nsci 314 life in the cosmos 3 – stars and their evolution (continued) and basic properties of life...

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NSCI 314 LIFE IN THE COSMOS 3 – STARS AND THEIR EVOLUTION (CONTINUED) AND BASIC PROPERTIES OF LIFE Dr. Karen Kolehmainen Department of Physics CSUSB COURSE WEBPAGE: http://physics.csusb.edu/~karen

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Page 1: NSCI 314 LIFE IN THE COSMOS 3 – STARS AND THEIR EVOLUTION (CONTINUED) AND BASIC PROPERTIES OF LIFE Dr. Karen Kolehmainen Department of Physics CSUSB COURSE

NSCI 314

LIFE IN THE COSMOS

3 – STARS AND THEIR EVOLUTION (CONTINUED)AND

BASIC PROPERTIES OF LIFE

Dr. Karen KolehmainenDepartment of Physics

CSUSB

COURSE WEBPAGE:http://physics.csusb.edu/~karen

Page 2: NSCI 314 LIFE IN THE COSMOS 3 – STARS AND THEIR EVOLUTION (CONTINUED) AND BASIC PROPERTIES OF LIFE Dr. Karen Kolehmainen Department of Physics CSUSB COURSE

REVIEW OF STAR FORMATION FORMED FROM A NEBULA (DENSER PART OF

THE INTERSTELLAR MEDIUM) NEBULA CONTRACTS DUE TO GRAVITY SPINS FASTER AND FLATTENS INTO A DISK

AS IT CONTRACTS GETS HOTTER, EVENTUALLY HOT ENOUGH

FOR NUCLEAR FUSION (H TO He) TO BEGIN IN THE CENTER

NOW IT IS A MAIN SEQUENCE STAR PLANETS AND SMALLER OBJECTS FORM

FROM MATERIAL LEFT OVER

Page 3: NSCI 314 LIFE IN THE COSMOS 3 – STARS AND THEIR EVOLUTION (CONTINUED) AND BASIC PROPERTIES OF LIFE Dr. Karen Kolehmainen Department of Physics CSUSB COURSE

HIGH TEMPERATURE IS NECESSARY FOR NUCLEAR FUSION. THE NUCLEI MUST BE MOVING FAST ENOUGH TO COLLIDE DESPITE THEIR ELECTRICAL REPULSION.

•IN THE CORE OF A MAIN SEQUENCE STAR, TEMPERATURE IS ABOUT 15 MILLION K (27 MILLION oF).

HYDROGEN NUCLEI (PROTONS) FUSE TO FORM HELIUM.

•FOUR 1H (PROTONS) FUSE TO ONE 4He + ENERGY.

•TWO OF THE PROTONS ARE CONVERTED TO NEUTRONS.

WHERE DOES THE ENERGY COME FROM?

•ONE 4He IS 0.7% LIGHTER THAN FOUR 1H COMBINED.

•THE LOST MASS IS CONVERTED TO ENERGY.

E = m c 2

ENERGY = MASS x (SPEED OF LIGHT)²

NUCLEAR REACTIONS IN MAIN SEQUENCE STARS

Page 4: NSCI 314 LIFE IN THE COSMOS 3 – STARS AND THEIR EVOLUTION (CONTINUED) AND BASIC PROPERTIES OF LIFE Dr. Karen Kolehmainen Department of Physics CSUSB COURSE

THE SUN CONVERTS 4 BILLION kg OF MATTER INTO ENERGY EACH SECOND.

THE SUN HAS SUFFICIENT HYDROGEN TO DO THIS FOR 100 BILLION YEARS, BUT WILL STOP AFTER ABOUT 10 BILLION YEARS BECAUSE ONLY THE CORE UNDERGOES FUSION. (THE OUTER PARTS OF THE STAR AREN’T HOT ENOUGH FOR FUSION.)

WHEN HYDROGEN IN THE CORE RUNS OUT, THIS MARKS THE END OF THE MAIN SEQUENCE LIFETIME.

