Astrophysics - Temperature of a star via flux and wavelength

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SUMMARY

The temperature of a star can be determined using Planck's law for blackbody radiation, specifically the equation F(ν, T) = (2πhν³/c²) / (e^(hν/kT) - 1). In the discussion, it was established that the flux at 450 nm is 1.3 times that at 650 nm, which requires incorporating both wavelengths into the calculations. The variable 'e' represents Euler's number, and to solve for temperature, one must utilize the natural logarithm to reverse the exponentiation. Proper modeling of the star as an ideal blackbody radiator is crucial for accurate temperature calculations.

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  • Understanding of Planck's law for blackbody radiation
  • Familiarity with the concepts of flux and wavelength
  • Knowledge of natural logarithms and their application in solving equations
  • Basic principles of astrophysics related to stellar properties
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  • Study the derivation and applications of Planck's law in astrophysics
  • Learn how to convert between frequency and wavelength in electromagnetic radiation
  • Explore the use of logarithmic functions in solving exponential equations
  • Investigate the characteristics of ideal blackbody radiators and their significance in astrophysics
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Astronomy students, astrophysicists, and educators seeking to deepen their understanding of stellar temperatures and blackbody radiation principles.

cwolfx2
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Homework Statement



What is the temperature of a star if the flux at 450 nm is measured to be 1.3 times the flux at 650 nm.

Homework Equations



I tried to use the equation Flux = 2πhv3/c2

ex-1
x= hv/kt

making 2 of the equations equal each other and solve for T. However being out of practice for months now i do not remember what e represents and how to solve for an exponent.

Though I imagine I may have the wrong equation and not sure if i need to or how to incorporate the wavelengths.
 
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cwolfx2 said:
What is the temperature of a star if the flux at 450 nm is measured to be 1.3 times the flux at 650 nm.

Homework Equations



I tried to use the equation Flux = 2πhv3/c2

ex-1
x= hv/kt

Your spacing wasn't preserved, but if you meant

[tex]F(\nu, T) = \frac{2\pi h\nu^3/c^2}{e^{h\nu/kT} - 1}[/tex]

then yes, this is Planck's law for blackbody radiation.

cwolfx2 said:
making 2 of the equations equal each other and solve for T. However being out of practice for months now i do not remember what e represents and how to solve for an exponent.

'e' is just a number. Granted, it's an irrational number, and it is often used as a base for exponentials because an exponential function with e as a base has certain special properties that are convenient.

In order to solve for x, you have to undo the raising of e to the power of it. In other words, you have to do the inverse operation of taking an exponential. That inverse operation is taking the logarithm to base e, which is also known as the natural logarithm.

cwolfx2 said:
Though I imagine I may have the wrong equation

Modelling the star as an ideal blackbody radiator seems like a reasonable approach.

cwolfx2 said:
and not sure if i need to or how to incorporate the wavelengths.

Of course you need to incorporate them. The Greek symbol 'nu' ([itex]\nu[/itex]) in Planck's law represents frequency. What is the relationship between frequency and wavelength?
 
Apologies for not getting back sooner, I had the wrong email attached to this account. Thanks for the response, I feel silly on some of my oversights such as e (need to look on my calculator more).
 

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