Large telescopes aren't built on mountain tops for the purpose of watching
weather systems. The ones that are built at high altitudes are intended to be
used to observe celestial objects ... planets, stars, galaxies, comets, nebulae,
quasars, novae, and the space around black holes.
The way a telescope does that is: It collects visible light and radiation with
other electromagnetic wavelengths, and people then analyze the radiation
that the telescope has collected.
When we use the telescope to do that, we want anything it collects to be
as close as possible to the radiation that actually left the star. The problem
is that anything the telescope collects must come down through AIR. The trip
through air changes the radiation before you have a chance to collect it, so
you can never see exactly what left the star.
The solution:
==> Build your telescope in a place where the light goes through less air
before it reaches the telescope.
==> Or ... if you can work it out somehow ... through NO air.
That means:
==> Build your telescope at high altitude, on a mountaintop, where
most of the Earth's air is BELOW you.
==> Or put your telescope in a spacecraft. Put the spacecraft in orbit
around the Earth, where there is almost NO air, and let the telescope
send its pictures and other data to you by radio.
Answer:
0072.00kW
Explanation:
1,200 hours multiply by 60W will give you 72000kW. Convert it to kW. That will give you 0072.00kW.
<span>Most objects tend to contain the same numbers of positive and negative charge because this is the most stable situation. In fact, if an object has an excess of positive charge, it tends to attract an equal number of negative charges to balance this effect and restore neutrality: the attracted negative charges combine with the excess of positive charges, leaving the object electrically neutral.</span>
Answer:
r = 1.63×10^5 mi
Explanation:
Let r = distance of object from earth
Rs = distance between earth and sun
Ms = mass of the sun
= 3.24×10^5 Me (Me = mass of earth)
At a distance R from earth, the force Fs exerted by the sun on the object is equal to the force Fe exerted by the earth on the object. Using Newton's universal law of gravitation,
Fs = Fe
GmMs/(Rs - r)^2 = GmMe/r^2
This simplifies to
Ms/(Rs - r)^2 = Me/r^2
(3.24×10^5 Me)/(Rs - r)^2 = Me/r^2
Taking the reciprocal and then its square root, this simplifies further to
Rs - r = (569.2)r ----> Rs = 570.2r
or
r = Rs/570.2 = (9.3×10^7 mi)/570.2
= 1.63×10^5 mi