THE MORE MASSIVE THE STAR, THE SHORTER THE MAIN SEQUENCE LIFETIME.

•EVEN THOUGH THERE IS MORE HYDROGEN TO FUSE, FUSION PROCEEDS SO MUCH MORE RAPIDLY (BECAUSE IT IS HOTTER) THAT THE HYDROGEN IN THE CENTER DOESN’T LAST AS LONG.

NUCLEAR REACTIONS IN MAIN SEQUENCE STARS

Page 5: NSCI 314 LIFE IN THE COSMOS 3 – STARS AND THEIR EVOLUTION (CONTINUED) AND BASIC PROPERTIES OF LIFE Dr. Karen Kolehmainen Department of Physics CSUSB COURSE

MAIN SEQUENCE STARSALL PROPERTIES OF A MAIN SEQUENCE STAR

DEPEND ON ITS MASS.–MORE MASSIVE STARS ARE LARGER.–MORE MASSIVE STARS ARE HOTTER.–MORE MASSIVE STARS ARE BLUER.–MORE MASSIVE STARS ARE BRIGHTER.–MORE MASSIVE STARS HAVE SHORTER

LIFETIMES. • EVEN THOUGH THEY HAVE MORE NUCLEAR FUEL,

THEY USE IT UP MORE QUICKLY BECAUSE OF THEIR HIGHER TEMPERATURES.

Page 6: NSCI 314 LIFE IN THE COSMOS 3 – STARS AND THEIR EVOLUTION (CONTINUED) AND BASIC PROPERTIES OF LIFE Dr. Karen Kolehmainen Department of Physics CSUSB COURSE

Brightness (Sun = 1)

SpectralType

Number of Stars in MW

Percent ofTotal

100,000

500

10

2

0.9

0.2

0.005

O

B

A

F

G

K

M

5 million

10 million

500 million

1 billion

10 billion

100 billion

1 trillion

80,000

360 million

2.4 billion

12 billion

28 billion

60 billion

290 billion

0.00002 %

0.09 %

0.6 %

3 %

7 %

15 %

73 %

Lifetime(Years)

PROPERTIES OF MAIN SEQUENCE STARS

Page 7: NSCI 314 LIFE IN THE COSMOS 3 – STARS AND THEIR EVOLUTION (CONTINUED) AND BASIC PROPERTIES OF LIFE Dr. Karen Kolehmainen Department of Physics CSUSB COURSE

AT THE END OF THE MAIN SEQUENCE LIFETIME… THE OUTER PART OF THE STAR EXPANDS (BY UP TO 200

TIMES), BRIGHTENS (BY UP TO 100 TIMES), AND COOLS TO 3,000 K. THE STAR BECOMES A RED GIANT. IN MASSIVE STARS, A SECOND STAGE OF EXPANSION AND COOLING PRODUCES A SUPERGIANT.

MEANWHILE, THE CORE CONTRACTS AND HEATS UP UNTIL HELIUM BEGINS TO FUSE TO FORM CARBON AND HEAVIER ELEMENTS.

THE STAR GOES THROUGH OCCASIONAL EPISODES OF INSTABILITY, WITH RAPID OSCILLATIONS IN SIZE, TEMPERATURE, AND BRIGHTNESS.

Page 8: NSCI 314 LIFE IN THE COSMOS 3 – STARS AND THEIR EVOLUTION (CONTINUED) AND BASIC PROPERTIES OF LIFE Dr. Karen Kolehmainen Department of Physics CSUSB COURSE

He FUSES INTO CARBON , NITROGEN AND OXYGEN + ENERGY. IN LOW MASS STARS, FUSION STOPS HERE BECAUSE IT NEVER GETS HOT ENOUGH TO FUSE C, N, AND O TO EVEN HEAVIER ELEMENTS.

IN MASSIVE STARS, CARBON FUSES TO FORM HEAVIER ELEMENTS, WHICH AGAIN FUSE TO FORM EVEN HEAVIER ELEMENTS, EVENTUALLY RESULTING IN IRON. AT EACH STEP, ENERGY IS PRODUCED.

