the surface facing the sun loses heat by radiation: in other words this is only valid for a black surface mounted on a good insulator.
Feb 15, 2017 · The Sun has actually set/risen and we see it due to the way light is bent across the atmosphere. Apparently due to coincidence of the size and distance of the sun, its exactly the same size - so if we see 50% of the sun, the sun is 50% below the horizon. So, I understand all this, so here is my question :
