Astronomy Chapters 1 – 7 – Flashcards

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universe
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totality of all space, time, matter, and energy
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astronomy
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study of the universe
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light-years
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distance that light, moving at a constant speed of 300,000 km/s, travels in one year. One of these is about 10 trillion kilometers
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theory
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framework of ideas and assumptions used to explain some set of observations and make predictions about the real world
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theoretical model
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attempt to construct a mathematical explanation of a physical process or phenomenon, within the assumptions and confines of a given theory. the model generally makes new predictions that can be tested by further observation
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scientific method
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set of rules used to guide science, based on the idea that scientific "laws" by continually tested, and modified or replaced if found inadequate
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constellations
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human grouping of stars in the night sky into a recognizable pattern
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celestial sphere
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imaginary sphere surrounding Earth to which all objects in the sky were once considered to be attached
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rotation
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spinning motion of a body about an axis
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celestial poles
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projection of Earth's North and South pole onto the celestial sphere
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celestial equator
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projection of Earth's equator onto the celestial sphere
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solar day
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period of time between the instant when the Sun is directly overhead (i.e. noon) to the next time it is directly overhead
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sidereal day
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time needed between successive risings of a given star
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diurnal motion
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daily progress of the sun and the other stars across the sky is known as
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revolution
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orbital motion of one body about another, such as Earth about the Sun
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zodiac
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12 constellations on the celestial sphere through which the Sun appears to pass during the course of a year
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summer solstice
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point on the ecliptic where the Sun is at its northernmost point above the celestial equator, occurring on or near June 21
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winter solstice
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point on the ecliptic where the Sun is at its southernmost point below the celestial equator, occurring on or near December 21
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seasons
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changes in average temperature and length of day that result from the tilt of Earth's (or any planet's) axis with respect to the plane of its orbit
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autumnal equinox
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date on which the Sun crosses the celestial equator moving southward, occurring on or near September
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vernal equinox
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date on which the Sun crosses the celestial equator moving northward, occurring on or near March 21
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tropical year
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the time interval between one vernal equinox and the next
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precession
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slow change in the direction of the rotation axis of a spinning object, caused by some external gravitation influence
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sidereal year
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time required for the constellations to complete one cycle around the sky and return to their starting points, as seen from a given point on Earth.
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phases
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appearance of the sunlit face of the moon at different points along its orbit, as seen from Earth
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new Moon
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all but invisible in the sky
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quarter Moon
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one week after new Moon, half of the lunar disk can be seen
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sidereal month
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time required for the moon to complete one trip around the celestial sphere
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eclipse
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event during which one body passes in front of another, so that the light from the occulted body is blocked
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lunar eclipse
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celestial event during which the moon passes through the shadow of Earth, temporarily darkening its surface
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partial eclipse
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celestial event during which only a part of the occulted body is blocked from view
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total eclipse
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celestial event during which one body is completely blocked from view by another
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solar eclipse
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celestial event during which the new moon passes directly between Earth and the sun, temporarily blocking the sun's light
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total solar eclipse
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alignment is perfect, planets and some stars become visible in the daytime as the Sun's light is reduced to nearly nothing
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partial solar eclipse
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Moon's path is slightly "off center" and only a portion of the Sun's face is covered
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umbra
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central region of the shadow cast by an eclipsing body
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penumbra
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portion of the shadow cast by an eclipsing object in which the eclipse is seen as partial
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annular eclipse
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solar eclipse occurring at a time when the moon is far enough away from Earth that it fails to cover the disk of the Sun completely, leaving a ring of sunlight visible around its edge
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line of nodes
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line of intersection of Earth's and the Moon's orbital planes
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eclipse seasons
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time of the year when the moon lies in the same plane as Earth and Sun, so that eclipses are possible
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triangulation
