Scattering Polarization Zeeman Effect 3 Hanle Effect

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Lecture 4: Polarimetry 2 Outline 1 Scattering Polarization 2 Zeeman Effect 3 Hanle Effect

Transcript of Scattering Polarization Zeeman Effect 3 Hanle Effect

Page 1: Scattering Polarization Zeeman Effect 3 Hanle Effect

Lecture 4: Polarimetry 2

Outline

1 Scattering Polarization2 Zeeman Effect3 Hanle Effect

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Scattering Polarization

Single Particle Scatteringlight is absorbed and re-emittedif light has low enough energy, no energy transfered to electron,but photon changes direction⇒ elastic scatteringfor high enough energy, photon transfers energy onto electron⇒inelastic (Compton) scatteringThomson scattering on free electronsRayleigh scattering on bound electronsbased on very basic physics, scattered light is linearly polarized

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Polarization as a Function of Scattering Angle

same variation of polarization with scattering angle applies toThomson and Rayleigh scatteringscattering angle θprojection of amplitudes:

1 for polarization direction perpendicular to scattering planecos θ for linear polarization in scattering plane

intensities = amplitudes squaredratio of +Q to −Q is cos2 θ (to 1)total scattered intensity (unpolarized = averaged over allpolarization states) proportional to 1

2

(1 + cos2 θ

)

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Limb Darkening

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Solar Continuum Scattering Polarization

Stenflo 2005

due to anisotropy of the radiation fieldanisotropy due to limb darkeninglimb darkening due to decreasing temperature with heightlast scattering approximation without radiative transfer

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Solar Spectral Line Scattering Polarization

resonance lines exhibit “large” scattering polarization signals

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Jupiter and Saturn

(courtesy H.M.Schmid and D.Gisler)

Planetary Scattered Light

Jupiter, Saturn show scatteringpolarizationmultiple scattering changespolarization as compared to singlescatteringmuch depends on cloud heightcan be used to study extrasolarplanetary systemsExPo instrument development atUU

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Zeeman Effect

photos.aip.org/

Splitting/Polarization of Spectral Linesdiscovered in 1896 by Dutch physicistPieter Zeemandifferent spectral lines show differentsplitting patternssplitting proportional to magnetic fieldsplit components are polarizednormal Zeeman effect with 3components explained by H.A.Lorentzusing classical physicssplitting of sodium D doublet could notbe explained by classical physics(anomalous Zeeman effect)quantum theory and electron’s intrinsicspin led to satisfactory explanation

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Quantum-Mechanical Hamiltionianclassical interaction of magnetic dipol moment ~µ and magneticfield given by magnetic potential energy

U = −~µ · ~B

~µ the magnetic moment and ~B the magnetic field vectormagnetic moment of electron due to orbit and spinHamiltonian for quantum mechanics

H = H0 + H1 = H0 +e

2mc

(~L + 2~S

)~B

H0 Hamiltonian of atom without magnetic fieldH1 Hamiltonian component due to magnetic field

e charge of electronm electron rest mass~L the orbital angular momentum operator~S the spin operator

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Energy States in a Magnetic Field

energy state 〈ENLSJ | characterized bymain quantum number N of energy stateL(L + 1), the eigenvalue of ~L2

S(S + 1), the eigenvalue of ~S2

J(J + 1), the eigenvalue of ~J2,~J = ~L + ~S being the total angular momentumM, the eigenvalue of Jz in the state 〈NLSJM|

for the magnetic field in the z-direction, the change in energy isgiven by

∆ENLSJ(M) = 〈NLSJM|H1|NLSJM〉

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The Landé g Factor

based on pure mathematics (group theory, Wiegner Eckarttheorem), one obtains

∆ENLSJ(M) = µ0gLBM

with µ0 = e~2m the Bohr magneton, and gL the Landé g-factor

in LS coupling where B sufficiently small compared to spin-orbitsplitting field

gL = 1 +J(J + 1) + L(L + 1)− S(S + 1)

2J(J + 1)

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hyperphysics.phy-astr.gsu.edu/hbase/quantum/sodzee.html

Spectral Lines -Transitions betweenEnergy States

spectral lines aredue to transitionsbetween energystates:

lower level with 2Jl + 1sublevels Ml

upper level with 2Ju + 1sublevels Mu

not all transitionsoccur

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Selection rulenot all transitions between two levels are allowedassuming dipole radiation, quantum mechanics gives us theselection rules:

Lu − Ll = ∆L = ±1Mu −Ml = ∆M = 0,±1Mu = 0 to Ml = 0 is forbidden for Ju − Jl = 0

total angular momentum conservation: photon always carriesJphoton = 1normal Zeeman effect: line splits into three components because

Landé g-factors of upper and lower levels are identicalJu = 1 to Jl = 0 transition

anomalous Zeeman effect in all other cases

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Effective Landé Factor and Polarized Componentseach component can be assigned an effective Landé g-factor,corresponding to how much the component shifts in wavelengthfor a given field strengthcomponents are also grouped according to the linear polarizationdirection for a magnetic field perpendicular to the line of sightπ components are polarized parallel to the magnetic field (pi for

parallel)σ components are polarized perpendicular to the magnetic field

(sigma for German senkrecht)

for a field parallel to the line of sight, the π-components are notvisible, and the σ components are circularly polarized

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Bernasconi et al. 1998

Zeeman Effect in Solar Physicsdiscovered in sunspots byG.E.Hale in 1908splitting small except for insunspotsmuch of intensity profile dueto non-magnetic area⇒filling factora lot of strong fields outside ofsunspotsfull Stokes polarizationmeasurements are key todetermine solar magneticfields180 degree ambiguity

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Fully Split Titanium Lines at 2.2µm

Rüedi et al. 1998

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Hanle Effect

Bianda et al. 1998

Depolarization and Rotationscattering polarizationmodified by magnetic fieldprecession around magneticfield depolarizes and rotatespolarizationsensitive ∼ 103 times smallerfield strengths that Zeemaneffectmeasureable effects even forisotropic field vectororientations