بلغات أخرى
- الألمانيّة: Elektromagnetische Strahlung
- الإنجليزيّة: Electromagnetic Radiation
- الإسبانيّة: Radiación electromagnética
- الفرنسيّة: Rayonnement électromagnétique
- الهندية: इलेक्ट्रोमॅग्नेटिक रेडिएशन (विद्युतचुंबकीय विकिरण)
- الإيطاليّة: Radiazione elettromagnetica
- اليابانيّة: 放射 (رابط خارجي)
- الكوريّة: 전자기복사
- المهاراتية: इलेक्ट्रोमॅग्नेटिक रेडिएशन (विद्युत चुंबकीय विकिरण)
- البرتغاليّة البرازيليّة: Radiação eletromagnética
- الصينيّة المبسطة: 电磁辐射
- الصينيّة التقليدية: 電磁輻射
الرسوم التوضيحية المرتبطة
إشعاع الجسم الأسود
إشعاع الجسم الأسود - كارثة الأشعة فوق البنفسجية
Stellar Structure
الشرح: Stars are balls of plasma. For most of a star’s life it burns hydrogen into helium in its core. This phase of a star’s life is known as the main sequence. Burning hydrogen into helium produces heat, that heat travels out of the star’s core eventually reaching the star’s photosphere (often referred to as the “surface” of the star). From here the heat can radiate into space as various forms of electromagnetic radiation. However, how heat travels from the core to the photosphere depends on the star’s mass.
Imagine a parcel of gas rising inside a star. As it rises, it moves into an area of lower pressure, so it cools down and expands. If the parcel is still hotter, and therefore less dense than its surroundings, it keeps moving upward due to buoyancy. Eventually, it will rise far enough to cool and sink back down. This rising and sinking cycle is called convection. Whether convection occurs depends on how quickly temperature changes as you move away from the star’s core. If the temperature in a star drops rapidly, rising parcels of gas are more likely to stay hotter than their surroundings, so convection dominates as the mode of energy transfer in this part of the star. Conversely if the temperature drops more slowly (i.e. if the temperature gradient is small) then heat will mostly be transferred by radiation (photons).
In the most massive main sequence stars (more massive than about 1.5 times the mass of the Sun, seen here on the left), hydrogen is burned into helium using the CNO cycle. This is highly temperature dependent and thus energy production is concentrated near the center of the star. This leads to a larger temperature gradient and thus a convective core. Further out the temperature gradient becomes smaller and heat transport is dominated by radiation. This is called the radiative zone.
For lower mass stars like the Sun (between 0.3 and 1.5 solar masses, seen here in the middle) hydrogen is burned to helium using a different process (the pp chain). This depends less on the internal temperature than the CNO cycle and so energy production is more distributed in the star’s core. This leads to a smaller temperature gradient and thus a radiative core where convection occurs surrounded by a radiative zone. Going further out the gas becomes cool enough for some elements to hang to on some of their electrons, i.e. not being completely ionised. This partially ionised gas is more opaque to photons, trapping heat. This leads to a large temperature gradient and thus convection.
The lowest mass stars (below 0.3 solar masses, seen here on the right) have no radiative zone and are fully convective.
The arrows in the radiative zone are shown as wavy lines heading out of the star. However, a photon’s journey out of a star is much more complex with each individual photon travelling only a short distance before being deflected by some of the charged particles that make up the plasma of the star’s interior. This leads to a long and winding road that takes millennia instead of the few seconds it would take if the photon did not interact with particles in the plasma.
المصدر: Based on a vector diagram by Wikimedia user Д.Ильин which itself is based on a diagram from sun.org
License: CC-BY-4.0 المشاع الإبداعي نَسب المُصنَّف 4.0 دولي (CC BY 4.0) أيقونات