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method of determining distance based on the principles of geometry. a distant object is sighted from two well-separated locations. distance between the two locations and the angle between the line joining them and the line to the distant object are all that are necessary to ascertain the object's distance
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cosmic distance scale
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collection of indirect distance-measurement techniques that astronomers use to measure distances in the universe
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parallax
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apparent motion of a relatively close object with respect to a more distant background as the location of the observer changese
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supernova
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explosion of a giant star, which scattered most of its mass into spaces
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cosmology
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study of the workings of the universe on the largest scales
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retrograde motion
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backward, westward loop traced out by a planet with respect to the fixed stars
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geocentric
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model of the solar system that holds that Earth is at the center of the universe and all other bodies are in orbit around it. Earliest theories of the solar system were geocentric
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epicycle
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construct of the geocentric model of the solar system which was necessary to explain observed planetary motions. each planet rides on a small ________ whose center in turn rides on a larger circle (the deferent)
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deferent
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construct of the geocentric model of the solar system which was needed to explain observed planetary motions. large cirlce encircling earth, on which an epicycle moves
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Ptolemaic model
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geocentric solar system model, developed by the second-century astronomer Cladius Ptolemy. predicted with great accuracy the positions of the then known planets
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heliocentric
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model of the solar system that is centered on the sun, with earth in motion about the sun
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Copernican revolution
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realization, toward the end of the 16th century, that earth is not at the center of the universe
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aberration of starlight
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small shift in the observed direction to a star, caused by Earth's motion perpendicular to the line of sight
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Copernican principle
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removal of Earth from any position of great cosmic significance is generally known as
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laws of planetary motion
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three laws derived by kepler describing the motion of the planets around the sun
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ellipse
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geometric figure resembling an elongated circle. characterized by its degree of flatness, or eccentricity, and the length of its long axis.
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focus
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one of two special points within an ellipse, whose separation from each other indicates the eccentricity.
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semimajor axis
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one-half of the major axis of an ellipse. the way in which the size of an ellipse is usually quantifies
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eccentricity
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measure of the flatness of an ellipse, equal to the distance between the two foci divided by the length of its major axis
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Kepler's first law
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Orbital paths of the planets are elliptical (not circular) with the Sun at one focus
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Kepler's second law
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An imaginary line connecting the Sun to any planet sweeps out equal areas of the ellipse in equal intervals of time
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period
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time needed for an orbiting body complete one revolution about another body
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Kepler's third law
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Square of a planet's orbital period is proportional to the cube of its semimajor axis
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astronomical unit
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average distance of Earth from the Sun.
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radar
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acronym for radio detection and ranging. radio waves are bounced off an object, and the time taken for the echo to return indicates its distance
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weight
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gravitational force exerted on you by earth
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force
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action on an object that causes its momentum to change. the rate at which the momentum changes is numerically equal to the force
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inertia
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tendency of an object to continue moving at the same speed and in the same direction
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mass
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measure of the total amount of matter contained within an object
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velocity
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displacement (distance plus direction) per unit time
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acceleration
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gradual growth of bodies, such as planets, by the accumulation of other smaller bodies
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gravity
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attractive effect that any massive object has on all other massive objects
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gravitational force
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force exerted on one body by another due to the effect of gravity. force is directly proportional to the masses of both bodies involved and inversely proportional to the square of the distance between them
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inverse-square law
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law that a field follows if its strength decreases with the square of the distance. fields that follow this decrease rapidly in strength as the distance increase, but never quite reach zero
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center of mass
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"average" position in space of a collection of massive bodies, weighted by their masses. for an isolated system this point moves with constant velocity, according to Newtonian mechanics
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escape speed
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speed necessary for one object to escape the gravitational pull of another. anything that moves away from a gravitation body with more than the escape speed will never return
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unbound
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orbit which does not stay in a specific region of space, but where an object escapes the gravitational field of another.
