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Oberflächentemperatur der Sonne

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That being said... How "difficult" is an exercise? It depends on many factors, like what was being taught etc.
In physics exercises, we try to follow this pattern:

Level 1 - One formula (one you would find in a reference book) is enough to solve the exercise. Example exercise

Level 2 - Two formulas are needed, it's possible to compute an "in-between" solution, i.e. no algebraic equation needed. Example exercise

Level 3 - "Chain-computations" like on level 2, but 3+ calculations. Still, no equations, i.e. you are not forced to solve it in an algebraic manner. Example exercise

Level 4 - Exercise needs to be solved by algebraic equations, not possible to calculate numerical "in-between" results. Example exercise

Level 5 -
Level 6 -

Exercise

https://texercises.com/exercise/oberflachentemperatur-der-sonne/

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The following quantities appear in the problem: Temperatur \(T\) / Leistung \(P\) / Fläche \(A\) / Radius \(r\) / Oberfläche \(S\) /

The following formulas must be used to solve the exercise: \(S = 4 \pi r^2 \quad \) \(\Phi = \epsilon\sigma A T^4 \quad \)

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No explanation / solution video for this exercise has yet been created.
But there is a video to a similar exercise:

In case your browser prevents YouTube embedding: https://youtu.be/WzXgGAyuoao

Exercise:
Schlagen Sie im Formelbuch folge Werte nach: Radius der Sonne mittlerer Abstand der Erde von der Sonne und die Solarkonstante. abcliste abc Werte herauslesen und angeben. abc Berechnen Sie die Strahlungsleistung der Sonne. abc Berechnen Sie die Oberflächentemperatur der Sonne. abcliste

Solution:
abcliste abc Geg R rSun r ncAE J ncJS abc GesStrahlungsleistungvarPhi siW % Unter der Annahme dass die Sonne ihre Wärme kugelförmig in alle Richtungen gleichmässig abstrahlt beträgt die Oberfläche der imaginären glqq Strahlungskugelgrqq al A AF pi qtyncAE^ A. Die Solarkonstante gibt an wie gross die Wärmestromdichte der von der Sonne abgestrahlten Wärme bei Eritt in die Erdatmosphäre ist. Mit der soeben berechneten Fläche erhält man damit die Strahlungsleistung der Sonne al varPhi J A PF ncJS A P. % varPhi PF &approx PS abc Gesabsolute TemperaturT siK % Die Oberfläche der Sonne beträgt al A' AsF pi qtyrSun^ As. Mit dem Stefan-Boltzmann-Gesetz erhalten wir die Oberflächentemperatur der Sonne al T sqrtfracvarPhiepsilon sigma A' sqrtfracPFepsilon sigma AsF TF sqrtfracPeps ncS As T. % T TF &approx TS abcliste

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Contained in these collections:

Wärmestrahlung by dk

1 | 7
Solarkonstante by TeXercises

6 | 7

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Branches	Heat Transfer
Tags	solarkonstante, sonnentemperatur, wärmestrahlung
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Difficulty	(3, default)
Points	0 (default)
Language	(Deutsch)
Type	Calculative / Quantity
Creator	dk
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