PHOTONS IN CHEMISTRY OUT WHY BOTHER?. E = h ν λν = c [3 10 8 m/s]

Slides:



Advertisements
Similar presentations
Laurea specialistica in Scienza e Ingegneria dei Materiali
Advertisements

Atmospheric chemistry
Laser physics EAL 501 Lecture 3. Energy units 1 eV= 1.6x (C) x 1 V= 1.6x J E =hc/ λ 1/λ=E/hc=1J/(6.6x x10 8 x100) 1 cm -1 =1.5 x
Journal Club: Introduction to Fluorescence Spectroscopy and Microscopy Avtar Singh 4/5/11.
Lecture 6 nitrogen and ozone photochemistry Regions of Light Absorption of Solar Radiation.
Bound – Bound Transitions. Bound Bound Transitions2 Einstein Relation for Bound- Bound Transitions Lower State i : g i = statistical weight Lower State.
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.
Lecture 36 Electronic spectroscopy (c) So Hirata, Department of Chemistry, University of Illinois at Urbana-Champaign. This material has been developed.
Physical Chemistry 2 nd Edition Thomas Engel, Philip Reid Chapter 25 Electronic Spectroscopy.
Lecture 3 Kinetics of electronically excited states
METO 621 LESSON 7. Vibrating Rotator If there were no interaction between the rotation and vibration, then the total energy of a quantum state would be.
Spectroscopy 1: Rotational and Vibrational Spectra CHAPTER 13.
Lecture 30 11/14/05. Spectrophotometry Properties of Light h = x J-s c = 3.00 x 10 8 m/s.
Introduction to radiative transfer
METO 621 Lesson 5. Natural broadening The line width (full width at half maximum) of the Lorentz profile is the damping parameter, . For an isolated.
Photochemical kinetics Intensity Transmittance Absorbance.
NB 2: The photophysics Is hidden in σ (So we haven’t done much yet) 1.
Introduction to Infrared Spectrometry Chap 16. Infrared Spectral Regions Table 16-1 Most used – 15.
7. Optical Processes in Molecules American Dye Source, Inc The intensities of the spectral lines 7.2. Linewidths 7.3. The.
Some of this weeks seminars: Dynamical Studies of the Photodissociation of Ozone: From the Near IR to the VUV February 12 | 4-5 p.m. | Pitzer Auditorium,
PHOTONS IN CHEMISTRY OUT. PHOTONS IN CHEMISTRY OUT WHY BOTHER?
LESSON 4 METO 621. The extinction law Consider a small element of an absorbing medium, ds, within the total medium s.
Chapter 6 Characteristics of Atoms Department of Chemistry and Biochemistry Seton Hall University.
METO 637 LESSON 3. Photochemical Change A quantum of radiative energy is called a photon, and is given the symbol h Hence in a chemical equation we.
LECTURE 6, SEPTEMBER 9, 2010 ASTR 101, SECTION 3 INSTRUCTOR, JACK BRANDT 1ASTR 101-3, FALL 2010.
Suprit Singh Talk for the IUCAA Grad-school course in Inter-stellar medium given by Dr. A N Ramaprakash 15 th April 2KX.
Transition Probabilities of Atoms and Molecules. Einstein’s analysis: Consider transitions between two molecular states with energies E 1 and E 2 (where.
UV-Vis spectroscopy Electronic absorption spectroscopy.
Photochemistry Lecture 1 Electronic excitation of atoms and molecules.
Lecture 4 Intramolecular energy transfer
Pat Arnott, ATMS 749, UNR, 2008 Chapter 9: Absorption by Atmospheric Gases Visible and UV Absorption: due to electronic transitions. Monatomic - polyatomic.
Vibrational and Rotational Spectroscopy
1 Part III Physical Chemistry III Points and credit: Approximately 20% for quiz & homework 80% final examination Note*Extra.
Photochemistry Reactions involving photons. (Radiation-induced chemical processes: chemical transformations induced by high energy photons. Radiochemistry.
Gas Absorption Line Broadening April 6. Summary in Words of Gas Transitions 3 types of quantized transitions important to us: Electronic (highest energy:
Chapters 9, 11, 12 Concepts covered that will also be candidates for exam questions.
B.SC.II PAPER-B (OPTICS and LASERS)
Radiation In astronomy, the main source of information about celestial bodies and other objects is the visible light or more generally electromagnetic.
Can we build individual molecules atom by atom? Mikkel F. Andersen Jack Dodd Centre for Quantum Technology, Department of Physics, University of Otago.
Absorption and Emission of Radiation:
Ch ; Lecture 26 – Quantum description of absorption.
441 Chem Introduction to Spectroscopy CH-1 1. Introduction to Spectroscopy Set of methods where interaction of electromagnetic radiation with chemical.
Chapters: 3and 4. THREE MAIN LIGHT MATTER INTERRACTION Absorption: converts radiative energy into internal energy Emission: converts internal energy into.
MODULE 26 (701) RADIATIONLESS DEACTIVATION OF EXCITED STATES We have used terms such as "internal conversion" and "intersystem crossing" without thinking.
§10. 6 Photochemistry. 6.1 Brief introduction The branch of chemistry which deals with the study of chemical reaction initiated by light. 1) Photochemistry.
23.7 Kinetics of photochemical reactions
Quantitative Chemical Analysis Seventh Edition Quantitative Chemical Analysis Seventh Edition Chapter 18 Fundamentals of Spectrophotometry Copyright ©
Mechanisms of enzyme inhibition Competitive inhibition: the inhibitor (I) binds only to the active site. EI ↔ E + I Non-competitive inhibition: binds to.
1.1 What’s electromagnetic radiation
Chapter – 7 Line Width Line Width (natural) Oscillator strength
Time independent H o  o = E o  o Time dependent [H o + V(t)]  = iħ  /  t Harry Kroto 2004 Time dependent Schrödinger [H o + V(t)]  = iħ  / 
Lecture 36 Electronic spectroscopy. Electronic spectroscopy Transition energies between electronic states fall in the range of UV/vis photons. UV/vis.
Chapter 8. Molecular Motion and Spectroscopy
Spectral Line Formation
MOLECULAR SPECTROSCOPY
Shanxi University Atomic Physics Chapter 7 The interaction of atoms with radiation Atomic Physics.
Saturation Roi Levy. Motivation To show the deference between linear and non linear spectroscopy To understand how saturation spectroscopy is been applied.
Spectroscopy.
Midterm 2 (53 students wrote the exam)
Ultrafast processes in molecules
CHAPTER 9 Molecules Rotations Spectra Complex planar molecules
Lecture 4 Intramolecular energy transfer
Really Basic Optics Instrument Sample Sample Prep Instrument Out put
Only three lines observed R(0) R(1) P(1)
Diatomic molecules
Einstein Coefficients
10.3 NMR Fundamentals nuclear spin calculations and examples
Chapter 9: Absorption by Atmospheric Gases
23.7 Kinetics of photochemical reactions
Presentation transcript:

