a short review the basic equation of transfer for radiation passing through gas: the change in...
TRANSCRIPT
![Page 1: A short review The basic equation of transfer for radiation passing through gas: the change in specific intensity I is equal to: -dI /d = I - j / =](https://reader036.vdocument.in/reader036/viewer/2022083005/56649f285503460f94c40a3b/html5/thumbnails/1.jpg)
A short review• The basic equation of transfer for
radiation passing through gas: the change in specific intensity I is equal to:
-dI /d = I - j/ = I - S
• Assumptions– LTE… (all physical processes in balance)
S= B
– Flux constant with depth– Plane parallel atmosphere
![Page 2: A short review The basic equation of transfer for radiation passing through gas: the change in specific intensity I is equal to: -dI /d = I - j / =](https://reader036.vdocument.in/reader036/viewer/2022083005/56649f285503460f94c40a3b/html5/thumbnails/2.jpg)
Black Body Radiation• walls heated• emit and reabsorb
radiation• interior of
chamber in thermodynamic equilibrium
• leakage in or out of the whole is small
• Stellar photospheres approximate blackbodies• Most photons are reabsorbed near where they are emitted• Higher in the atmosphere, a star departs from a black body
![Page 3: A short review The basic equation of transfer for radiation passing through gas: the change in specific intensity I is equal to: -dI /d = I - j / =](https://reader036.vdocument.in/reader036/viewer/2022083005/56649f285503460f94c40a3b/html5/thumbnails/3.jpg)
See: http://homepages.wmich.edu/~korista/phys325.html
![Page 4: A short review The basic equation of transfer for radiation passing through gas: the change in specific intensity I is equal to: -dI /d = I - j / =](https://reader036.vdocument.in/reader036/viewer/2022083005/56649f285503460f94c40a3b/html5/thumbnails/4.jpg)
See: http://www.jb.man.ac.uk/distance/life/sample/stars/index.html
![Page 5: A short review The basic equation of transfer for radiation passing through gas: the change in specific intensity I is equal to: -dI /d = I - j / =](https://reader036.vdocument.in/reader036/viewer/2022083005/56649f285503460f94c40a3b/html5/thumbnails/5.jpg)
See: http://astro1.panet.utoledo.edu/~ndm/4810.html
![Page 6: A short review The basic equation of transfer for radiation passing through gas: the change in specific intensity I is equal to: -dI /d = I - j / =](https://reader036.vdocument.in/reader036/viewer/2022083005/56649f285503460f94c40a3b/html5/thumbnails/6.jpg)
Black Bodies - Observations
• spectrum continuous, isotropic, unpolarized• continuum intensity depends on frequency
and temperature• observed relation:
• From this observational result can be derived Wien’s law (peak intensity) and the Stefan-Boltzman law (luminosity)
• Also Rayleigh-Jeans approx. and Wien approx. of flux above and below BB peak
T
fI
3
![Page 7: A short review The basic equation of transfer for radiation passing through gas: the change in specific intensity I is equal to: -dI /d = I - j / =](https://reader036.vdocument.in/reader036/viewer/2022083005/56649f285503460f94c40a3b/html5/thumbnails/7.jpg)
Wien’s Law – Peak Intensity
Iis maxat max = 0.29/T ( in cm)
or’max = 0.51/T (where ’max is the wavelength at which I is max)
Thought Problem: Calculate the wavelengths at which I and I are maximum in the Sun. Think about why these are different.
![Page 8: A short review The basic equation of transfer for radiation passing through gas: the change in specific intensity I is equal to: -dI /d = I - j / =](https://reader036.vdocument.in/reader036/viewer/2022083005/56649f285503460f94c40a3b/html5/thumbnails/8.jpg)
Luminosity – Stefan Boltzman Law
• F = T4 or L = 4 R2 T4
• Class Problem: What is the approximate absolute magnitude of a DA white dwarf with an effective temperature of 12,000, remembering that its radius is about the same as that of the Earth?– what is the simplest approach?
