We're throwing in the Nexus 4 for this comparison because it also can
do Photospheres out of the box.
Not exact matches
The older idea that acoustic waves flowing out of lower levels heats the corona was abandoned in the 1970s, when the Orbiting Solar Observatory 8 spacecraft
did not see such waves in the chromosphere, the layer just above the
photosphere (the apparent «surface» of the sun in visible light).
A related question is why, if the corona is so hot, it
does not heat up the
photosphere until it has an equally high temperature.
It will
do this via high - speed (sub-second timescales) spectroscopic and magnetic measurements of the solar
photosphere, chromosphere and corona.
In reality, the stellar spectrum
does not cancel out in transmission spectroscopy, because the first - order approximation described above confusingly equates two different light sources: the stellar disk (the spectrum of which is observed before the transit) and the actual light source, which is just a very small fraction of the stellar disk — the projection of the transit chord onto the stellar
photosphere (see figure).
As we pass up through the
photosphere, the temperature drops and the gases, because they are cooler,
do not emit as much light energy.
This integral can be
done at the OD = 1 point, because that is the
photosphere radius for the IR, and for the non-GHG frequencies it doesn't matter where you
do the integral.
2) As you say, when more GHG is added, the altitude of the
photosphere rises (I don't see that the tropopause would rise), and its temperature is reduced: so less power must be radiated away.
But the downward radiation, which is sourced by the upper atmosphere,
does not: At the radius of the old
photosphere, before the addition of the GHG, the downward radiation was rather small, because there wasn't much of the sourcing GHG above it.