FUSION OF IRON TO EVEN HEAVIER ELEMENTS WOULD REQUIRE ENERGY AS AN INPUT INSTEAD OF RELEASING ENERGY. (THE NUCLEUS THAT WOULD RESULT FROM FUSION IS HEAVIER THAN THE NUCLEI THAT WOULD FUSE TO FORM IT.)

THIS ENERGY IS UNAVAILABLE, SO FUSION DOESN’T PROCEED BEYOND IRON, NO MATTER HOW MASSIVE THE STAR.

NUCLEAR REACTIONS IN RED GIANTS AND SUPERGIANTS

Page 9: NSCI 314 LIFE IN THE COSMOS 3 – STARS AND THEIR EVOLUTION (CONTINUED) AND BASIC PROPERTIES OF LIFE Dr. Karen Kolehmainen Department of Physics CSUSB COURSE

LATE STAGES OF STELLAR EVOLUTION FOR SOLAR-TYPE (LOW MASS) STARS

PLANETARY NEBULA: THE OUTER PART OF THE STAR IS EJECTED. THE EJECTED MATERIAL EXPANDS, COOLS, AND ENRICHES THE INTERSTELLAR MEDIUM WITH HEAVIER ELEMENTS (FUSION PRODUCTS). THE CORE OF STAR REMAINS IN THE CENTER OF THE NEBULA, AND BECOMES A …

WHITE DWARF: CORE OF THE ORIGINAL STAR LEFT AFTER OUTER PARTS ARE EJECTED. IT SHRINKS TO ABOUT EARTH-SIZE, AND IS VERY DENSE. (A TEASPOONFUL OF WHITE DWARF MATERIAL WOULD WEIGH ABOUT A TON.) THERE IS NO MORE FUSION, SO THE WHITE DWARF COOLS AND DIMS (VERY, VERY SLOWLY) UNTIL EVENTUALLY IT BECOMES A …

BLACK DWARF: NO MORE LIGHT EMITTED. STELLAR CORPSE IS A DENSE SOLID BALL OF CARBON, NITROGEN, AND OXYGEN. THE UNIVERSE ISN'T OLD ENOUGH FOR BLACK DWARFS TO HAVE FORMED YET.

Page 10: NSCI 314 LIFE IN THE COSMOS 3 – STARS AND THEIR EVOLUTION (CONTINUED) AND BASIC PROPERTIES OF LIFE Dr. Karen Kolehmainen Department of Physics CSUSB COURSE
Page 11: NSCI 314 LIFE IN THE COSMOS 3 – STARS AND THEIR EVOLUTION (CONTINUED) AND BASIC PROPERTIES OF LIFE Dr. Karen Kolehmainen Department of Physics CSUSB COURSE

LATE STAGES OF STELLAR EVOLUTION FOR MASSIVE STARS SUPERNOVA (TYPE II)

– IRON CORE OF RED SUPERGIANT COLLAPSES UNTIL NUCLEI COLLIDE WITH EACH OTHER.

– NUCLEI BOUNCE APART VIOLENTLY, PUSHING MATERIAL OUTWARD AND CAUSING STAR TO EXPLODE.

– LOTS OF ENERGY IS RELEASED IN EXPLOSION, STAR BRIGHTENS ENORMOUSLY.

– ENERGY OF EXPLOSION CAUSES FUSION OF HEAVY ELEMENTS (EVEN HEAVIER THAN IRON).

– EJECTED MATERIAL FORMS A SUPERNOVA REMNANT, WHICH EXPANDS AND ADDS MATERIAL (ENRICHED IN HEAVY ELEMENTS) TO THE INTERSTELLAR MEDIUM.

