Answer:
r_{cm} = 4.67 10⁶ m
We see that none of the answers is correct, the closest is the third, but the center of mass is within the radius of the Earth
Explanation:
The definition of the center of mass is
= 1 / M ∑
Where M is the total mass, 
and 
mi are the position and the mass gives each of the bodies
We must locate a reference system for the calculation, we will locate it with the origin in the center of the Earth, the data we have are
Mass of the Earth Me = 5.98 1024 kg
Moon mass m = 7.36 1022 kg
Earth to Moon Distance r = 3.84 108 m
Let's apply this to our case
r_{cm} = 1 / (Me + m) (Me 0 + m R)
r_{cm} = 1 / (598 +7.36) 10²² (0 + 7.36 10²² 3.84 10⁸)
r_{cm} = 4.67 10⁶ m
We can see that this distance is less than the radius of the Earth
We see that none of the answers is correct, the closest is the third, but the center of mass is within the radius of the Earth
<span>A star is born when atoms of light elements are squeezed under enough pressure for their nuclei to undergo fusion. All stars are the result of a balance of forces: the force of gravity compresses atoms in interstellar gas until the fusion reactions begin. And once the fusion reactions begin, they exert an outward pressure. As long as the inward force of gravity and the outward force generated by the fusion reactions are equal, the star remains stable. Clouds of gas are common in our galaxy and in other galaxies like ours. These clouds are called nebulae. A typical nebula is many light-years across and contains enough mass to make several thousand stars the size of our sun. The majority of the gas in nebulae consists of molecules of hydrogen and helium--but most nebulae also contain atoms of other elements, as well as some surprisingly complex organic molecules. These heavier atoms are remnants of older stars, which have exploded in an event we call a supernova. The source of the organic molecules is still a mystery.
STAR BIRTHS are started when the interstellar matter in gas clouds, such as the Eagle Nebula shown here, compresses and fuses. Irregularities in the density of the gas causes a net gravitational force that pulls the gas molecules closer together. Some astronomers think that a gravitational or magnetic disturbance causes the nebula to collapse. As the gases collect, they lose potential energy, which results in an increase in temperature. As the collapse continues, the temperature increases. The collapsing cloud separates into many smaller clouds, each of which may eventually become a star. The core of the cloud collapses faster than the outer parts, and the cloud begins to rotate faster and faster to conserve angular momentum. When the core reaches a temperature of about 2,000 degrees Kelvin, the molecules of hydrogen gas break apart into hydrogen atoms. Eventually the core reaches a temperature of 10,000 degrees Kelvin, and it begins to look like a star when fusion reactions begin. When it has collapsed to about 30 times the size of our sun, it becomes a protostar. When the pressure and temperature in the core become great enough to sustain nuclear fusion, the outward pressure acts against the gravitational force. At this stage the core is about the size of our sun. The remaining dust envelope surrounding the star heats up and glows brightly in the infrared part of the spectrum. At this point the visible light from the new star cannot penetrate the envelope. Eventually, radiation pressure from the star blows away the envelope and the new star begins its evolution. The properties and lifetime of the new star depend on the amount of gas that remains trapped. A star like our sun has a lifetime of about 10 billion years and is just middle-aged, with another five billion years or so left.</span>
Answer:
7.74m/s
Explanation:
Mass = 35.9g = 0.0359kg
A = 39.5cm = 0.395m
K = 18.4N/m
At equilibrium position, there's total conservation of energy.
Total energy = kinetic energy + potential energy
Total Energy = K.E + P.E
½KA² = ½mv² + ½kx²
½KA² = ½(mv² + kx²)
KA² = mv² + kx²
Collect like terms
KA² - Kx² = mv²
K(A² - x²) = mv²
V² = k/m (A² - x²)
V = √(K/m (A² - x²) )
note x = ½A
V = √(k/m (A² - (½A)²)
V = √(k/m (A² - A²/4))
Resolve the fraction between A.
V = √(¾. K/m. A² )
V = √(¾ * (18.4/0.0359)*(0.395)²)
V = √(0.75 * 512.53 * 0.156)
V = √(59.966)
V = 7.74m/s
<span>d = 950 m - 4.9t^2 m
The distance an object moves under constant acceleration is
d = 0.5at^2
where
d = distance
a = acceleration
t = time.
Since we're falling and since we're starting at 950 m above ground, the formula becomes:
d = 950 m - 0.5at^2
Substituting known values, and simplifying gives us
d = 950 m - 0.5*9.8 m/s^2 * t^2
d = 950 m - 4.9 m/s^2 * t^2
Since time is in seconds, we can cancel out the seconds in the units, getting
d = 950 m - 4.9t^2 m</span>
Inertia is the tendency of an object to resist changes in its state of motion.
