In order to predict whether a star will eventually fuse oxygen into a heavier element, you mainly want to know about the star's mass.
<u>Explanation:</u>
Stellar evolution is procedure by which star experiences a succession of radical change during its lifetime. Depending upon the mass of stars, this lifetimes range from just two or three million years for most big to the trillions of years for a least massive, which is significantly longer or more than the age of universe.
All stars are conceived from falling billows of gas and residue, frequently called nebulae or sub-atomic mists. Throughout a large number of years, the protostar settles down into a condition of balance, turning out to be what is also known as the main- sequence - star.
A=65 divideded by 55 plus 1000000000000000000000000000000000000000000000000000000000000000000000000000000000000000000000
Explanation:
Answer:
Scalar quantity can never be Negative. Because scalar has only magnitude not direction. And magnitude can't be negative.
Explanation:
Answer:
KE_2 = 3.48J
Explanation:
Conservation of Energy
E_1 = E_2
PE_1+KE_1 = PE_2+KE_2
m*g*h+(1/2)m*v² = m*g*h+(1/2)m*v²
(0.0780kg)*(9.81m/s²)*(5.36m)+(.5)*(0.0780kg)*(4.84m/s)² = (0.0780kg)*(9.81m/s²)*(2m)+KE_2
4.10J+0.914J = 1.53J + KE_2
5.01J = 1.53J + KE_2
KE_2 = 3.48J
