physics_lecture_note_energy_flow_human.ppt

The Flow of Energy
Where it comes from; where it goes

Spring 2006
UCSD: Physics 8; 2006
2
Energy as a tool in physics
• Energy is a very abstract notion, but it is a very useful
and quantifiable notion
• We use the conservation of energy to predict
behavior
– by setting E = mgh + ½mv2 = constant we can elucidate the
value of the velocity at any height:
v2 = 2g(height fallen from rest)
– We rely on the fact that energy is not created out of nowhere
• Where did the energy we see around us come from?
– most of what we use derives from the sun
– some derives from other, exploded stars (nuclear fission)
– ultimately, all of it was donated in the Big Bang
• but surprisingly, the net energy of the universe can be (and
looks to be) zero!

Spring 2006
3
Energy is Conserved
• Conservation of Energy is different from Energy
Conservation, the latter being about using energy
wisely
• Conservation of Energy means energy is neither
created nor destroyed. The total amount of energy in
the Universe is constant!!
• Don’t we create energy at a power plant?
– No, we simply transform energy at our power plants
• Doesn’t the sun create energy?
– Nope—it exchanges mass for energy

Spring 2006
4
height reference
h
Energy Exchange
• Though the total energy of a system is constant, the
form of the energy can change
• A simple example is that of a pendulum, in which a
continual exchange goes on between kinetic and
potential energy
pivot
K.E. = 0; P. E. = mgh K.E. = 0; P. E. = mgh
P.E. = 0; K.E. = mgh

Spring 2006
5
Perpetual Motion
• Why won’t the pendulum swing forever?
• It’s impossible to design a system free of energy
paths
• The pendulum slows down by several mechanisms
– Friction at the contact point: requires force to oppose; force
acts through distance  work is done
– Air resistance: must push through air with a force (through a
distance)  work is done
– Gets some air swirling: puts kinetic energy into air (not really
fair to separate these last two)
• Perpetual motion means no loss of energy
– solar system orbits come very close

Spring 2006
6
Some Energy Chains:
• A toilet bowl with some gravitational potential energy
is dropped
• potential energy turns into kinetic energy
• kinetic energy of the toilet bowl goes into:
– ripping the toilet bowl apart (chemical: breaking bonds)
– sending the pieces flying (kinetic)
– into sound
– into heating the ground and pieces through friction as the
pieces slide to a stop
• In the end, the local environment is slightly warmer

Spring 2006
7
How Much Warmer?
• A 20 kg toilet bowl held 1 meter off the ground has 200 J of
gravitetional potential energy
– mgh = (20 kg)(10 m/s2)(1 m) = 200 kg·m2/s2 = 200 J
• A typical heat capacity is 1000 J/kg/C (a property of the material)
• So 200 J can heat 0.2 kg of material by 1C or 1 kg by 0.2C or 20
kg by 0.01C
– heat capacity follows intuitive logic:
• to get same T, need more energy or less mass
• given fixed energy input, get smaller T for larger mass
• for a given mass, get larger T for more energy input
• So how much mass is effectively involved?
– initially not much (just contact surfaces): so hot at first
– but heat diffuses into surrounding bulk: cools down
– so answer is ill-defined: depends on when
• But on the whole, the temperature rise is hardly noticeable

Spring 2006
8
Gasoline Example
• Put gas in your car
• Combust gas, turning chemical energy into kinetic energy of the
explosion (motion of gas particles)
• Transfer kinetic energy of gas to piston to crankshaft to drive
shaft to wheel to car as a whole
• That which doesn’t go into kinetic energy of the car goes into
heating the engine block (and radiator water and surrounding
air), and friction of transmission system (heat)
• Much of energy goes into stirring the air (ends up as heat)
• Apply the brakes and convert kinetic energy into heat
• It all ends up as waste heat, ultimately

Spring 2006
9
Bouncing Ball
– Superball has gravitational potential energy
– Drop the ball and this becomes kinetic
energy
– Ball hits ground and compresses (force times
distance), storing energy in the spring
– Ball releases this mechanically stored energy
and it goes back into kinetic form (bounces
up)
– Inefficiencies in “spring” end up heating the
ball and the floor, and stirring the air a bit
– In the end, all is heat

Spring 2006
10
Why don’t we get hotter and hotter
• If all these processes end up as heat, why aren’t we
continually getting hotter?
• If earth retained all its heat, we would get hotter
• All of earth’s heat is radiated away as infrared light
– hotter things radiate more heat
• If we dump more power, the temperature goes up,
the radiated power increases dramatically
– comes to equilibrium: power dumped = power radiated
– stable against perturbation: T tracks power budget

Spring 2006
11
Another Piece of the Energy Zoo: Light
• The power given off of a surface in the form of light is
proportional to the fourth power of that surface’s temperature!
P = AT4 in Watts
– the constant, , is numerically 5.6710-8 W/ºK4/m2
– easy to remember constant: 5678
– A is surface area of hot thing, in square meters
– temperature must be in Kelvin:
• ºK = ºC + 273
• ºC = (5/9)(ºF –32)
• Example: radiation from your body:
(1 m2)(5.67 10-8) (310)4 = 523 Watts
(if naked in the cold of space: don’t let this happen to you!)

