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142 Cards in this Set
- Front
- Back
- 3rd side (hint)
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ISOTOPES
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ATOMS THAT HAVE THE SAME # OF PROTONS BUT DIFFERENT # OF NEUTRONS
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IONS
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AN ATOM THAT HAS LOST OR GAINED AN ELECTRON
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MOLECULES
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TWO OR MORE ATOMS BANDED TOGETHER
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ELECTRON ORBITS
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-electrons are bound by the attraction between (-) and (+) charge of the nucleus
-electrons can be kicked to higher orbit when absorbs photon w/exactly |
the right energy
-excited state |
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ENERGY LEVELS
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SIZE OF ELECTRONS ORBIT DEPENDS ON ENERGY
ORBITS=ENERGY LEVEL GROUND STATE: SMALLEST AND TIGHTEST |
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HYDROGEN ATOM
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MOST ABUNDANT
ONE PROTON (+1 ELECTRON) |
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HELIUM ATOM
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2 PROTONS (2 NEUTRONS + 2 ELECTRONS)
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STARLIGHT TELLS US
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-TOTAL ENERGY OUTPUT
-SURFACE TEMP -RADIUS -CHEMICAL COMPOSITION -RADIUS |
-VELOCITY RELATIVE TO EARTH
-ROTATION PERIOD |
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TEMPERATURE SCALES
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BLUE: HOTTER
RED: RED COOLER |
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BLACK BODY RADIATION
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1. the hotter the object the more luminous it is
2. the peak of the blackbody spectrum shifts towards shorter wavelengths when temp increases |
collision among particles accelerate electrons and cause emission
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WEINS LAW
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the hotter object emits more blue light than red and looks blue
the cooler object emits more red light and look red |
a hotter object will have a shorter wavelength of maximum emitted intensity
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KIRCHOFFS 3 LAWS
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3 KINDS OF SPECTRUM
1CONTINUOUS 2EMISSION 3ABSORPTION |
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CONTINUOUS SPECTRUM
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A SOLID LIQUID OR GAS EXCITED TO EMIT LIGHT WILL RADIATE AT ALL WAVELENGTHS
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EMISSION SPECTRUM
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IF LIGHT COMPRISING A CONTINUOUS SPECTRUM PASSES THRU A COOL, LOW DENSITY GAS
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ABSORPTION SPECTRUM
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A LOW DENSITY GAS EXCITED TO EMIT LIGHT WILL DO SO AT SPECIFIC WAVELENGTHS
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DOPPLER EFFECT
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THE LIGHT OF A MOVING SOURCE IS BLUE/RED SHIFTER
BLUE: HIGHER FREQUENCY RED: LOWER FREQUENCY |
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PHOTOSPHERE
7 |
COOLEST LAYER OF STAR
APARENT SURFACE LAYER OF SUN ENERGY TRANSPORT THRU CONVECTION |
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CHROMOSPHERE
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MIDDLE TEMP
REGION ABOVE PHOTOSPHERE HOTTER THAN PHOTOSPHERE KNOW EXIST VIA FILTERGRAMS |
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CORONA
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HOTTEST
FAINT OUTER ATMOSPHERE COMPOSED OF LOW HIGH TEMP GAS KNOW EXIST VIA ECCLIPSE |
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SUNSPOTS
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COOLER REGIONS OF PHOTOSPHERE
11yr cycle poles switch 22yr cycle poles switch and go back |
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GRANULATION
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THE VISIBLE CONSEQUENCE OF CONVECTION
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SUPER GRANULES
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CAUSED BY CONVECTION CURRENTS DEEPER IN SUN
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CONVECTION
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WAY OF TRANSPORTING ENERGY
OCCURS WHEN HOT MATERIAL RISES AND COLD MATERIAL SINKS EX: BOILING WATER |
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FILTERGRAM
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WAY WE DETECT CHROMOSPHERE
LOOKING AT WAVELENGTH WITH STRONG ABSORPTION LINES GIVES INFO ABOUT CHROMOSPHERE |
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SPICULES
