 The radiation zone is the region of the stellar interior where the flux of energy outward is dependent on radiative heat transfer , since convective heat transfer is inefficient in that zone . In this region the plasma will not be perturbed , and any mass motions will die out . If this is not the case , however , then the plasma becomes unstable and convection will occur , forming a convection zone . This can occur , for example , in regions where very high energy fluxes occur , such as near the core or in areas with high opacity ( making radiatative heat transfer inefficient ) as in the outer envelope . 
 The radiation zone <a href='drop_aux' title='1'><mark>is</mark></a>the region of the stellar interior where the flux of energy outward <a href='drop_aux' title='2'><mark>is</mark></a>dependent on radiative heat transfer , since convective heat transfer <a href='drop_aux' title='3'><mark>is</mark></a>inefficient in that zone . In <a href='None' title='4'><mark>this</mark></a><a href='negative_concord' title='5'><mark>region</mark></a> the plasma will not be perturbed , and any mass motions will die out . If this <a href='negative_concord' title='6'><mark>is</mark></a> <a href='negative_concord' title='7'><mark>not</mark></a><a href='None' title='8'><mark>the</mark></a><a href='negative_concord' title='9'><mark>case</mark></a> , however , then the plasma <a href='uninflect' title='10'><mark>becomes</mark></a> unstable and convection will occur , forming a convection zone . This can occur , for example , in regions where very high energy fluxes occur , such as near the core or in areas with high opacity ( making radiatative heat transfer inefficient ) as in the outer envelope . 
The radiation zone da region of the stellar interior where the flux of energy outward dependent on radiative heat transfer , since convective heat transfer inefficient in that zone . In no region tdaplasma gon not b perturbed , and any mass motions wgondie out . If dis ain't no case , however , then the plasma become unstable and convection will occur , forming a convection zone . Tdiscan occur , for example , in regions where very high energy fluxes occur , such as near the core or in areas with high opacity ( making radiatative heat transfer inefficient ) as in the outer envelope .