PHOTONS IN CHEMISTRY OUT WHY BOTHER?

E = h ν

λν = c [ m/s]

~ nm Take 500 nm

Boltzman T [ o K]n 2 /n x x x ,0006 x ,0003 x ,4001 % 10, % 20,00024 % 50,00056 %

Grotthuss-Draper law: Only the light absorbed in a molecule can produce photochemical Change in the molecule (1871 and 1841) Stark - Einstein: If a species absorbs radiation, then one particle is excited for each quantum of radiation absorbed

Stark - Einstein: If a species absorbs radiation, then one particle is excited for each quantum of radiation absorbed QUANTUM YIELD: Φ = The number of molecules of reactant consumed for each quantum of radiation absorbed Primary Φ ≤ 1 Sum of all primary Φ’s = 1

Photochemical kinetics

Transmittance Absorbance Beer’s Law

Molar extinction Coefficient ~250 L.mol -1 cm -1 Cross section ~ cm 2

NB 1: Beer fails when photochemistry happens NB 2: The photophysics Is hidden in σ (So we haven’t done much yet)

Absorption of a mixture

Photochemical kinetics STEADY STATE HYPOTESIS

NB 2: The photophysics Is hidden in σ (So we haven’t done much yet)

EINSTEIN COEFFICIENT # of transitions / second: Amplitude of TRANSITION MOMENT # of molecules degeneracy Radiation density =# of photons/unit freq.

Stimulated emission Spontaneous emission

Stimulated emission Spontaneous emission

Boltzman Planck

Oscillator strength

Lifetimes Einstein coefficients are rate constants

Heisenberg may have been here

Contributions to excited state lifetime  Natural lifetime  Pressure broadening  Saturaiton broadening  Doppler broadening NB: f(v) in a gas is Gaussian  Doppler line shape is Gausian

(depends on coordinates of electrons and nuclei And on time) electrons Nuclei

NB: Resonant frequency NB 1: I = f  e 0 and µ becomes permanent dipole NB 2: ν if as beat frequency NB 3:compare to nuclear vibrations

Compare s -1 to IR: Nuclear motion is 2 orders of Magnitude slower than Electronic motion Born-Oppenheimer approximation

Orthogonal (no overlap) tells if allowed or forbidden: must be symmetric  selection rules Franck-condon factors

M x is odd:

One more parameter………. SPIN αβ updown ↑↓ +½-½

If we can separate space and spin (no spin-orbit coupling):

Conical Intersections R1 R2 E