NEUTRON STAR OR BLACK HOLE: CORE OF ORIGINAL STAR LEFT OVER AFTER THE SUPERNOVA EXPLOSION, EXTREMELY DENSE

Page 12: NSCI 314 LIFE IN THE COSMOS 3 – STARS AND THEIR EVOLUTION (CONTINUED) AND BASIC PROPERTIES OF LIFE Dr. Karen Kolehmainen Department of Physics CSUSB COURSE

“BEFORE AND AFTER” PICTURES OF A SUPERNOVA

Page 13: NSCI 314 LIFE IN THE COSMOS 3 – STARS AND THEIR EVOLUTION (CONTINUED) AND BASIC PROPERTIES OF LIFE Dr. Karen Kolehmainen Department of Physics CSUSB COURSE
Page 14: NSCI 314 LIFE IN THE COSMOS 3 – STARS AND THEIR EVOLUTION (CONTINUED) AND BASIC PROPERTIES OF LIFE Dr. Karen Kolehmainen Department of Physics CSUSB COURSE

NEUTRON STAR BALL OF NEUTRONS (LIKE ONE BIG NUCLEUS)

MASS BETWEEN ABOUT 1.4 AND 3 SOLAR MASSES

RADIUS ABOUT 10 km

VERY HIGH DENSITY – ONE TEASPOONFUL OF NEUTRON STAR MATERIAL WOULD WEIGH A BILLION TONS

MANY NEUTRON STARS EMIT PULSES OF RADIO WAVES AND OTHER ELECTROMAGNETIC RADIATION, AND ARE OBSERVED AS PULSARS

Page 15: NSCI 314 LIFE IN THE COSMOS 3 – STARS AND THEIR EVOLUTION (CONTINUED) AND BASIC PROPERTIES OF LIFE Dr. Karen Kolehmainen Department of Physics CSUSB COURSE

BLACK HOLE IF THE STELLAR CORE LEFT AFTER A

SUPERNOVA IS SUFFICIENTLY MASSIVE (MORE THAN ABOUT 3 SOLAR MASSES), IT COLLAPSES TO FORM A BLACK HOLE

EVEN HIGHER DENSITY THAN A NEUTRON STAR

ESCAPE VELOCITY EXCEEDS THE SPEED OF LIGHT

Page 16: NSCI 314 LIFE IN THE COSMOS 3 – STARS AND THEIR EVOLUTION (CONTINUED) AND BASIC PROPERTIES OF LIFE Dr. Karen Kolehmainen Department of Physics CSUSB COURSE

ESCAPE VELOCITY SPEED NEEDED WHEN TAKING OFF FROM THE SURFACE OF

A PLANET OR OTHER OBJECT IN ORDER TO ESCAPE THE OBJECT’S GRAVITY (TECHNICALLY, TO ESCAPE TO AN INFINITE DISTANCE AWAY, SLOWING TO ZERO SPEED IN THE PROCESS).

EARTH'S ESCAPE VELOCITY IS 11 km/s.

THE MORE MASSIVE THE OBJECT YOU'RE ESCAPING FROM, THE LARGER THE ESCAPE VELOCITY.

THE SMALLER THE RADIUS OF THE OBJECT YOU'RE ESCAPING FROM, THE LARGER THE ESCAPE VELOCITY.

THEREFORE, A MASSIVE BUT SMALL OBJECT (i.e., A DENSE OBJECT) HAS A LARGE ESCAPE VELOCITY.

Page 17: NSCI 314 LIFE IN THE COSMOS 3 – STARS AND THEIR EVOLUTION (CONTINUED) AND BASIC PROPERTIES OF LIFE Dr. Karen Kolehmainen Department of Physics CSUSB COURSE

BLACK HOLE ESCAPE VELOCITY EXCEEDS THE SPEED OF LIGHT. THEREFORE NOTHING CAN ESCAPE, NOT EVEN LIGHT. AN “EVENT HORIZON” SEALS OFF THE INTERIOR FROM THE REST

OF THE UNIVERSE. THE EVENT HORIZON HAS A RADIUS OF SEVERAL km FOR A

STELLAR MASS BLACK HOLE. MATTER INSIDE EVENT HORIZON PROBABLY CONTRACTS TO A

“SINGULARITY” – INFINITE DENSITY! CAN SOMETIMES BE DETECTED VIA GRAVITATIONAL EFFECTS

ON OTHER OBJECTS (E.G., IN A DOUBLE STAR SYSTEM) AND/OR VIA X-RAYS EMITTED BY MATTER FALLING IN.

