# Spectroscopy Spectral lines The Fraunhofer spectrum Charlotte Moore Sitterly –Multiplet table –Rowland table Formalism of spectroscopy 1990 Bruce Gold.

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Spectroscopy Spectral lines The Fraunhofer spectrum Charlotte Moore Sitterly –Multiplet table –Rowland table Formalism of spectroscopy 1990 Bruce Gold Medal 1937 AJC Prize

Quantum Numbers of Atomic States Principal quantum number n defines the energy level Azimuthal quantum number l –states with l=0 called s states –states with l=1 called p states –states with l=2 called d states –states with l=3 called f states “orbits” of s states become more eccentric as n increases Electron transitions take place between adjacent angular momentum states (i.e.  l=1) –“sharp series” lines from p to higher s states –“principal series” lines from s to higher p states –“diffuse series” lines from p to higher d states –“fundamental series” lines from d to higher f states The first line(s) of the principal series (s to p) are called resonance lines since it involves the ground level In alkali metals, the p, d, and f energy levels are doubled (e.g. the Na D lines) due to the coupling between the magnetic moment of the orbital motion and the spin of the electron (the quantum number s, which can be +1/2 or –1/2

Spectroscopic Notation The total angular momentum quantum number is j –For s states, j=1/2 –For p states, j=1/2 or j=3/2 Electron levels are designated by the notation “n 2 (L) J ” n is the total quantum number The superscript 2 indicates the levels are doubled L is the azimuthal quantum number (S,P,D,F) J denotes the angular momentum quantum number For the sodium ground level is 3s 2 S 1/2 The two lowest p levels are 3p 2 P 1/2 and 3p 2 P 3/2 The Na D lines are described 3s 2 S ½ - 3p 2 P 3/2  5889.953 and 3s 2 S ½ - 3p 2 P 1/2 5895.923 * This is a different S than the s state!

More Spectroscopic Vocabulary The Pauli exclusion principle requires that two s-electrons in the same state must have opposite spin Therefore S=0 and these are called “singlet” states The ground state of He is a singlet state – 1 S 0 –The superscript 1 means singlet –The subscript 0 means J=0 In the first excited state of He, one electron is in the 1s state, and the second can be in either the 2s or the 2p state. Depending on how the electrons’ spins are aligned, these states can either be singlets or triplets Electrons can only jump between singlet states or between triplet states

It goes on and on and on… The state of the electrons is described with a term for each electron above the closed shell. For carbon atoms, “1s 2 2s 2 2p 2 ”says there are –2 electrons in the 1s state –2 electrons in the 2s state –2 electrons in the 2p state Allowed and forbidden transitions –Transitions with  l=1 and  J=1 and 0 are allowed (except between J=0 and J=0) –Other transitions are forbidden –For some electron states there are no allowed transitions to lower energy states. Such levels are called metastable –The situation is more complex in atoms with more electrons –A multiplet is the whole group of transitions between two states, say 3 P- 3 D

Grotrian Diagram for He Struve and Wurm 1938, ApJ

Grotrian Diagram for Li I NIST

Grotrian Diagram for O I NIST

Fraunhofer Lines LinesDue To...Wavelengths (Å) A - (band)O 2 (telluric)7594 - 7621 B - (band)O 2 (telluric)6867 - 6884 CH-alpha6563 a - (band)O 2 (telluric)6276 - 6287 D - 1, 2Na5896 & 5890 EFe5270 b - 1, 2Mg5184 & 5173 cFe4958 FH-beta4861 dFe4668 eFe4384 fH-gamma4340 G (band)Fe & Ca, CH4308 gCa4227 hH-delta4102 HCa3968 KCa3934

Spectral Line Formation Classical picture of radiation Intrinsic vs. extrinsic broadening mechanisms Line absorption coefficient Radiative transfer in spectral lines

Spectral Line Formation-Line Absorption Coefficient Radiation damping (atomic absorptions and emissions aren’t perfectly monochromatic – uncertainty principle) Thermal broadening from random kinetic motion Collisional broadening – perturbations from neighboring atoms/ions/electrons) Hyperfine structure Zeeman effect

Classical Picture of Radiation Photons are sinusoidal variations of electro-magnetic fields When a photon passes by an electron in an atom, the changing fields cause the electron to oscillate Treat the electron as a classical harmonic oscillator: mass x acceleration = external force – restoring force – dissipative E&M is useful! (well…)

Atomic Absorption Coefficient N 0 is the number of bound electrons per unit volume the quantity - 0 is the frequency separation from the nominal line center the quantity  is the dielectric constant (  =1 in free space) and  g/m is the classical damping constant The atomic absorption coefficient includes atomic data (f, ,  ) and the state of the gas (N 0 ), and is a function of frequency. The equation expresses the natural broadening of a spectral line.

The Classical Damping Constant For a classical harmonic oscillator, The shape of the spectral line depends on the size of the classical damping constant For - 0 >>  /4 , the line falls off as ( - 0 ) -2 Accelerating electric charges radiate. and is the classical damping constant ( is in cm) The mean lifetime is also defined as T=1/ , where T=4.5 2

The Classical Damping Line Profile

The Classical Line Profile Look at a thin atmospheric layer between  2 (the deeper layer) and  1 The line profile is proportional to  At line center = 0, and Half the maximum depth occurs at ( - 0 )=  /4  In terms of wavelength Very small – and the same for ALL lines!

