Use LEFT and RIGHT arrow keys to navigate between flashcards;
Use UP and DOWN arrow keys to flip the card;
H to show hint;
A reads text to speech;
67 Cards in this Set
- Front
- Back
femto (f)
|
10^(-15)
|
|
pico (p)
|
10^(-12)
|
|
tera (T)
|
10^12
|
|
giga (G)
|
10^9
|
|
mega (M)
|
10^6
|
|
kilo (k)
|
10^3
|
|
centi (c)
|
10^(-2)
|
|
milli (m)
|
10^(-3)
|
|
micro (mu)
|
10^(-6)
|
|
nano (n)
|
10^(-9)
|
|
joule
|
kg*m^2*s^(-2)
|
|
coulomb
|
A*s
|
|
hertz
|
s^(-1)
|
|
electron mass m
|
9.11 × 10^(-31) kg
|
|
speed of light c
|
2.998 x 10^8 m/s
|
|
equation for speed, wavelength, and frequency of electromagnetic radiation
|
c = lambda*nu
|
|
order of electromagnetic spectrum
|
gamma, X, UV, visible (violet to red), infrared, microwave, radio
|
|
along the electromagnetic spectrum, wavelength _____
|
increases
|
|
along the electromagnetic spectrum, frequency _______
|
decreases
|
|
along the electromagnetic spectrum, energy ________
|
decreases
|
|
range of wavelengths of visible light spectrum
|
390 nm (blue) to 760 nm (red)
|
|
constructive interference
|
in-phase, amplitudes combine
|
|
destructive interference
|
out-of-phase (by 1/2 lambda), amplitudes cancel
|
|
diffraction
|
dispersion of a light beam into different wavelength components because of interference
|
|
refraction
|
bending of light (due to change in speed) when it passes from one medium to another
|
|
Lyman series
|
(UV emission lines for H) nf=1
|
|
Balmer series
|
(visible emission lines for H) nf = 2
|
|
Pashen series
|
(IR emission lines for H) nf = 3
|
|
blackbody radiation
|
light emitted by heated solids
|
|
Rayleigh-Jeans law for blackbody
|
equation predicts inverse relationship between energy density and wavelength
|
|
Planck's constant h
|
h = 6.62607 x 10^(-34) J s
|
|
Planck's equation for energy of a photon given frequency
|
E = h*nu
|
|
Planck's equation for energy of a photon given wavelength
|
E = h*c/lambda
|
|
photoelectric effect
|
when light hits the surface of some metals, electrons are ejected
|
|
kinetic energy of emitted electron given velocity
|
KEe = (1/2)m*u^2
|
|
work function definition
|
energy binding electron to surface
|
|
work function phi given threshold frequency
|
phi = h*nu0
|
|
kinetic energy of emitted photoelectrons given work function, frequency
|
KEe = h*nu - phi = h*nu - h*nu0
|
|
bohr radius a0
|
a0 = 52.9 pm
|
|
radius rn of orbit n given Z
|
rn = n^2 *a0/Z
|
|
energy of orbit n given Z
|
En = -Z^2*h*c*Rh/n^2
|
|
Davisson & Germer (and Thompson) experiment
|
confirm wave properties of electrons using electron diffraction
|
|
de Broglie equation for wavelength of matter given velocity, mass
|
lambda = h/u*m
|
|
uncertainty in momentum given uncertainty in position, or vice versa
|
dx*dp >/= h/4pi
|
|
the square of the wavefunction describes _________
|
the probability of finding the electron in space (this probability determines orbital shape)
|
|
principle quantum number n
|
n=1, 2, 3, 4,... determines numbers of principal electronic shells
|
|
orbital angular momentum l
|
l may be zero or a positive integer, but not larger than n-1. determines shape. (s=0, p=1, d=2, f=3)
|
|
magnetic quantum number ml
|
may be integer from -l to l. determines orientation. (e.g. d=-2, -1, 0, 1, 2. so d has 5 orbitals)
|
|
s type orbitals
|
1 orbital. sphere. l = 0
|
|
p type orbitals
|
3 orbitals, represented as px, py, pz. two balloons tied together. l = 1
|
|
d type orbitals
|
5 orbitals. four balloons tied together. l = 2
|
|
f type orbitals
|
7 orbitals. l=3
|
|
spin quantum number ms
|
ms = +/- (1/2). determines electron spin
|
|
paramagnetic
|
atom has unpaired electrons
|
|
stern-gerlach experiment
|
demonstrates magnetic fields generated by electrons. atoms with unpaired electrons go up or down, while diamagnetic atoms go straight
|
|
exception to rule of minimum energy configuration
|
groups starting with chromium and copper: electron abandons s orbital for the d orbital
|
|
Pauli exclusion principle
|
all electrons in an atom have different quantum numbers
|
|
Hund's rule
|
an atom tends to have as many unpaired electrons as possible
|
|
ultraviolet catastrophe
|
(failure of Rayleigh-Jeans law for blackbody) energy density goes to infinity as wavelength gets smaller
|
|
|
|
|
orbital energy En given effective nuclear charge Zeff
|
En = -Zeff^2*h*c*Rh/n^2
|
|
ionization energy
|
absorption energy for ni=1, nf=infinity
|
|
ionization energy given Z
|
dEie = Z^2*h*c*Rh
|
|
atomic radius increases
|
left and down
|
|
ionization energy increases
|
right and up
|
|
electron affinity increases
|
right and up
|
|
for isoelectronic cations, the more positive the charge, the _______ the ionic radius
|
smaller
|