IN ADDITION TO STELLAR-MASS BLACK HOLES FORMED AT END OF LIVES OF MASSIVE STARS, LARGER BLACK HOLES EXIST IN THE CENTER OF MOST GALAXIES (INCLUDING THE MILKY WAY).

Page 18: NSCI 314 LIFE IN THE COSMOS 3 – STARS AND THEIR EVOLUTION (CONTINUED) AND BASIC PROPERTIES OF LIFE Dr. Karen Kolehmainen Department of Physics CSUSB COURSE

A CLOSED SYSTEM AND ITS ENVIRONMENT

CLOSED SYSTEM

MATTER ENERGY

MATTER ENERGY

Page 19: NSCI 314 LIFE IN THE COSMOS 3 – STARS AND THEIR EVOLUTION (CONTINUED) AND BASIC PROPERTIES OF LIFE Dr. Karen Kolehmainen Department of Physics CSUSB COURSE

AN OPEN SYSTEM AND ITS ENVIRONMENT

OPEN SYSTEM

MATTER ENERGY

WASTE ENERGYWASTE MATTER

Page 20: NSCI 314 LIFE IN THE COSMOS 3 – STARS AND THEIR EVOLUTION (CONTINUED) AND BASIC PROPERTIES OF LIFE Dr. Karen Kolehmainen Department of Physics CSUSB COURSE

ENTROPY AND ORDER ENTROPY: A MEASURE OF THE DISORDER IN A

SYSTEM

– LOW ENTROPY = HIGHLY ORDERED

– HIGH ENTROPY = VERY DISORDERED OR MESSY SECOND LAW OF THERMODYNAMICS:

– IN ANY CLOSED SYSTEM (MEANING THAT NOTHING ENTERS OR LEAVES), NO PROCESS CAN OCCUR IN WHICH THE SYSTEM'S ENTROPY DECREASES. IN OTHER WORDS, A CLOSED SYSTEM CAN'T BECOME MORE ORDERED (LESS MESSY) AS TIME GOES ON.

– THEREFORE, THE AMOUNT OF DISORDER IN A CLOSED SYSTEM EITHER INCREASES WITH TIME OR IT DOESN’T CHANGE WITH TIME. USUALLY, THE ENTROPY INCREASES WITH TIME, i.e., A CLOSED SYSTEM GETS MESSIER AS TIME GOES ON.

Page 21: NSCI 314 LIFE IN THE COSMOS 3 – STARS AND THEIR EVOLUTION (CONTINUED) AND BASIC PROPERTIES OF LIFE Dr. Karen Kolehmainen Department of Physics CSUSB COURSE

ENTROPY AND ORDER

SECOND LAW OF THERMODYNAMICS: IN ANY CLOSED SYSTEM, NO PROCESS CAN OCCUR IN WHICH THE ENTROPY DECREASES WITH TIME, i.e., A CLOSED SYSTEM CANNOT BECOME MORE ORDERED WITH TIME.

WHAT ABOUT THE ENTROPY OF AN OPEN SYSTEM?

AN OPEN SYSTEM INTERACTS WITH ITS ENVIRONMENT. IF WE INCLUDE THE ENVIRONMENT AS PART OF THE SYSTEM (INSTEAD OF SOMETHING OUTSIDE OF THE SYSTEM), WE NOW HAVE A CLOSED SYSTEM, AND ITS TOTAL ENTROPY CAN'T DECREASE WITH TIME. HOWEVER, THE ENTROPY OF THE ORIGINAL OPEN SYSTEM CAN DECREASE, AS LONG AS THE ENTROPY OF ITS ENVIRONMENT INCREASES BY AN EVEN LARGER AMOUNT.

