Descriptive Inorganic Chemistry Chem M, W Bill Vining 232 Physical Sciences Building Sit in First 8 Rows

Inorganic Chemistry One of the three descriptive chemistries: – Organic Chemistry – Biochemistry – Inorganic Chemistry  Theoretical and Practical Chemistries:  Physical Chemistry  Analytical Chemistry

Inorganic Chemistry: Chemistry for the rest of the elements.

Chem 241 Topics Origin of the Elements Nuclear Chemistry – Stability – Practical Nuclear Chemistry Chemical Formation of the Earth and Ore Obtaining the Elements: Extraction – Methods for Metals and Nonmetals Properties of the Main Group Elements – The elements themselves – Oxides, halides of the elements Bonding and Properties of Metals

Chem 241 Topics Chemistry in Water – Charge Density – Enthalpy, Entropy and Solubility – Acid-Base Properties Atmospheric Chemistry – Global Warming – Acid Rain – Ozone Coordination Chemistry – Complex Types – Bonding – Symmetry in Chemistry – Spectroscopy

Official Stuff Course Website: Text: Online pdf Grading: Three exams, including the final (not cumulative)300 points Homework100 points Element Poster Session50 points Homework: OWL Choose Chemistry General, UMass Amherst, then choose SUNY Oneonta, Chem 241 Login: SUCO + your up to sign (mine would be SUCOviningwj) Password: your A00 number

First Topic Where do all these elements come from? How are they made? Are they made?

Our Guide:

What aspects of this should we explain?

What will our explanations depend on? Thermodynamics: relative stability Kinetics: rate and mechanism

General Decrease in Abundance with Atomic Number

Even > Odd

Peak at Fe

Peak at Pb

Trough at Be

Missing Tc and Pm and Above N = 83

Nucleosynthesis of the Elements Hydrogen Burning 1 H + 1 H  2 H + e + + v e­ 2 H + 1 H  3 He +  3 He + 3 He  4 He +2 1 H Why does this happen only in stars? 4 1 H  4 He + 2e + + 2v e

Helium Burning 4 He + 4 He  8 Be 8 Be + 4 He  12 C*  12 C +  3 4 He  12 C +  Is this easier or harder than hydrogen burning?

Carbon Burning, etc. 12 C + 4 He  16 O +  16 O + 4 He  20 Ne +  20 Ne + 4 He  24 Mg +  12 C + 12 C  24 Mg +  12 C + 12 C  23 Na + 1 H 12 C + 12 C  20 Ne + 4 He Go back to initial Questions. Can we answer any?

The  -Process 20 Ne +   16 O + 4 He 20 Ne + 4 He  24 Mg +  2 20 Ne  16 O + 24 Mg +  40 Ca + 4 He  44 Ti* +  44 Ti* + e -  44 Sc* + v + 44 Sc*  44 Ca +  + + v + 44 Ca + 4 He  48 Ti + 

Interlude: Nuclear Reaction Equations

Neutron Capture-Beta Decay

r- and s-processes:

Stability of Nuclei Which nuclei exist and which are radioactive. What are the trends in nuclear binding energy.

Common types of Radioactive Decay Beta decay: Cu-66 Alpha decay: U-238 Positron emission: Electron capture:

Island of stability

The problem with Radon.

Explain trends in Island of Stability

Binding Energy How much more stable are nucleons in a nucleus than they are alone? Measured as a mass defect (loss):

Class Calculations Element protons mass number exact mass

Using Excel to do this: isotopedata_stable.xls