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electromagnetic radiation
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another term for light, transfers energy and information from one place to another
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visible light
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small range of the electromagnetic spectrum that human eyes perceive as light. visible spectrum ranges from about 4000-7000 angstroms, corresponding to blue through red light
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radio
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region of electromagnetic spectrum corresponding to the longest wavelength radiation
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infrared
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region of the electromagnetic spectrum just outside the visible range, corresponding to light of a slightly longer wavelength than red light
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x-rays
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region of the electromagnetic spectrum corresponding to radiation of high frequency and short wavelength, far beyond the visible spectrum
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gamma rays
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region of the electromagnetic spectrum, far beyond the visible spectrum, corresponding to radiation of very high frequency and very short wavelength
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waves
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pattern that repeats itself cyclically in both time and space. characterized by the speed at which they move, their frequency, and their wavelength
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amplitude
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maximum deviation of a wave above or below the zero point
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frequency
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number of wave crests passing any given point in a unit time
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electron
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elementary particle with a negative electric charge; one of the components of the atom
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proton
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elementary particle carrying a positive electric charge, a component of all atomic nuclei. number of these in the nucleus of an atom dictates what type of atom it is
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electric field
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field extending outward in all directions from a charged particle, such as a proton or electron. determines the electric force exerted by the particle on all other charged particles in the universe; the strength of this decreases with increasing distance from the charge according to an inverse-square law
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magnetic field
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field that accompanies any changing electric field and governs the influence of magnetized objects on one another
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electromagnetism
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union of electricity and magnetism, which do not exist as independent quantities but are in reality two aspects of a single physical phenomenon
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wave theory of radiation
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description of light as a continuous wave phenomenon, rather than as a stream of individual particles
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electromagnetic spectrum
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complete range of electromagnetic radiation, from radio waves to gamma rays, including the visible spectrum. all types of electromagnetic radiation are basically the same phenomenon, differing only by wavelength, and all move at the speed of light
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opacity
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quantity that measures a material's ability to block electromagnetic radiation
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diffraction
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ability of waves to bend around corners. establishes its wave nature
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interference
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ability of two or more waves to interact in such a way that they either reinforce or cancel each other
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temperature
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measure of the amount of heat in an object, and an indication of the speed of the particles that comprise it
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blackbody curve
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characteristic way in which the intensity of radiation emitted by a hot object depends on frequency. frequency at which the emitted intensity is highest is an indication of the temperature of the radiating object
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Wien's Law
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relation between the wavelength at which a black body curve peaks and the temperature of the emitter. the peak wavelength is inversely proportional to the temperature, so the hotter the object, the bluer its radiation
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Stefan's law
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relation that gives the total energy emitted per square centimeter of its surface per second by an object of a given temperature. shows that the energy emitted increases rapidly with an increase in temperature, proportional to the temperature raised to the fourth power
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Doppler effect
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any motion-induced change in the observed wavelength (or frequency) of a wave
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spectroscope
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instrument used to view a light source so that it is split into its component colors
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continuous spectra
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spectrum in which the radiation is distributed over all frequencies, not just a few specific frequency ranges. A prime example is the blackbody radiation emitted by a hot, dense body
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emission lines
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bright line in a specific location of the spectrum of radiating material, corresponding to emission of light at a certain frequency. A heated gas in a glass container produces emission lines in its spectrum
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emission spectrum
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pattern of spectral emission lines produced by an element
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absorption lines
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dark line in an otherwise continuous bright spectrum, where light within one narrow frequency range has been removed
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spectroscopy
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study of the way in which atoms absorb and emit electromagnetic radiation. allows astronomers to determine the chemical composition of stars
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Kirchhoff's laws
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three rules governing the formation of different types of spectra
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atoms
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building block of matter, composed of positively charged protons and neutral neutrons in the nucleus surrounded by negatively charged electrons
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nucleus
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dense, central region of an atom, containing both protons and neutrons, and orbited by one or more electrons
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ground state
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lowest energy state that an electron can have within an atom
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ionized
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state of an atom or molecule that has lost one or more of its electrons
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orbitals
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one of several energy states in which an electron can exist in an atom