LIFE: ENTROPY DECREASES WITHIN AN ORGANISM AS RAW MATERIALS ARE REARRANGED IN HIGHLY ORDERED WAYS. HOWEVER, THE ORGANISM IS AN OPEN SYSTEM, AND THE ENTROPY OF ITS ENVIRONMENT INCREASES.

Page 22: NSCI 314 LIFE IN THE COSMOS 3 – STARS AND THEIR EVOLUTION (CONTINUED) AND BASIC PROPERTIES OF LIFE Dr. Karen Kolehmainen Department of Physics CSUSB COURSE

LIFE AND ITS ENVIRONMENT

ORGANISMENTROPY DECREASES

MATTER ENERGY

WASTE MATTER WASTE ENERGY

ENVIRONMENTENTROPY INCREASES

Page 23: NSCI 314 LIFE IN THE COSMOS 3 – STARS AND THEIR EVOLUTION (CONTINUED) AND BASIC PROPERTIES OF LIFE Dr. Karen Kolehmainen Department of Physics CSUSB COURSE

WHAT IS LIFE? HARD TO DEFINE, BUT LET'S LIST SOME

OF ITS PROPERTIES. NECESSARY PROPERTIES:

– USES ENERGY– INTERACTS WITH ITS ENVIRONMENT– MAINTAINS A LOW ENTROPY (HIGH DEGREE

OR ORDER OR COMPLEXITY) INTERNALLY LIKELY (BUT MAYBE NOT NECESSARY)

PROPERTIES:– GROWS AND DEVELOPS– REPRODUCES– MUTATES AND EVOLVES

Page 24: NSCI 314 LIFE IN THE COSMOS 3 – STARS AND THEIR EVOLUTION (CONTINUED) AND BASIC PROPERTIES OF LIFE Dr. Karen Kolehmainen Department of Physics CSUSB COURSE

REQUIREMENTS FOR LIFE MATTER:

PRODUCED IN BIG BANG (H & He) AND STARS (HEAVIER ELEMENTS)

ARE CERTAIN ELEMENTS NEEDED? STABLE ENERGY SOURCE:

LOW MASS MAIN SEQUENCE STARS (OR SOMETHING ELSE?)

PROTECTED ENVIRONMENT:PLANETARY OR LUNAR SURFACES

PLANETARY OR LUNAR INTERIORS

THICK PLANETARY OR LUNAR ATMOSPHERES CHEMICAL SOLVENT (LIQUID): WATER (OR SOMETHING ELSE?)

APPROPRIATE TEMPERATURE RANGE: NEEDED TO KEEP THE SOLVENT LIQUID (APPROXIMATELY 0 TO

100o C IF WATER IS THE LIQUID SOLVENT)

IF IT’S TOO HOT, COMPLEX STRUCTURES ARE BROKEN APART

IF IT’S TOO COLD, INTERACTIONS ARE TOO SLOW

Page 25: NSCI 314 LIFE IN THE COSMOS 3 – STARS AND THEIR EVOLUTION (CONTINUED) AND BASIC PROPERTIES OF LIFE Dr. Karen Kolehmainen Department of Physics CSUSB COURSE

Sun Earth Earth’s Crust

Hydrogen

Helium

Oxygen

Carbon

Neon

Nitrogen

Magnesium

Silicon

Iron

Sulfur

Argon

Aluminum

Calcium

Sodium

Nickel

Chromium

Phosphorus

90.99%

8.87

0.078

0.033

0.011

0.010

0.004

0.003

0.003

0.002

0.0003

0.0003

0.0002

0.0002

0.0002

0.00003

0.00003

Oxygen

Iron

Silicon

Magnesium

Sulfur

Nickel

Aluminum

Calcium

Sodium

Chromium

Phosphorus

50%

17

14

14

1.6

1.1

1.1

0.74

0.66

0.13

0.08

Oxygen

Silicon

Aluminum

Iron

Calcium

Sodium

Potassium

Magnesium

Titanium

Hydrogen

Phosphorus

Manganese

Fluorine

Strontium

Sulfur

47%

28

8.1

5.0

3.6

2.8

2.6

2.1

0.44

0.14

0.10

0.10

0.063

0.038

0.026

Page 26: NSCI 314 LIFE IN THE COSMOS 3 – STARS AND THEIR EVOLUTION (CONTINUED) AND BASIC PROPERTIES OF LIFE Dr. Karen Kolehmainen Department of Physics CSUSB COURSE

