At the core of all stars, there's a glowing nuclear furnace. We can be sure of this because we can measure how many neutrinos are streaming out of the sun with experiments like the Sudbury Neutrino Observatory. This property of neutrinos, that they can pass through the core of the star virtually unimpeded, is because neutrinos are weakly interacting particles. Which is to say that they do not interact with electromagnetic forces. Light particles or photons do interact electromagnetically and thus they have a very difficult time leaving the core of a star.
모든 별의 중심부는 핵융합로다. 얼마나 많은 중성미자(neutrino)가 방출되는지 측정하면 핵융합로의 규모를 알 수 있다. 서드베리 뉴트리노 관측소에서 중성미자를 관측한다. [일본은 카미오칸데.] 뉴트리노는 중력과 매우 약하게 상호작용하기 때문에 별 중심부에서 방해없이 표면으로 방출된다. 별중심부의 핵융합으로 엄청난 양의 중성미자가 방출되지만 심지어 전자기장과도 작용하지 않기 때문에 관측하기도 매우 어렵다.
Let's carve into our own sun and examine how the energy produced at the core is radiated away as the light that we see here on Earth. The innermost region of the sun extending from the center to about one quarter of the radius of the sun, is the region where nuclear fusion takes place. This is aptly named the thermonuclear energy core. In this innermost region, the temperature, pressure, and density are extremely high, suitable for elements to combine in the process of fusion. The temperature has been estimated to be 1.55 x 10 to the power of 7 K, roughly 15 million degrees. The density of the material is nearly 14 times the density of lead and the pressure is almost a billion times the atmospheric pressure here on Earth. Needless to say, you wouldn't want to go there but if you did find yourself there, you'd want to escape pretty fast.
태양 중심에서 1/4가량되는 영역이 핵융합이 일어나는 곳이다. 열핵 에너지 중심(the thermonuclear energy core)이라고 한다.
In order for energy to escape from this region, it needs to be carried away by one of three processes: conduction, convection, and radiation.
에너지가 전달되는 3가지 방식: 전도(conduction), 대류(convection), 복사(radiation) 가 있다.
Conduction, which is the propagation of heat through a solid, is inefficient in the sun because, well, the sun isn't a solid. In this centermost region, extending to about three quarters of the diameter of the sun, energy is carried away by radiative processes, the motion of photons.
전도(Conduction)에 의한 열전달은 고체(solid)에서 유효하다. 밀도가 높은 태양 중심부에서 전도가 유효하며 3/4의 영역에서 열전달은 빛(광자)의 운동에 의한 복사(Radiation)가 지배적이다.
Extending outward from the thermonuclear energy core, the radiative zone is a region of the sun where photons dominate the energy flow towards the surface of the sun. You would think that light, travelling at just over a billion kilometers per hour, wouldn't take long to escape from the core of the sun. And indeed, if there was nothing impeding the progress of photons inside the sun, they would take about 2.3 seconds to cross the sun's nearly 700,000 kilometer radius. But photons are impeded by the materials of the sun. Instead of 2.3 seconds, photons take an average of 170,000 years to escape into space. That's right, the energy we observe in the form of sunlight has been working its way to the surface of the sun for hundreds of thousands of years.
Within the first three-quarters of the diameter of the sun, photons bounce around on very short paths, randomly walking their way towards the surface. Each step taken by a photon amounts to about 1 centimeter and the energy must be carried nearly 700,000 kilometers. Just like the balls in this toy version of a rain stick, photons jostle through the materials of the sun, colliding and careening their way to the surface. Not every step will be directed towards the surface of the sun, though.
태양중심에서 3/4 구간동안 광자는 내부의 물질들에 부디치며 난수 뜀(randomly walking)을 하며 짧은 경로를 택해 이동한다. 표면을 향해 이동하는 광자는 1센티미터 마다 차이를 보이며 70만 키로미터를 이동한다.
But photons will preferentially migrate towards the surface due to the temperature gradient. If you consider that this rain stick has a gravity radiant, instead of a temperature one, it's not a bad analogy for the motion of photons within the sun. Have a look at the math. If you took a 1 centimeter step every second, it would take you over 2,000 years to walk 700,000 kilometres. But that's assuming that you would walk in a straight line. If you stumbled around randomly, say, after getting off a dizzying rollercoaster, it would take you quite a bit longer to get where you want to go. Eventually, the energy from the core of the sun stumbles its way to the surface.
극심한 온도차를 격기 전까지 광자는 꾸준히 표면을 향해 나간다. 초당 1센티미터로 70만 킬로미터를 가려면 2천년이 걸린다. 이는 직진할때 시간이고 수많은 충돌을 격으며 이리저리 방향을 틀며 이동하면 훨씬 긴 경로를 움직여야 한다.
From the centermost thermonuclear energy core, encompassing the first one quarter of the sun's radius, through the radiative zone, from one quarter to about seven tenths of the sun, photons encounter the convective zone, the outermost layer of the sun's surface. As you move outward, the average temperature of the sun drops. And at the boundary of the convective zone, it's cool enough for electrons and protons to join into hydrogen atoms which happen to be very good at absorbing photons.
Radiative energy transfer is no longer the dominant process and convection takes over. Atoms heated at the bottom of the convective zone become buoyant and the mass of the hot atoms and plasma rise to the surface like bubbles in a lava lamp. Cooler gas at the surface of the sun sinks down to replace the hot gas that's rising and the process repeats.
Once the hot gas reaches the sun's surface, energy stored in the heat of the gas is emitted as black body photons which can then travel across the vast distances of space, virtually unimpeded. Now that there are finally some photons escaping the sun, let's put on our safe solar filtering glasses and have a look.
* 태양 중심부 온도 1천 5백만K에서 표면 온도 6천K로 떨어진다.
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