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FILAMENTS OF COOLER GAS FROM PHOTOSPHERE RISING UP INTO CHROMSPHERE
LAST 5-15 MINS |
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CORNOGRAPHS
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ARTIFICIAL SOLAR ECLIPSE TO STUDY CORONA
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MAGNETIC CARPET
7 |
MAGNETIC FIELDS THRU PHOTOSPHERE
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HELIOSEISMOLOGY
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ANALYSIS OF VIBRATION PATTERNS VISIBLE ON THE SOLAR SURFACE
-ONLY WAY TO INVESTIGATE SOLAR INTERIOR |
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SOLAR WIND
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SUN ENERGY BEING RELEASED
STIRS UP DUST AND GAS PARTICLES |
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MAUNDER BUTTERFLY DIAGRAM
7 |
22 yr cycle: starts away from equator
gets closer to equator on equator : 11yr jumps to south |
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ZEEMAN EFFECT
7 |
A WAY TO MEASURE MAGNETIC FIELDS ON THE SUN
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MAUNDER MINIMUM
7 |
VERY FEW SUN SPOTS
COINCIDES WITH LITTLE ICE AGE UNUSUAL COLD WEATHER |
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ACTIVE REGIONS
7 |
CONTAINS POWERFUL MAGNETIC FIELDS
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DYNAMIC EFFECT
7 |
PRODUCES SUN MAGNETIC FEILD
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DIFFERENTIAL ROTATION
7 |
DIFFERENT PARTS ROTATE DIFFERENT TIMES
equatorial region of photosphere rotates faster than regions of higher latitudes |
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BABCOCK MODEL
7 |
way to describe magnetic feild cycle
can tell where more active regions are where sun spots should appear |
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POLARITY OF SUN
7 |
NORTH AND SOUTH POLES AND EVERY 11YRS SWITCH POLES
SEE PAGE 129 |
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SOLAR CONSTANT
7 |
A MEASURE OF THE ENERGY OUTPUT OF THE SUN
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WEAK FORCE
7 |
INVOLVED IN RADIOACTIVE DECAY
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STRONG FORCE
7 |
BINDS TOGETHER PROTONS AND NEUTRONS
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FOUR WAYS MATTER EFFECTS OTHER MATTER
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1. GRAVITY
2. ELECTROMAGNETIC 3. STRONG 4. WEAK |
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NUCLEAR FISSION
7 |
STARS DONT USE
He-->H reactions that split uranium nuclei into less massive fragments |
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NUCLEAR FUSION
7 |
STARS USE
H-->HE |
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PROMINENCES
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CIRCULAR EXPLOSION
IONIZED GAS TRAPPED IN MAGNETIC ARCH RISING UP THRU PHOTO AND CHROMO INTO LOWER CORONA |
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FILAMENTS
7 |
SOLAR PROMINENCE SEEN FROM ABOVE
SILHOUETTED AGAINST BRIGHT PHOTSPHERE |
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RECONNECTION EVENT
7 |
PRODUCE SOLAR FLARES
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AURORAS
7 |
SOLAR WIND CAUSES AURAS
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CORONAL MASS EJECTION (CME)
7 |
EXPLOSION FROM CORONA
WE CAN TELL WHEN ONE HAPPENS:MESSES UP EARTH MAGNETIC FEILD |
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CORONAL HOLES
7 |
WHERE MAGNETIC FEILD DOES NOT LOOP BACK TO SUN
PRODUCE SOLAR WINDS |
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PROTON PROTON CHAIN
7 |
3 NUCLEAR REACTIONS TO BUILD HELIUM NUCLEUS
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POSITRON
7 |
A POSITIVELY CHARGED VERSION OF AN ELECTRON
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NEUTRINOS
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A SUBATOMIC PARTICLE HAVING AN EXTREMELY LOW MASS AND A SPEED NEARLY EQUAL TO THE SPEED OF LIGHT
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DEUTRIUM
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HEAVY HYDROGEN
+ ADDED NEUTRON TO HYDROGEN NUCLEUS NEUTRAL HYDROGEN JUST 1 PROTON AND 1 ELECTRON |
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COULOMB BARRIER
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NUCLEAR RESISTANCE TO COLLISIONS
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RADIATIVE ZONE
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INNER PARTS OF SUN
CORE-RADIATIVE ZONE-CONVECTIVE ZONE |
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CONVECTION ZONE
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CLOSER TO SURFACE WHERE HOT GAS RISE AND COOL GAS SINK
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STELLAR PARALLAX
8 |
DISTANCE STAR BY MEASURING APPARENT SHIFT AGAINST BACKGROUND STAR
VERY SMALL SHIFT D(PC)= 1/P |
1PC=2.06X10
1P=3.26LY p=parallax d=distance pc=parsec |
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PARSEC
