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Understanding Spectral Line Profiles in Astrophysics

Explore the limb darkening, Doppler broadening, and curve of growth in spectral line structures, analyzing red/blue shifted absorption lines and their impact on equivalent width.

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Understanding Spectral Line Profiles in Astrophysics

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  1. 0 Sirius A and B

  2. 0 Il (tl) = Il (0) e-hn/kT + Bl(T) (1 – e-hn/kT)

  3. 0 Limb Darkening

  4. 0 Structure of Spectral Lines

  5. 0 Equivalent Width W 1 0.8 0.6 Fl/Fcont 0.4 0.2 l l0

  6. 0 Doppler Broadening Red shifted abs. Blue shifted abs. vr Observer vr Atoms in random thermal motion

  7. 0 Line Profiles Gauss Profile 1 0.8 Lorentz Profile 0.6 Fl/Fcont 0.4 0.2 l l0

  8. 0 Line Profiles Increasing number of absorbing atoms 1 0.8 0.6 Fl/Fcont 0.4 0.2 l l0

  9. 0 Curve of Growth Log(W/l0) ~ √Nfl -4 ~ √log(Nfl) -4.5 -5 ~ Nfl -5.5 11 12 13 14 15 16 Log(Nfl)

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