Earth’s Atmosphere Bacteria Human Beings

Nitrogen

Oxygen

Argon

Carbon**

Neon

Helium

78%

21

0.93

0.03

0.0018

0.00052

Hydrogen

Oxygen

Carbon

Nitrogen

Phosphorus

Sulfur

63%

29

6.4

1.4

0.12

0.06

Hydrogen

Oxygen

Carbon

Nitrogen

Calcium

Phosphorus

Sulfur

61%

26

10.5

2.4

0.23

0.13

0.13

Page 27: NSCI 314 LIFE IN THE COSMOS 3 – STARS AND THEIR EVOLUTION (CONTINUED) AND BASIC PROPERTIES OF LIFE Dr. Karen Kolehmainen Department of Physics CSUSB COURSE

BOTTOM LINE:

THE ELEMENTS THAT MAKE UP TERRESTRIAL LIVING ORGANISMS ARE VERY COMMON IN STARS AND IN THE INTERSTELLAR MATERIAL FROM WHICH STARS AND PLANETS ARE FORMED.

IN LIVING THINGS, THE ATOMS OF THESE ELEMENTS ARE ORGANIZED IN ORGANIC MOLECULES, MANY OF WHICH ARE LARGE AND COMPLEX.

Page 28: NSCI 314 LIFE IN THE COSMOS 3 – STARS AND THEIR EVOLUTION (CONTINUED) AND BASIC PROPERTIES OF LIFE Dr. Karen Kolehmainen Department of Physics CSUSB COURSE

ORGANIC MOLECULESMOLECULE: A COMBINATION OF TWO OR MORE ATOMSEXAMPLES: H2O CO2 CH4 NH3 H2 N2 O2 C2H5O2N

ORGANIC MOLECULE: A MOLECULE COMPOSED OF CARBON AND HYDROGEN ATOMS (AND OFTEN OTHER ELEMENTS ALSO)

EXAMPLES: CH4 C2H5O2N

MONOMER: A SIMPLE ORGANIC MOLECULE SUCH AS AN AMINO ACID, SIMPLE SUGAR, FATTY ACID, OR GENETIC BASE

POLYMER: A LARGE ORGANIC MOLECULE COMPOSED OF A CHAIN OF REPEATING MONOMERS

Page 29: NSCI 314 LIFE IN THE COSMOS 3 – STARS AND THEIR EVOLUTION (CONTINUED) AND BASIC PROPERTIES OF LIFE Dr. Karen Kolehmainen Department of Physics CSUSB COURSE

EXAMPLES OF POLYMERSCARBOHYDRATES: STARCHES, CELLULOSE, SUCROSE.

MONOMERS: SIMPLE SUGARS, GLUCOSE

LIPIDS: FATS, CHOLESTEROL, HORMONES, CELLULAR MEMBRANES.

MONOMERS: FATTY ACIDS

NUCLEIC ACIDS: DEOXYRIBONUCLEIC ACID (DNA) & RIBONUCLEIC ACID (RNA).

MONOMERS: GENETIC BASES

PROTEINS: STRUCTURAL PROTEINS FOR BONE, ORGANS, TISSUE, AND MEMBRANES; ENZYMES, CHEMICAL SENSORS AND TRANSPORTERS.

MONOMERS: AMINO ACIDS

NEXT TIME: LET’S EXAMINE NUCLEIC ACIDS AND PROTEINS IN MORE DETAIL.