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PHYS-307 Midterm Questions With 100% Correct Answers 2024/2025

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PHYS-307 Midterm Questions With 100% Correct Answers 2024/2025 Energy as a function of quantum number - ANS-= -13.6 eV (Z²/n²) lifetime of an orbit/time to decay to lower energy level - ANS-t = E/(dE/dt) = E_n/P = 4.7x10^-11 s (h⁶/Z⁴) energy difference between two states, n1 and n2: - AN...

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PHYS-307 Midterm Questions With 100% Correct Answers 2024/2025
Energy as a function of quantum number - ANS-✔✔= -13.6 eV (Z²/n²)



lifetime of an orbit/time to decay to lower energy level - ANS-✔✔t = E/(dE/dt) = E_n/P

= 4.7x10^-11 s (h⁶/Z⁴)



energy difference between two states, n1 and n2: - ANS-✔✔∆E = 13.6 eV (Z²) [1/n₁² - 1/n₂²]



photon energy in terms of wavelength - ANS-✔✔∆E = hv = hc/λ



wavelength in terms of frequency - ANS-✔✔λ=c/f



transition wavelength - ANS-✔✔1/λ_ab = R(1/n_b² - 1/n_a²)



Kinetic energy of an outgoing electron - ANS-✔✔m_e v²/2 - ∆E



energy of a photon - ANS-✔✔E = hv



thermal broadening - ANS-✔✔depends on temperature and composition of a gas



Root-Mean-Square Speed (v_rms)) - ANS-✔✔v_rms = (2kT/m)^(1/2)



relation between kinetic energy and thermal energy of a particle - ANS-✔✔1/2 mv² = kT

,What is the maximum of the Maxwell-Boltzmann distribution, and how do we find it? What does it
represent? - ANS-✔✔v_p = (2kT/m)^1/2



It represents the most probable speed for a particle



average speed of a particle - ANS-✔✔<v> = 1.6 (kT/m)^1/2



mean kinetic energy per particle: - ANS-✔✔<E> = 3/2 kT



Rotational Broadening - ANS-✔✔seen in rapidly rotating objects



Which three types of broadening are all very general Doppler-based motion/line-of-sight effects? - ANS-
✔✔thermal, turbulent, and rotational broadening



optical depth - ANS-✔✔a measure of how much the intensity of light is attenuated by traveling through
the gas



T(x) = σN(x)

if N is constant:

T(x) = σnx



optically thin - ANS-✔✔T(x) << 1

σnx << 1



optically thick - ANS-✔✔T(x) >> 1

σnx >> 1

,mean free path (mfp) - ANS-✔✔average distance a photon will travel through a gas before being
absorbed

-for a gas with constant n and σ:

<x> = 1/nσ



mfp is the distance over which the optical depth grows from T=0 to T=1



Curve of growth:

Describe line and profile anatomy at low optical depth T₀<1 - ANS-✔✔the shape and width of the
absorption line is determined by thermal Doppler broadening

-Gaussian shape, width depends on temperature and molecular mass of absorbing particles. the wings
are weak



Curve of growth:

Describe line and profile anatomy at larger optical depth, 1<T₀<10⁴ - ANS-✔✔the line core saturates,
the line is black at the center because none of the photons with a wavelength enar the line center make
it through the absorbing gas. the width of the line only grows slowly with optical depth



Curve of growth:

Describe line and profile anatomy at very large optical depth, T₀>10⁴ - ANS-✔✔the cumulative effects
of the (v-v₀)² wings of the Lorentz profile are important. the column density of atoms is now so large
that photons far from the center (|v-v₀|>>γ) have a fair probability at being absorbed

-even at low resolution, absorption lines are easily detected and measured



equivalent width - ANS-✔✔width of a rectangle from continuum to zero with the same area as a line;
use FWHM or triangle approximation

W = ∫(I_cont-I_line)/I_cont dλ = ∫[1-e^(-Tλ)]dλ

, curve of growth - ANS-✔✔a plot of an absorption line's equivalent width W as a function of T₀ (or a
function of column density N of the absorbing atoms) with 3 parts



Local Thermodynamic Equilibrium - ANS-✔✔all particles characterized by the same temperature T,
where:

½mv² = (3/2)kT;

all molecules have frequent collisions, so they all have the same average kinetic energy and temperature



What do we need to achieve LTE with photons? - ANS-✔✔1. a high number density of photons and
massive particles (nuclei)

2. optically thick at all wavelengths- otherwise particles, photons are decoupled



What does the Boltzmann equation tell us? - ANS-✔✔gives the relationship between the number of
atoms in one excitation state to another, e.g., n₂/n₁, and allows us to relate what we see in spectral lines
to the physical conditions of the gas



Trends for a fixed E_B and E_A, and for a fixed T in the Boltzmann equation - ANS-✔✔1. As T → ∞,
N_B/N_A → g_B/g_A

2. As T → 0 , N_B/N_A → 0



When T is fixed:

1. As E_B increases, or E_A-E_B→∞, N_B/N_A→0

2. as E_A-E_B → -kT, N_B/N_A → e-¹

3. As E_A-E_B → 0 , N_B/N_A → g_B/g_A



What is different between the Saha and Boltzmann equations? - ANS-✔✔electron density dependence

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