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SPECIAL UNIT OF DISTANCE TO MEASURE DISTANCE TO STARS
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FLUX
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AMOUNT OF ENERGY EMITTED PER SEC PER SURFACE AREA
energy/sec x areas j/sm |
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INTRINSIC BRIGHTNESS
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TOTAL AMOUNT OF LIGHT STAR EMITS
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ABSOLUTE VISUAL MAGNITUDE
Mv 8 |
Mv
MEASURING THE AMOUNT OF LIGHT AT DISTANCE OF 10 PC **only used in equation (10pc) when finding the Mv** |
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MAGNITUDE DISTANCE FORMULA
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mv-Mv=5log(d)-5
mv=apparent visual magnitude Mv=absolute visual magnitude d=distance IN PARSECS |
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APARENT VISUAL MAGNITUDE
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mv
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LUMINOSITY
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ENERGY START TO EMIT PER SEC
ENERGY/SECONDS J/S |
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BALMER THERMOMETER
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used to determine stars temp
***balmer lines*** strongest: med temp (a-o stars) weakest: hot(H ionizes) cold (ground state) |
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SPECTAL CLASSES/TYPES
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HOTTEST: Oh Be A Fine Girl Kiss Me Lovingly Tonight :COLDEST
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SPECTRAL SEQUENCE
8 |
SUN IS A G2 STAR
TEMP OF STAR WITHIN 5% ACCURACY |
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L DWARFS
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VISIBLE INFRARED
EVEN COLDER THAN M STAR |
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LUMINIOSITY/ RADIUS/ TEMP
RELATIONSHIP 8 |
L=
INCREASE LUMINOSITY BY TEMP AND SURFACE AREA |
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HR DIAGRAM
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ENABLES ASTRONOMERS TO SORT CLASSIFY STARS BASED ON TEMP AND LUMINOSITY
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MAIN SEQUENCE
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STARS SPEND 90% ON MAIN SEQUENCE
80% all stars on main sequence must be fusing H-->He once stop fusing this star moves off main sequence |
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GIANT
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10-100 TIMES LARGER THAN SUN (MORE LUMINOUS)
COLDER THAN SUN |
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SUPERGIANT
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EITHER REALLY BIGGER OR REALLY HOTTER THAN GIANTS
1000 TIMES LARGER THAN SUN |
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WHITE DWARF
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SMALLER THAN RED DWARFS BUT HOTTER
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LUMINOSITY CLASSES
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Ia. luminous supergiant
Ib. supergiant II. luminous giant III. giant IV. subgiant V. main sequence |
WAY TO CALCULATE DISTANCE OF STARS WHEN THEY ARE TOO FAR FOR PARALLAX
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LINES OF CONSTANT RADII
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RELATES THE SIZE TO OUR SUN
PG 155 |
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SPECTROSCOPIC PARALLAX
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method determine distance to star by:
1. spectral type 2. luminosity class 3. apparent magnitude (mv) |
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BINARY STARS
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TWO STAR SYSTEM THAT ORBITS COMMON CENTER OF MASS
3 TYPES: VISUAL. SPECTROSCOPIC. ECCLIPSING |
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KEPLERS THIRD LAW TO BUNARY STARS
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Ma+Mb=a / p
Ma+Mb: solar masses p: orbit period in yrs a: semimajor axis in AU |
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VISUAL BINARIES
8 |
SEE TWO STARS THRU TELESCOPE
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SPECTROSCOPIC BINARIES
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SEE STARS THRU SPECTRAL LINES
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ECCLIPSING BINARIES
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ONE STAR PASSES IN FRONT O THE OTHER
DETECTED BY LIGHT CURVE |
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MASS LUMINOSITY RELATION
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MORE MASS=MORE LUMINOSITY
L=M |
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SURVEY OF STARS
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MOST STARS FAINT
ALOT OF RED DWARFS MOST STARS MAIN SEQ STARS |
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INTERSTELLAR MEDIUM (ISM)
9 |
ISM
