Stars produce the majority of their energy through nuclear <1>. It is possible to get energy out of a nuclear reaction as long as the process moves toward <2> on the binding energy per nucleon graph. Processes where small nuclei are combined into larger ones are known as <3> and examples of this include stars and hydrogen bombs. Processes where a large nucleus is split into two smaller nuclei are called fission and examples of this include atomic bombs and <4>.
The most important fusion reaction in $star is the <5>. In this process 4 hydrogen atoms are converted into 1 <6> atom and the resulting loss of mass is converted into energy as decribed in the equation E=mc2. This reaction only occurs in the <7> of a star where the temperature is high enough to overcome the Coubomb barrier. Energy is then transported to the surface predominantly by <8> in the $region1 part of the sun and by <9> in the $region2 part of the sun. This outward streaming flow of radiation balancing the weight of the overlying areas is known as <10>.
@ qu.1.1.algorithm= $num=rint(2); $star=switch($num,"medium-mass stars","massive stars"); $process=switch($num,"Proton-Proton Chain","CNO Cycle"); $badprocess=switch($num,"CNO Cycle","Proton-Proton Chain"); $num2=rint(2); $region1=switch($num2,"inner","outer"); $region2=switch($num2,"outer","inner"); $thermal1=switch($num2,"radiation","convection"); $thermal2=switch($num2,"convection","radiation"); @ qu.1.1.blank.1=fusion,fission,gravitational contraction@ qu.1.1.blank.2=iron,hydrogen,helium,carbon@ qu.1.1.blank.3=fusion,fission,gravitational contraction@ qu.1.1.blank.4=nuclear reactors,nucleosynthesis,the proton-proton chain@ qu.1.1.blank.5=$process,$badprocess,Triple-Alpha Process@ qu.1.1.blank.6=helium,lithium,carbon,iron@ qu.1.1.blank.7=core, convective zone,corona,photosphere@ qu.1.1.blank.8=$thermal1,$thermal2,conduction@ qu.1.1.blank.9=$thermal2,$thermal1,conduction@ qu.1.1.blank.10=hydrostatic equilibrium,heliosiesmology,ideal gas pressure@ qu.1.1.grader.1=menu@ qu.1.1.grader.2=menu@ qu.1.1.grader.3=menu@ qu.1.1.grader.4=menu@ qu.1.1.grader.5=menu@ qu.1.1.grader.6=menu@ qu.1.1.grader.7=menu@ qu.1.1.grader.8=menu@ qu.1.1.grader.9=menu@ qu.1.1.grader.10=menu@ qu.1.2.mode=Blanks@ qu.1.2.editing=useHTML@ qu.1.2.name=SolarEnergy@ qu.1.2.question=Stars produce the majority of their energy through nuclear <1>. It is possible to get energy out of a nuclear reaction as long as the process moves toward <2> on the binding energy per nucleon graph. Processes where a large nucleus is split into two smaller nuclei are called fission and examples of this include atomic bombs and <3>. Processes where small nuclei are combined into larger ones are known as <4> and examples of this include stars and hydrogen bombs.
The most important fusion reaction in $star is the <5>. In this process 4 hydrogen atoms are converted into 1 <6> atom and the resulting loss of mass is converted into energy as decribed in the equation E=mc2. This reaction only occurs in the <7> of a star where the temperature is high enough to overcome the Coubomb barrier. Energy is then transported to the surface predominantly by <8> in the $region1 part of the sun and by <9> in the $region2 part of the sun. This outward streaming flow of radiation balancing the weight of the overlying areas is known as <10>.
@ qu.1.2.algorithm= $num=rint(2); $star=switch($num,"medium-mass stars","massive stars"); $process=switch($num,"Proton-Proton Chain","CNO Cycle"); $badprocess=switch($num,"CNO Cycle","Proton-Proton Chain"); $num2=rint(2); $region1=switch($num2,"inner","outer"); $region2=switch($num2,"outer","inner"); $thermal1=switch($num2,"radiation","convection"); $thermal2=switch($num2,"convection","radiation"); @ qu.1.2.blank.1=fusion,fission,gravitational contraction@ qu.1.2.blank.2=iron,hydrogen,helium,carbon@ qu.1.2.blank.3=nuclear reactors,nucleosynthesis,the proton-proton chain@ qu.1.2.blank.4=fusion,fission,gravitational contraction@ qu.1.2.blank.5=$process,$badprocess,Triple-Alpha Process@ qu.1.2.blank.6=helium,lithium,carbon,iron@ qu.1.2.blank.7=core,convective zone,corona,photosphere@ qu.1.2.blank.8=$thermal1,$thermal2,conduction@ qu.1.2.blank.9=$thermal2,$thermal1,conduction@ qu.1.2.blank.10=hydrostatic equilibrium,heliosiesmology,ideal gas pressure@ qu.1.2.grader.1=menu@ qu.1.2.grader.2=menu@ qu.1.2.grader.3=menu@ qu.1.2.grader.4=menu@ qu.1.2.grader.5=menu@ qu.1.2.grader.6=menu@ qu.1.2.grader.7=menu@ qu.1.2.grader.8=menu@ qu.1.2.grader.9=menu@ qu.1.2.grader.10=menu@