![Page 9: A short review The basic equation of transfer for radiation passing through gas: the change in specific intensity I is equal to: -dI /d = I - j / =](https://reader036.vdocument.in/reader036/viewer/2022083005/56649f285503460f94c40a3b/html5/thumbnails/9.jpg)
Deriving the Planck Function• Several methods (2 level atom,
atomic oscillators, thermodynamics)• Use 2-level atom: Einstein
Coefficients– Spontaneous emission proportional to
Nn x Einstein probability coefficient
j = NuAulh
– Induced (stimulated) emission proportional to intensity
= NlBluh – NuBulh
![Page 10: A short review The basic equation of transfer for radiation passing through gas: the change in specific intensity I is equal to: -dI /d = I - j / =](https://reader036.vdocument.in/reader036/viewer/2022083005/56649f285503460f94c40a3b/html5/thumbnails/10.jpg)
Steps to the Planck Function
• Energy level populations given by the Boltzman equation:
• Include spontaneous and stimulated emission
• Solve for I, substitute Nu/Nl
• Note that
IBNIBNAN lululuulu
kTh
l
n
l
u eg
g
N
N /
u
lluul g
gBB ulul B
c
hA
2
32
![Page 11: A short review The basic equation of transfer for radiation passing through gas: the change in specific intensity I is equal to: -dI /d = I - j / =](https://reader036.vdocument.in/reader036/viewer/2022083005/56649f285503460f94c40a3b/html5/thumbnails/11.jpg)
Planck’s Law
• Rayleigh-Jeans Approximation (at long wavelength, h/kT is small, ex=x+1)
• Wien Approximation – (at short wavelength, h/kT is large)
1
12)(
/5
2
kThce
hcTB
1
12)(
/2
3
kThec
hTB
kThec
hI /
2
32
22
2
22 kt
ckTI
![Page 12: A short review The basic equation of transfer for radiation passing through gas: the change in specific intensity I is equal to: -dI /d = I - j / =](https://reader036.vdocument.in/reader036/viewer/2022083005/56649f285503460f94c40a3b/html5/thumbnails/12.jpg)
Class Problem
• The flux of M3’s IV-101 at the K-band is approximately 4.53 x 105 photons s–1 m–2 m-1. What would you expect the flux to be at 18 m? The star has a temperature of 4250K.
![Page 13: A short review The basic equation of transfer for radiation passing through gas: the change in specific intensity I is equal to: -dI /d = I - j / =](https://reader036.vdocument.in/reader036/viewer/2022083005/56649f285503460f94c40a3b/html5/thumbnails/13.jpg)
Using Planck’s Law
Computational form:
For cgs units with wavelength in Angstroms
1
1019.1)(
/1044.1
527
8
Txe
xTB
![Page 14: A short review The basic equation of transfer for radiation passing through gas: the change in specific intensity I is equal to: -dI /d = I - j / =](https://reader036.vdocument.in/reader036/viewer/2022083005/56649f285503460f94c40a3b/html5/thumbnails/14.jpg)
Class Problems
• You are studying a binary star comprised of an B8V star at Teff = 12,000 K and a K2III giant at Teff = 4500 K. The two stars are of nearly equal V magnitude. What is the ratio of their fluxes at 2 microns?
• In an eclipsing binary system, comprised of a B5V star at Teff = 16,000K and an F0III star at Teff = 7000K, the two stars are known to have nearly equal diameters. How deep will the primary and secondary eclipses be at 1.6 microns?
![Page 15: A short review The basic equation of transfer for radiation passing through gas: the change in specific intensity I is equal to: -dI /d = I - j / =](https://reader036.vdocument.in/reader036/viewer/2022083005/56649f285503460f94c40a3b/html5/thumbnails/15.jpg)
Class Problems
• Calculate the radius of an M dwarf having a luminosity L=10-2LSun and an effective temperature Teff=3,200 K. What is the approximate density of this M dwarf?
• Calculate the effective temperature of a proto-
stellar object with a luminosity 50 times greater than the Sun and a diameter of 3” at a distance of 200 pc.
![Page 16: A short review The basic equation of transfer for radiation passing through gas: the change in specific intensity I is equal to: -dI /d = I - j / =](https://reader036.vdocument.in/reader036/viewer/2022083005/56649f285503460f94c40a3b/html5/thumbnails/16.jpg)
Class Problems
• You want to detect the faint star of an unresolved binary system comprising a B5V star and an M0V companion. What wavelength regime would you choose to try to detect the M0V star? What is the ratio of the flux from the B star to the flux from the M star at that wavelength?
• You want to detect the faint star of an an unresolved binary system comprising a K0III giant and a DA white dwarf with a temperature of 12,000 K (and MV=10.7). What wavelength regime would you choose to try to detect the white dwarf? What is the ratio of the flux from the white dwarf to the flux from the K giant at that wavelength?