Atomic Structure, Radiative Transition

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Einstein Coefficients andOscillator Strengthwlu=B Jluνul432π2B = d j( ω ), B B3chlu 2 ul ul ul=lu4 3πνul364 dulAul=3chOscillator Strengthf2 24πeclassicalB = f = B fhνmclu lu lu luul2lu

X線天文衛星すざくを用いた超新星残骸 Cygnus Loop 西の破れ領域の ...

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(SpaceWire Test Module)の開発 - 大阪大学X線天文グループ

Dipole Approximation∫rφ e I d xr r* ik ⋅3f⋅ ∇jφir r rik ⋅r 1 r r 2e = 1 + ik ⋅ + ( ik⋅ ) + ...2rd ≡ e ∑jj∑24πr r 2wfi = ( l ⋅d) ( )2fij ωfih c24π2 wfi = d ( )2 fij ωfih c•

Einstein Coefficients andOscillator Strengthwlu=B Jluνul432π2B = d j( ω ), B B3chlu 2 ul ul ul=lu4 3πνul364 dulAul=3chOscillator Strengthf2 24πeclassicalB = f = B fhνmclu lu lu luul2lu

Page 4 and 5: Bohr Model• E=-Z 2 /n 2 BohrModel
Page 6 and 7: • H 2s(l=0)2p(l=1)• j• H 2p(
Page 8 and 9: Spectroscopic Terms • S+1• L
Page 10 and 11: H-likeAtoms• s r=0• • II,
Page 12 and 13: Symmetry vs Anti-symmetry{ }{ } ψ
Page 14 and 15: Exchange EnergyH = e / rH = ϕH ϕd
Page 16: He-atomII,
Page 19: Transition Probabilityw=4πh TH( ω

Atomic Structure, Radiative Transition

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