Spring 2006
12
Radiant Energy, continued
• Example: The sun is 5800ºK on its surface, so:
P/A = T4 = (5.6710-8)(5800)4 = 6.4107 W/m2
Summing over entire surface area of sun gives
3.91026 W
• Compare to total capacity of human energy
“production” on earth: 3.31012 W
– Single power plant is typically 0.5–1.0 GW (109 W)
• In earthly situations, radiated power out is partially
balanced by radiated power in from other sources
– Not 523 W/m2 in 70ºF room, more like 100 W/m2
• goes like Th
4 – Tc
4

Spring 2006
13
Rough numbers
• How much power does the earth radiate?
• P/A = T4 for T = 288ºK = 15ºC is 390 W/m2
• Summed over entire surface area (4R2, where R =
6,378,000 meters) is 2.01017 W
– For reference, global “production” is 31012 W
• Solar radiation incident on earth is 1.81017 W
– just solar luminosity of 3.91026 W divided by geometrical
fraction that points at earth
• Amazing coincidence of numbers! (or is it…)

Spring 2006
14
No Energy for Free
• No matter what, you can’t create energy out of
nothing: it has to come from somewhere
• We can transform energy from one form to another;
we can store energy, we can utilize energy being
conveyed from natural sources
• The net energy of the entire Universe is constant
• The best we can do is scrape up some useful crumbs

Spring 2006
15
Energy and Calories
• A calorie is a unit of energy
(1 cal is the amount of
energy required to raise the
temperature of 1 cc of water
1˚C.)
– 1 cal = 4.184 J
• Food Calories are measured
in kcal (1 Cal = 1000 cal)
– 1 Cal = 4184 J
• 250 Calories is enough
energy to raise 250 liters
(about 66 gallons) of water
1˚C.

Spring 2006
16
Human Energy Requirements
• 1,500 Calories per day just to be a couch-potato
– 6,280,000 J
• Average human power consumption is then:
– 6.28 MJ / 86,400 seconds  75 W
– We’re like light bulbs, constantly putting out heat
• Need more like 2,000 Cal for active lifestyle
– 100 W of power

Spring 2006
17
Energy from Food
• Energy from fat, carbohydrates, protein
– 9 Calories per gram for fat
– 7 Calories per gram for alcohol
– 4 Calories per gram for carbohydrate
• Fiber part doesn’t count
– 4 Calories per gram for protein
• Calculate 63 fat, 84 CH, 40 protein Cals
– total is 187 Calories (180 is in the
ballpark)
• 1 Calorie (kilo-calorie) is 4,187 J
– 180 Cal = 753 kJ
– set equal to mgh climb 1100 m
vertically, assuming perfect efficiency

Spring 2006
18
Not So Fast…
• Human body isn’t 100% efficient: more like 25%
– To put out 100 J of mechanical work, must eat 400 J
– 180 Calorie candy bar only gets us 275 m, not 1100 m
• Maximum sustained power output (rowing, cycling) is about 150-
200 W (for 70 kg person)
– Consuming 600-800 W total, mostly as wasted heat
– For 30 minutes  800 J/s 1800 s = 1.44 MJ = 343 Cal
• Can burst 700 W to 1000 W for < 30 sec
– put out a full horsepower momentarily!

Spring 2006
19
Most impressive display of human power
• The Gossamer Albatross crossed the English Channel in
1979, powered by Bryan Allen
– Flight took 49 minutes, wiped Bryan out!
– Sustained power out ~250 W

Spring 2006
20
Human Energy Requirements Summarized
• We need chemical energy from food to run
– Ultimate source is sun, long chain of events to twinkies
– Constantly burn energy at rate of 75-100W
– We spend energy at about 25% efficiency
– Maximum sustained power is 150-200 W
• actually burn 4 times this due to inefficiencies

Spring 2006
21
Exercise
• Ways to transform chemical
energy of food → work and
heat
• When we exercise, we do a
little bit of both, but mostly
we transform energy from
food into heat
– 3:1 ratio, given 25%
efficiency

Spring 2006
22
Air Resistance
• We’re always “neglecting air resistance” in physics
– Can be difficult to deal with
• Affects projectile motion
– Friction force opposes velocity through medium
– Imposes horizontal force, additional vertical forces
– Terminal velocity for falling objects
• Dominant energy drain on cars, bicyclists, planes

Spring 2006
23
Drag Force Quantified
• With a cross sectional area, A (in m2), coefficient of
drag of 1.0 (most objects), sea-level density of air,
and velocity, v (m/s), the drag force is:
Fdrag = ½ cD··A·v2 Newtons
– cD is drag coefficient: ~1.0 for most things, 0.35 for car
–  is density of medium: 1.3 kg/m3 for air, 1000 kg/m3 water
– typical object in air is then Fdrag  0.65·A·v2
• Example: Bicycling at 10 m/s (22 m.p.h.), with
projected area of 0.5 m2 exerts 32.5 Newtons
– requires F·v of power  325 Watts to maintain
speed

Spring 2006
24
“Free” Fall
• Terminal velocity reached when Fdrag = Fgrav (= mg)
• For 75 kg person subtending 0.5 m2,
vterm  50 m/s, or 110 m.p.h.
which is reached in about 5 seconds, over 125 m of fall
• actually takes slightly longer, because acceleration
is reduced from the nominal 10 m/s2 as you begin to
encounter drag
• Free fall only lasts a few seconds, even for skydivers

Spring 2006
25
Announcements/Assignments
• Next up:
– a simple model for molecules/lattices
– electrons, charge, current, electric fields
• Assignments:
– read chapter 7, pp. 212–214, 225–228
– read chapter 3, 83–87; chapter 9 265–269, 278–279
– HW1: 1.E.4, 1.E.7, 1.E.8, 1.E.20, 1.E.25, 1.E.34, 1.P.1,
1.P.8, 1.P.10 (in Newtons), 1.P.14, 1.P.16, 1.P.18, 1.P.22,
2.E.28, 2.P.10, 2.P.11: due 4/13
– First Q/O due Friday, 4/14 by 6PM via WebCT

physics_lecture_note_energy_flow_human.ppt

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