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quantized
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fact that light and matter on small scales behave in a discontinuous manner, and manifest themselves in the form of tiny "packets" of energy, call quanta
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quantum mechanics
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laws of physics as they apply on atomic scales
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excited state
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state of an atom when one of its electrons is in a higher energy orbital than the ground state
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photons
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individual packet of electromagnetic energy that makes up electromagnetic radiation
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photoelectric effect
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emission of an electron from a surface when a photon of electromagnetic radiation is absorbed
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element
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matter made up of one particular atom. number of protons in the nucleus of the atom determines which _______ it represents
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neutrons
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an elementary particle with roughly the same mass as a proton, but which is electrically neutral. form the nuclei of atoms
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molecule
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a tightly bound collection of atoms held together by the atoms' electromagnetic fields. emit and absorb photons at specific wavelengths
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telescope
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instrument used to capture as many photons as possible from a given region of the sky and concentrate them into a focused beam for analysis
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refraction
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tendency of a wave to bend as it passes from one transparent medium to another
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refracting telescope
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a telescope that uses a lens to gather and focus light from a distant object
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reflecting telescope
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a telescope which uses a curved mirror to focus light from a distant object
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prime focus
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point in a reflecting telescope where the mirror focuses incoming light to a point
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images
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optical representation of an object produced when the object is reflected or refracted by a mirror or lens
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Newtonian telescope
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basic laws of motion, postulated by Newton, which are sufficient to explain and quantify virtually all of the complex dynamical behavior found on Earth and elsewhere in the universe
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Cassegrian telescope
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type of reflecting telescope in which incoming light hits the primary mirror and is then reflected upward toward the prime focus, where a secondary mirror reflects the light back down through a small hole in the main mirror into a detector or eyepiece
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angular resolution
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ability of a telescope to distinguish between adjacent objects in the sky
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diffraction-limited resolution
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theoretical resolution that a telescope can have due to diffraction of light at the telescope's aperture. depends on the wavelength of radiation and the diameter of the telescope's mirror
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charge-coupled devices (CCDs)
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electronic device used for data acquisition; composed of many tiny pixels, each of which records a buildup of charge to measure the amount of light striking it
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photometry
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branch of observational astronomy in which the brightness of a source is measured through each of a set of standard filters
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spectrometer
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instrument used to produce detailed spectra of stars. records a spectrum on a photographic plate, or more recently, in electronic form on a computer
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photometer
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a device that measures the total amount of light received in all or part of the image
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seeing
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term used to describe the ease with which good telescopic observations can be made from Earth's surface, given the blurring effects of atmospheric turbulence
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seeing disk
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roughly circular region on a detector over which a star's point-like images is spread, due to atmospheric turbulence
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light pollution
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unwanted upward-directed light from streets, homes, and businesses, that scatters back to Earth from dust in the air, obscuring the faint objects that astronomers want to observe
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active optics
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collection of techniques used to increase the resolution of ground-based telescopes. minute modifications are made to the overall configuration of an instrument as its temperature and orientation change; used to maintain the best possible focus at all timesla
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adaptive optics
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collection of techniques used to increase the resolution of a telescope by deforming the shape of the mirror's surface under computer control while a measurement is being taken; used to undo the effects of atmospheric turbulence
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radio telescopes
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large instrument designed to detect radiation from space at radio wavelengths
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interferometry
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technique in widespread use to dramatically improve the resolution of radio and infrared maps. several telescopes observe the object simultaneously, and a computer analyzes how the signals interfere with each other
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interferometer
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collection of two or more telescopes working together as a team, observing the same object at the same time and the same wavelength. effective diameter of an this is equal to the distance between its outermost telescopes
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infrared telescopes
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telescope designed to detect infrared radiation. many such telescopes are designed to be lightweight so that they can be carried above (most of) Earth's atmosphere by balloons, airplanes, or satellites
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ultraviolet telescope
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telescope that is designed to collect radiation in the ultraviolet part of the spectrum. earth's atmosphere is partially opaque to these wavelengths, so ultraviolet telescopes are put on rockets, balloons, and satellites to get high above most or all of the atmosphere
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high-energy telescopes
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telescope designed to detect X- and gamma-ray radiation
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collecting area
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total area of a telescope capable of capturing incoming radiation. larger the telescope, the greater its __________ and the fainter the objects it can detect
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pixels
