Sunspots, prominences and flares are all manifestations of magnetic fields, and these are indicators of processes going on deeper within the Sun. Also, just as earthquakes can help geologists study the Earth's interior, so can "sun-quakes" provide info about the Sun's interior.
The Sun's atmosphere is called the chromosphere and the corona. The photosphere which is below the chromosphere and is the visible surface of the Sun is usually considered to be part of the atmosphere also.
We can't see material below the photosphere because it is opaque to visible light. The high density and temperature of the material, combined with the scattering and absorption of light within it, prevent light from passing through it easily. This makes it impossible for us to directly observe what lies beneath the photosphere with visible light.
The photosphere is the layer in the sun's atmosphere that is dense enough to emit plenty of light but not so dense that the light can't escape. Below the photosphere, the gas is denser and hotter therefore radiates plenty of light, but that light cannot escape from the sun because it is blocked by the outer layers of gas. so you cannot detect light from these deeper layers.Sources: Book The Solar System by Seeds/Backman (7th Edition) P.143
Convection is the dominant form of energy transport just below the photosphere of the Sun. Here, hot plasma rises, cools, and then sinks back down, creating a circulation pattern that helps transfer heat from the interior to the surface.
The Cromoshpere Is Found Just Above The Photosphere. For A Few Moments You Can See The Chromoshpere During A Solar Eclipse Or When Using a Special Instrument.
The Sun's atmosphere is called the chromosphere and the corona. The photosphere which is below the chromosphere and is the visible surface of the Sun is usually considered to be part of the atmosphere also.
The Sun's atmosphere consists of three main layers: the photosphere, chromosphere, and corona. The photosphere is the visible surface of the Sun, where sunlight is emitted. Above it lies the chromosphere, a thin layer that can be observed during solar eclipses, characterized by its reddish color. The outermost layer, the corona, extends far into space and is visible during total solar eclipses, exhibiting a much higher temperature than the layers below it.
The photosphere is the outer part of the star that is visible, inside which the star becomes opaque to visible light. The photosphere is the layer below the star's atmosphere (the chromosphere, and so forth).
We can't see material below the photosphere because it is opaque to visible light. The high density and temperature of the material, combined with the scattering and absorption of light within it, prevent light from passing through it easily. This makes it impossible for us to directly observe what lies beneath the photosphere with visible light.
The sun has no real surface, just different layers of plasma. The layer of the sun that we see is called the "photosphere." The temperatures of the different layers are shown below -- Center -- 27-million degrees Convective zone -- about 7-million degrees Photosphere -- 10,300 degrees Chromosphere -- 22,900 degrees Corona -- 2-million degrees
The photosphere is the layer in the sun's atmosphere that is dense enough to emit plenty of light but not so dense that the light can't escape. Below the photosphere, the gas is denser and hotter therefore radiates plenty of light, but that light cannot escape from the sun because it is blocked by the outer layers of gas. so you cannot detect light from these deeper layers.Sources: Book The Solar System by Seeds/Backman (7th Edition) P.143
The chromosphere is the second of the three main layers of the Sun's atmosphere, located above the photosphere and below the corona. It is characterized by a reddish color and consists of hot, thin gas that emits light primarily in the hydrogen-alpha spectral line. The chromosphere is most easily visible during solar eclipses.
The radiative zone extends from about 25% to 70% of the distance from the Sun's core to its surface, which corresponds to roughly 70-200 thousand kilometers below the photosphere.
Convection is the dominant form of energy transport just below the photosphere of the Sun. Here, hot plasma rises, cools, and then sinks back down, creating a circulation pattern that helps transfer heat from the interior to the surface.
Every layer of rock, as one moves up from the core, is younger than the one below it. This means that the layers of rock above and below the coal are different ages, with the one above younger and the one below older.
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The ocean is stratified with denser layers below less dense layers.