An example… The Na D lines have a wavelength of 5.9x10 -5 cm.  = 6.4 x 10 7 sec -1 The absorption coefficient per gram of Na atoms at a distance of 2A from line center can be calculated:  0 - = 1.7 x 10 11 sec -1 and N = 1/  = 2.6 x 10 22 atoms gm -1 Then  = 3.7 x 10 4 f and f=2/3, so  = 2.5 x 10 4 per gram of neutral sodium

The Abundance of Sodium In the Sun, the Na D lines are about 1% deep at a distance of 2A from line center Use a simple one-layer model of depth x (the Schuster-Schwarzschild model) Or  x=0.01, and  x=4x10 -7 gm cm -2 (recall that  Na =2.5 x 10 4 per gram of neutral sodium at a distance of 2A from line center) the quantity  x is a column density

Natural Broadening From Heisenberg's uncertainty principle: The electron in an excited state is only there for a short time, so its energy cannot have a precise value. Since energy levels are "fuzzy," atoms can absorb photons with slightly different energy, with the probability of absorption declining as the difference in the photon's energy from the "true" energy of the transition increases. The FWHM of natural broadening for a transition with an average waiting time of  t o is given by A typical value of (  ) 1/2 = 2 x 10 -4 A. Natural broadening is usually very small. The profile of a naturally broadened linen is given by a dispersion profile (also called a damping profile, a Lorentzian profile, a Cauchy curve, and the Witch of Agnesi!) of the form (in terms of frequency) where  is the "damping constant."

The Classical Damping Constant For a classical harmonic oscillator, The shape of the spectral line depends on the size of the classical damping constant For - 0 >>  /4 , the line falls off as ( - 0 ) -2 Accelerating electric charges radiate. and is the classical damping constant ( is in cm) The mean lifetime is also defined as T=1/ , where T=4.5 2

Line Absorption with QM Replace  with  ! Broadening depends on lifetime of level Levels with long lifetimes are sharp Levels with short lifetimes are fuzzy QM damping constants for resonance lines may be close to the classical damping constant QM damping constants for other Fraunhofer lines may be 5,10, or even 50 times bigger than the classical damping constant

Add Quantum Mechanics Define the oscillator strength, f: related to the atomic transition probability B ul : f-values usually tabulated as gf-values. theoretically calculated laboratory measurements solar

Collisional Broadening Perturbations by discrete encounters Change in energy approximated by a power law of the form  E = constant x r -n (r is the separation between the atom and the perturber) Perturbations by static ion fields (linear Stark effect broadening) (n=2) Self-broadening - collisions with neutral atoms of the same kind (resonance broadening, n=3) if perturbed atom or ion has an inner core of electrons (i.e. with a dipole moment) (quadratic Stark effect, n=4) Collisions with atoms of another kind (neutral hydrogen atoms) (van der Waals, n=6) Assume adiabatic encounters (electron doesn’t change level) Non-adiabatic (electron changes level) collisions also possible

Pressure Broadening –  E=constant x r -n nTypeLines AffectedPerturber 2Linear StarkHydrogenProtons, e- 3Self broadening or resonance broadening Common species Atoms of the same type 4Quadratic StarkMost, esp. in hot stars Ions, e- 6Van der WaalsMost, esp. in cool stars Neutral hydrogen

Approaches to Collisional Broadening Statistical effects of many particles (pressure broadening) –Usually applies to the wings, less important in the core Some lines can be described fully by one or the other Know your lines! The functional form for collisional damping is the same as for radiation damping, but  rad is replaced with  coll Collisional broadening is also described with a dispersion function Collisional damping is sometimes 10’s of times larger than radiation damping

Damping Coefs for Na D

Doppler Broadening Two components contribute to the intrinsic Doppler broadening of spectral lines: –Thermal broadening –Turbulence – the dreaded microturbulence! Thermal broadening is controlled by the thermal velocity distribution (and the shape of the line profile) where v r is the line of sight velocity component The Doppler width associated with the velocity v 0 (where the variance v 0 2 =2kT/m) is and is the wavelength of line center

More Doppler Broadening Combining these we get the thermal broadening line profile: At line center, = 0, and this reduces to Where the line reaches half its maximum depth, the total width is

Thermal + Turbulence The average speed of an atom in a gas due to thermal motion - Maxwell Boltzmann distribution. The most probably speed is given by Moving atoms are Doppler shifted, and individual atoms will absorb light at slightly different wavelengths because of the Doppler shift. Spectral lines are also Doppler broadened by turbulent motions in the gas. The combination of these two effects produces a Doppler-broadened profile: Typical values for  1/2 are a few tenths of an Angstrom. The line depth for Doppler broadening decreases exponentially from the line center.

Combining the Natural, Collisional and Thermal Broadening Coefficients The combined broadening coefficient is just the convolution of all of the individual broadening coefficients The natural, Stark, and van der Waals broadening coefficients all have the form of a dispersion profile: With damping constants (  rad,  2,  4,  6 ) one simply adds them up to get the total damping constant: The thermal profile is a Gaussian profile:

The Voigt Profile The convolution of a dispersion profile and a Gaussian profile is known as a Voigt profile. Voigt functions are tabulated for use in computation In general, the shapes of spectra lines are defined in terms of Voigt profiles Voigt functions are dominated by Doppler broadening at small , and by radiation or collisional broadening at large  For weak lines, it’s the Doppler core that dominates. In solar-type stars, collisions dominate , so one needs to know the damping constant and the pressure to compute the line absorption coefficient For strong lines, we need to know the damping parameters to interpret the line.

Calculating Voigt Profiles Tabulated as the Hjerting function H(u,a) u=  /  D a=( 2 /4  c)/  D =(  /4  )  D Hjertung functions are expanded as: H(u,a)=H 0 (u) + aH 1 (u) + a 2 H 2 (u) + a 3 H 3 (u) +… or, the absorption coefficient is

Plot a Damped Profile

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