Ast Unit 1

Front 1

aphelion

Back 1

farthest point away in orbit

Front 2

Perihelion

Back 2

nearest point in orbit

Front 3

zodiac

Back 3

18 degree wide belt centered on the ecliptic

Front 4

ecliptic

Back 4

sun path, 23 degree, changes 1 degree per year

Front 5

plannet

Back 5

wanderer in the skycircumpolar zone

Front 6

diffuse nebula

Back 6

cloud of gas illuminated by stars

Front 7

double star

Back 7

stars close enough in sky to appear as one

Front 8

magnitude

Back 8

how bright a star appears to us

Front 9

open cluster

Back 9

10s to 100s of new stars in a group

Front 10

zinith

Back 10

point directly above head

Front 11

AU

Back 11

distance from earth to son, 93 million miles

Front 12

kepler first law

Back 12

planets orbit are elipses with son as foci

Front 13

kepler 2nd law

Back 13

the motion of the plan sweeps out and equal area in an equal time

Front 14

eccentricity calculation

Back 14

e= distance between foci/ length of major axis

 

more e means more squished,

Front 15

kepler third law

Back 15

the square of the period of revolution is directly proportional to the cubes of the semi-major axis when the distance between is in AU and the period is in years

Front 16

eraosthenes

Back 16

200 BC, measured circumference of the earth, no sure of how close because of the uncertancy in his method

Front 17

aristarchus

Back 17

260 bc, aristarchus of Samos suggessted that the earth was moving around the sun, but his ideas were rejected due to observers not being able to observe any stellar paralax

Front 18

hipparchus

Back 18

150 BC, defined and measured positions , direction and magnitude of 850 stars

 

recognized precession of earths axis

Front 19

Ptolemy

Back 19

140 bc, constucted a geometrical representtion of the solar system using epicycles that predicted the position of the planets for any desired time and date.

explained mars retrograde motion

Front 20

Nicolaus Copernicus

Back 20

1500 AD, recognised father of modern astronomy

sun was at center, heliocentric vs geocentric

Front 21

Galileo

Back 21

1600 AD, beggining of modern science, built telescope

discovered sun spot

observed phases of venus

described details of lunar surface

discoverd 4 moons of jupiter (not geocentric)

milky way

Front 22

Newton's 1st law

Back 22

a body in motion will stay in motion unless compelled to change

 

rest is equivalent to constant motion

Front 23

Newton's second law

Back 23

defines what a force is =>F=ma

or force equals mass times acceleration

Front 24

Newton's third law

Back 24

for every action there is an equal and opisite reaction

Front 25

Angular Momentum

Back 25

momentum thought of mass in motion that is always convered

angular momentum is a measure of the spinning and revolving object and is convered as well

Front 26

density

Back 26

mass not wwieght,

mass/volume

Front 27

Law of Universal Gravity

Back 27

every piece of mass attracts every other piece of matter. The magnitude of the attraction depends upon the individual masses and the distances squared between their centers

Front 28

Moon Phase

Back 28

28 days

takes the same time to rotate as orbit so we only see one side

 

new, cresent, 1st quarter, gibbous, full

Front 29

waxing

Back 29

increasing the visable surface of the moon, the right side of the moon will be lit

Front 30

waning

Back 30

decreasing the visible surface of the moon. the left side will be lit

Front 31

lunar eclipse

Back 31

moon blocked by earths shadow

Front 32

solar

Back 32

sun blocked by moon

Front 33

earthts tilt

Back 33

23 degree, dosnt change over time

Front 34

equinox

Back 34

spring-vernal equinox

fall- autumnal equinox

Front 35

solstice

Back 35

summer

winter solstice

Front 36

equinox

Back 36

sun corsses the celestial equater

Front 37

solstice

Back 37

sun is manimum point below the celestial equatior

Front 38

wave

Back 38

movemnt of energy

Front 39

mechanical wave

Back 39

requires medium to travel on

Front 40

electromagnetic wave

Back 40

dosn't need medium to travel on

Front 41

transverse wave

Back 41

moves perpendicular direction of motion

Front 42

longitudinal wave

Back 42

moves parallel to the direction of motion

Front 43

torsional wave

Back 43

twisting wave

Front 44

wavelength frequency and period

Back 44

(1/p=1&1/f=p)

Front 45

amplitude

Back 45

energy

Front 46

reflection

Back 46

bpuncing back of waves from hitting a barrier

Front 47

refraction

Back 47

benfing of waves due to changes in medium

Front 48

diffraction

Back 48

bending of waves around a barrier

Front 49

interference

Back 49

sum of energies when waves cross

Front 50

doppler effect

Back 50

apparent change in frequencies of waves due to motion of source, observer or both

Front 51

disperion

Back 51

spreading out of waves

Front 52

polarization

Back 52

alignment of waves oscillation

Front 53

light

Back 53

the form of radient energy that stimulates the organs of sight having for normal human vision wavelengths ranging from about 3900 to 7700 angsroms and traveling at a speed of about 186300 miles per second

Front 54

electromagnetic spectrum

Back 54

the continuum of light that travels at the speed of light in a vacuum

Front 55

spped of light

Back 55

3x10 to the power of eight meters per second

or

186000 miles per second

Front 56

light spectra

Back 56

continuous

emission (bright line)

absoption (dark line)

 

Front 57

blackbody radiation

Back 57

a black body is a theoretical abject that absorbs 100% of the radiation that it hits. therefore it reflects no raidiation and appears perfectly black

Front 58

ass temperature increases

Back 58

the peak wavelength emited by the black body decreases

Front 59

as temperature increases

Back 59

the total energy emitted increases because the total area under the curve increases

Front 60

the light gathering ability of a telescope is determined by

Back 60

area the device is collecting

Front 61

aperture of an optical telescope 

Back 61

diameter of the lens or mirror in front of the scope

Front 62

largest type of telescope

Back 62

reflecting because its supported underneath

Front 63

resolution

Back 63

fineness pf the detail present in the image

 

smallest degree of separation that can be seen between two light sources at some distance

Front 64

adaptive optics

Back 64

improves the resolution of a telescope as the light passes through the earth's atmosphere

Front 65

magnification

Back 65

focal lengthn of the objective divided by the focal length of the eyepiece

Front 66

obective

Back 66

lens/mirror in front and the eyepiece is the lens/mirror closest to the eye device

Front 67

converging

Back 67

concave mirror and convex lens

Front 68

diverging

Back 68

concave lens and convex mirror

Front 69

hubble

Back 69

orbiting telescope

Front 70

parts of eye

Back 70

cornea 

iris

pupil

lens

retina

optical nerve