hard to detect in visible detectable in radio and infrared dense regions ISM where stars made |
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INTERSTELLAR EXTINCTION
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MAKES STARS APPEAR DIMMER
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INTERSTELLAR ABSORPTION LINES
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absorption lines due to the ISM
1. type of absorption line 2. width of line *stars naturally produce absorption spectrum* |
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MOLECULAR CLOUDS
9 |
COLDEST DENSEST REGIONS IN ISM
MADE OF MOLECULES |
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INTERSTELLAR EMISSION LINES
9 |
EMISSION LINES DUE TO ISM
WAY TO STUDY ISM TELL WHAT GAS AND DUST ARE MADE OF |
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INTERSTELLAR ABSORPTION LINES
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ABSORPTION LINES DUE TO ISM
WAY TO STUDY ISM TELL WHAT GAS AND DUST ARE MADE OF |
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INTERSTELLAR DUST
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1% OF ISM 99% GAS
REALLY SMALL <1000NM OR 1 MICRON IN DIAMETER |
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INTERSTELLAR REDDING
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LIGHT PASSING THRU ISM MAKES LIGHT LOOK REDDER
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21CM RADIO LINE
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TO MAP THE LOCATION OF COLD LOW DENSITY GAS IN GALAXY
photon creates 21cm wavelength measured in radiowaves |
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NEBULA
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DENSE CLOUDS OF DUST AND GAS: EASILY SEEN VISIBLE WAVELENGTH: APPEAR HAZY
3TYPES: |
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STAR FORMATION
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-shock triggered by supernova passes thru molecular cloud -causes cloud to compress-compressing region press down and becomes dense-dense region creates star
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-continues process until all gas/dust is used/gone
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EMISSION NEBULAE
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PINK: PRODUCE EMISSION SPECTRA
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REFLECTION NEBULAE
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BLUE: REFLECT LIGHT
ABSORPTION SPECTRA |
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DARK NEBULAE
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BLACK: LIGHT GETS FILTERED/ ABSORBED
ABSORPTION SPECTRA |
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HII REGIONS
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HII: SINGLY IONIZED (IONIZED H)
HI: NEUTRAL HII: AREAS WHERE YOU HAVE IONIZED H: HOT >25,000 B1 or hotter stars: seen emission nebulae |
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FREE FALL COLLAPSE
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STARS OWN GRAVITY CAUSES COLLAPSION
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COCOONS
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CLOUDS OF GAS/DUST AROUND A PROTOSTAR
MAKES HARD TO SEE STAR |
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PROTOSTAR
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INCOMPLETE FORMING STAR
IS PROTOSTAR UNTIL BEGIN FUSING HYDROGEN IN CORE ONLY DETECT INFRARED WAVE STARTS COLD AND SMALL |
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BOK GLOBULES
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WHERE STARS FORM SMALL DARK CLOUDS
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BIRTHLINE
9 |
FIRST TIME WE CAN DETECT PROTOSTAR
TETARY STAGE: STAR SHEDDING COCOOON |
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YOUNG STELLAR OBJECTS
9 |
YSO
STARS THAT ARE NOT ON MAIN SEQUENCE YET NOT FUSING HYDROGEN IN CORE |
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PROTOSTELLAR DISKS
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DISKS AROUND NEWLY FORMED PROTOSTARS
EITHER BLOWN OF OR USED TO HELP FORM PLANETS: not always but required for planet formation |
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ASSOCIATION
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CLUSTER OF STARS NOT HELD TOGETHER BY GRAVITY
WILL SPREAD APART OVER TIME |
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T ASSOCATION
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ASSOCIATION THAT CONTAINS T TAURI STARS
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OB ASSOCIATION
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ASSOCIATION THAT CONTAINS O AND B STARS
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T TAURI STARS
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STARS THAT FLUCTUATE IN BRIGHTNESS
JUST BEGUN SHEDDING COCOON LOW MASS PRE MAIN SEQUENCE |
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HERBIG-HARO OBJECTS
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WHERE JETS PRODUCED BY PROTOSTAR HIT THE ISM
