The energy that is lost becomes free energy.
The Sun is the major source of energy for organisms and the ecosystems of which they are a part. Producers, such as plants and algae, use energy from sunlight to make food energy by combining carbon dioxide and water to form organic matter. This process begins the flow of energy through almost all food webs.
Nuclear fusion is the source of all energy the Sun releases into space. The Sun fuses hydrogen at a steady rate, thanks to a natural feedback process that acts as a thermostat for the Sun's interior (p-p chain). Solar energy production remains steady because the rate of nuclear fusion is very sensitive to temperature.
<h3>Nuclear fusion</h3>
When two or more atomic nuclei join, one or more new atomic nuclei and subatomic particles are created. This reaction is known as nuclear fusion (neutrons or protons). Energy is released or absorbed depending on how much mass the reactants and products have in common.
The atomic nuclei before and after the reaction had different nuclear binding energies, which is how this difference in mass developed. Active or main sequence stars, along with other high-magnitude stars, are powered by nuclear fusion, which releases enormous amounts of energy. Energy will often be released during nuclear fusion that creates atomic nuclei lighter than iron-56 or nickel-62. Both their mass and nucleon binding energy are relatively high for these elements.
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(3); try using the phrase "AN OX ate the RED CAT"
(anode=oxidation, reduction=cathode)
Answer:
=14.8 grams
Explanation:
The remaining amount is normally calculated using the formula:
Remaining mass= 1/2ⁿ × Original mass where n is the number of half-lives.
Therefore, original mass= Remaining mass × 2ⁿ
Remaining mass= 2.2 grams
Number of half lives= 2.75 half lives
Original mass= 2.2g × 2²·⁷⁵
=14.8 grams
