Astronomy Exam 1
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| Introduced "Objective Reality" | Thales
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| First to picture an infinite universe | Anaximander
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| Originated the 7-day week and the roots of the 24-hour day and 60 minute hour | Summerians
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| Perpetuated the calendar choices of the Sumerians, developed algebra | Babylonians
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| Used a 10-day week. Developed geometry | Egyptians
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| Atomic Theory and the Vacuum | Democritus and Leucipus
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| Separated science and philosophy | The Pythagoreans
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| Suggested the Earth rotated on its axis, and possibly was not the center of the universe | The Pythagoreans
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| One of the Athenian Philosophers | Socretes
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| deepest thinker of the Athenian philosophers. founded the first "University" - Empirical Philosophy | Plato
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| Founded the current scientific disciplines - founded his own university. big contributions in biology. Argued the Earth was a sphere. Argued against a heliocentric theory because of the lack of an observable stellar parallax. Also an Athenian Philosopher | Aristotle
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| A contemporary of Plato and Aristotle. Early developments of Mechanics in physics | Eudoxus
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| First serious proponent of the Heliocentric theory | Aristarchus
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| The greatest observational astronomer in antiquity. Developed the Stellar Magnitude scale. Produced a star catalog. Measured the distances to the sun and moon. discovered the 26000 year precession of the Earth's axis of rotation. Argued against the helioc | Hipparchus
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| Passed down to us much of what we know about the earlier contributions. Set down the principals of celestial navigation and Astrology | Ptolemy
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| Re-introduced the Heliocentric theory. Described the Solar System with the correct Sidereal periods | Copernicus
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| Compiled large volumes of observational data | Tycho
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| Used Tycho's data to discern his 3 laws of planetary motion. | Kepler
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| The father of modern science. Used telescope to discover the 4 brightest moons of Jupiter, the crescent phases of Venus, stars too dim to be seen with the naked eye | Galileo
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| Discovered the Law of Inertia and introduced the scientific method | Galileo
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| The father of modern physics | Newton
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| Three laws of motion: *The law of inertia (An object in motion...) *F = ma *Conservation of Momentum - mv (Action - Reaction) | Newton
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| The Law of Universal Gravitation - F = G m1m2/r^2 | Newton
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| General form of Kepler's 3rd law (M1 + M2)p^2 = a^3 | Newton
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| The reflecting telescope and the spectrum of light | Newton
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| Electric charges (q/r^2) and changing magnetic fields (delta B / delta t) | Electric Field Sources
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| Causes a force in the direction of the field on all charges | Electric Field Effects
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| Moving charges (Right-Hand-Rule) and changing electric fields | Magnetic Field Sources
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| Causes a force on moving charges (qvB) perpendicular to the field and the direction of motion of the charge (Right-Hand-Rule) | Magnetic Field Effects
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| Light is composed of | Electromagnetic Waves
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| Accelerating charges create | Electromagnetic Waves
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| nucleus with negatively charged electrons orbiting around them | atoms
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| positively charged protons and neutral neutrons | Nuclei
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| number of protons | atomic number
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| determines the chemical element properties | atomic number
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| total number of neutrons and protons | atomic weight
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| number of neutrons determins the | isotope
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| when atoms gain or lose electrons | ions
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| same number of electrons as protons | neutral atoms
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| losing electrons | ionized
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| when electrons drop from a higher level to a vacancy in a lower level they emit | photons
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| quanta of light. they have momentum and energy given by their frequency times Planck's Constant. they also behave like waves | photons
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| Spectra - when all wavelengths are present | continuous
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| when hot solid objects or high pressure gasses radiate | Black Body Radiation
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| Spectra - when light is present at all wavelengths EXCEPT at certain wavelengths | absorption
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| when light passes through a diffuse gas and certain wavelengths are absorbed out of the light that continues on | absorption
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| when light is present ONLY at certain wavelengths | emission
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| when light passes through a diffuse gas and is absorbed, raising electrons to higher levels, when those electrons drop back down they emit light | emission
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| due to fundamental quantum effects | natural width
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| due to doppler shift from the motion of the emitting molecules at any temperature above absolute zero | thermal broadening
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| due to frequent collisions of the emitting atoms in a high pressure gas | collisional broadening
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| due to the splitting of levels in strong magnetic fields | zeeman effect
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| due to emission from a rapidly rotating star where the doppler shifts mix from emissions on different sides of the star | rotational broadening
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| the positioins of the lines are a characteristic function of the individual emitting elements. this allow identification of the relative composition of the source | spectral line positions
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| these characteristic positions are shifted by the doppler effect when the entire source is moving with respect to the observers on the earth | spectral line positions
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| a difference of 5 magnitudes means a factor of <blank> in brightness | 100, (2.5)^difference in magnitude
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| the smaller the algebraic value of the magnitude the <blank> the source | brighter
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| <blank> magnitudes are the magnitude a star would have if it were at a distance of 10 parasecs | absolute
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| <blank> magnitude is the magnitude that an object appears to have | apparent
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| if you know both the apparent and absolute magnitudes, you can calculate the <blank> | distance
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| the relative brightness of stars is a function of | temperature, surface area and distance
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| the surface brightness varies as T^4 | temperature
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| the total luminosity is proportional to R^2 | surface area
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| apparent brightness is proportional to 1/d^2 | distance
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| the spectral type classification scheme is a surface <blank> classification for stars | temperature
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| O B A F G K M | Oh Be A Fine Girl Kiss Me
<==hot -- cold==>
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| within each letter class there are sub-classes numbered 0-9 from | hotter to cooler
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| from kepler's and newton's laws, the masses of each star in a binary system can be determined | (M1+M2)p^2 = (r1+r2)^3 and M1/M2 = r2/r1
need to determine p, r1 and r2 to find M1 and M2
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| not a true binary but an optical double | optical
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| a true binary where both stars are clearly seen | visual
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| only one star is seen, but moves in an oscillatory way | astrometric
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| when viewed edge on-the spectral lines are alternately doppler shifted as the stars orbit one another | spectroscopic
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| the light shows two incompatible spectra | spectrum
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| the intensity of the light dims as the stars eclipse. these are usually also spectroscopic binaries as well | eclipsing
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| the bayer catalog divided the sky into <blank> constellations and named the stars with respect to the constellation they are in | 88
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| named by constellation but with latin letters starting with R-Z, RR-ZZ, AA-QQ | variable stars
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