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BIPOLAR FLOW
9 |
PROTOSTAR JETS=BIPOLAR FLOWS
BIPOLAR FLOWS EVIDENCE THAT PROTOSTAR HAS DISK |
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HYDROSTATIC EQUILIBRIUM
9 |
BALANCE BETWEEN PRESSURE OF STAR AND WEIGHT OF STAR
FARTHER IN STAR THE MORE PRESSURE AND WEIGHT |
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ENERGY TRANSPORT
9 |
3 WAYS:
CONDUCTION: STOVE CONVECTION: BOILING WATER RADIATION: SUNBURN |
STAR CORE: VIA CONVECTION
STAR PHOTOSPHERE: VIA RADIATION |
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OPACITY
9 |
COOL GAS: more opaque hard time transfer energy by raditation
HOT GAS: less opaque easier transfer energy via radiation |
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CNO CYCLE
9 |
CARBON NITROGEN OXYGEN
RECYCLED /REUSED IN CYCLE 4 PROTON COMBINED =HELIUM NUCLEUS=HYDROGEN FUSION hotter stars: hoe energy fuses in core |
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PRESSURE TEMPERATURE THERMOSTAT
9 |
MECHANISM WHICH STAR REGULATES HOW RAPIDLY ITS FUSING HYDROGEN
MORE MASSIVE-SHORTER LIFE-BURN FUEL FASTER |
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STELLAR MODELS
9 |
MATHEMATICAL WAY DESCRIBING HOW INSIDE OF STAR WORKS
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STELLAR LUMINOSITY AND LIFETIME OF STAR RELATE
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MORE MASSIVE-MORE LUMINOUS-SHORTER LIFETIME
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LIFE ON MAIN SEQUENCE
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90% life on main sequence
move off done fusing how long on ms depends on size |
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CALCULATING LIFE EXPECTANCIES OF STARS
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T=M
M=MASS T=LIFETIME |
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NOVA
10 |
ERUPTION OF AN OLD STAR
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SUPERNOVA
10 |
VIOLENT EXPLOSION OF AGING STAR
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STAR CLUSTER TURN OFF POINT
10 |
TELL AGE OF CLUSTER
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CHANDRASEKHAR LIMIT
10 |
WHITE DWARF: THE SMALLER THE MORE MASSIVE; LESS LUM
1.4 SOLAR MASS CANNOT GET ANY MORE MASSIVE AS WD |
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ROCHE LOBES/ROCHE SURFACE
10 |
TRANSFER MASS BETWEEN THE BINARY SYSTEM STARS
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LAGRANGE POINTS
10 |
BINARARY SYSTEM
BETWEEN STARS IMPORTANT: POINTS WHERE OBJECT IS GRAVITATIONAL STABLE/BOUND |
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HOW WILL EARTH END:
10 |
SUN WILL TURN INTO GIANT AND WE WILL BURN TO DEATH
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TYPE II SUPERNOVA
10 |
MASSIVE STAR BLOWING UP
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TYPE I SUPERNOVA
10 |
CAUSED BY WHITE DWARF BLOWING UP
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SUPERNOVA REMNANT
10 |
STUFF LEFT OVER AFTER SUPERNOVA
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END STATE OF DYING STARS
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WHITE DWARFS
NEUTRON STARS BLACK HOLES |
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RED DWARFS
WHITE DWARFS |
MOST ABUNDANT
SECOND MOST ABUNDANT |
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PROTON PROTON CHAIN
CNO CYCLE |
BOTH FUSING H-->HE
CNO: HOTTER/MORE MASSIVE STARS PROTONPROTON: COLDER/LESS MASSIVE STARS |
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TWO WAYS TO INCREASE LUM
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SIZE OR TEMP
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PHOTOSPHERE
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CAUSES SUNS ABSORPTION LINES
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CORE OF STAR
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CONTINUOUS SPECTRA
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NUCLEAR FUSION
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HEATS CORONA AND CHROMOSPHERE
NUCLEAR FUSION-RADIATION-CONVECTION |
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HELIUM FLASH
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MOVES OFF MAIN SEQUENCE HELIUM CORE NOT HOT ENOUGH TO FUSE HE
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NOT ALL STAR EXPERIENCE HELIUM FLASH
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1. less massive .4 solar mass never get hot enough to ignite He
2. more massive 3 solar mass ignite He before contracting cores become degenerate |
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RED DWARFS
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LESS MASSIVE
TOTALLY CONVECTIVE |
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NEUTRON STAR FORMATION
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supernova explosion of >8Msun
blown away outer layers central core colapse pressure so high proton electron=form neutron |
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