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one of many tiny picture elements, organized into a two dimensional array making up a digital image
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solar system
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sun and all the bodies that orbit it -- Mercury, Venus, Earth, Mars, Jupiter, Saturn, Uranus, Neptune, their moons, the asteroids, the comets, and trans-Neptunian objects
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comparative planetology
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systematic study of the similarities and differences among the planets, with the goal of obtaining deeper insight into how the solar system formed and has evolved in time
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density
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measure of the compactness of the matter within an object, computed by dividing the mass of the object by its volum
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terrestrial planets
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one of the four innermost planets of the solar system, resembling Earth in general physical and chemical properties
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nebular theory
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one of the earliest models of the solar system formation, dating back to Descartes, in which a large cloud of gas began to collapse under its own gravity to form the Sun and planets
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solar nebula
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swirling gas surrounding the early Sun during the epoch of solar system formation, also referred to as the primitive solar system
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condensation theory
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currently favored model of solar system formation which combines features of the old nebular theory with new information about interstellar dust grains, which acted as condensation nuclei
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planetsimals
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term given to objects in the early solar system that had reached the size of small moons, at which point their gravitational fields were strong enough to begin influencing their neighbors
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gravitational instability theory
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theory that the jovian planets formed directly from the solar nebula via instabilities in the gas leading to gravitational contraction
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core-accretion theory
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theory that the jovian planets formed when icy protoplanetary cores became massive enough to capture gas directly from the solar nebula
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core
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central region of Earth, surrounded by the mantle
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mantle
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layer of Earth just interior to the crust
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crust
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layer of Earth which contains the solid continents and the seafloor
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hydrosphere
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layer of Earth that contains the liquid oceans and accounts for roughly 70% of Earth's total surface area
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atmosphere
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layer of gas confined close to a planet's surface by the force of gravity
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troposphere
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portion of Earth's atmosphere from the surface to about 12 km
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convection
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churning motion resulting from the constant upwelling of warm fluid and the concurrent downward flow of cooler material to take its place
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magnetosphere
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a zone of charged particles trapped by a plent's magnetic field, lying above the atmosphere
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ionosphere
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layer in Earth's atmosphere above about 80 km where the atmosphere is significantly ionized and conducts electricity
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stratosphere
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portion of Earth's atmosphere lying above the troposphere, extending up to an altitude of 40 - 50 km
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ozone layer
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layer of Earth's atmosphere at an altitude of 20 - 50 km where incoming ultraviolet solar radiation is absorbed by oxygen, ozone, and nitrogen in the atmosphere
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greenhouse effect
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partial trapping of solar radiation by a planetary atmosphere, similar to the trapping of heat in a greenhouse
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seismic waves
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a wave that travels outward from the site of an earthquake through Earth
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inner core
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central part of Earth's core, thought to be solid, and composed mainly of nickel and iron
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outer core
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outermost part of Earth's core, thought to be liquid and composed mainly of nickel and iron
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differentiation
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variation in the density and composition of a body such as Earth, with low-density material on the surface and higher density material in the core
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radioactive
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release of energy by rare, heavy elements when their nuclei decay into lighter nuclei
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plate tectonics
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motions of regions of Earth's lithosphere, which drift with respect to one another aka continental drift
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lithosphere
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Earth's crust and a small portion of the upper mantle that make up Earth's plates. this layer of Earth undergoes tectonic activity
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asthenosphere
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layer of Earth's interior, just below the lithosphere, over which the surface plates slide
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rock cycle
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process by which surface rock on Earth is continuously redistributed and transformed from one type into another
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Van Allen belts
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one of at least two doughnut-shaped regions of magnetically trapped, charged particles high above Earth's atmosphere
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dynamo theory
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theory that explains planetary and stellar magnetic fields in terms of rotating, conducting material flowing in an object's interior
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tides
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rising and falling motion of terrestrial bodies of water, exhibiting daily, monthly, and yearly cycles.
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aurora
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event that occurs when atmospheric molecules are excited by incoming charged particles from the solar wind, then emit energy as they fall back to their ground states. generally occur at high latitudes near the north and south magnetic poles
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tidal bulges
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elongation of earth caused by the difference between the gravitational force on the side nearest the Moon and the force on the side farthest from the Moon. the long axis of this points toward the Moon. More generally, the deformation of any body produced by the tidal effect of a nearby gravitating object
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theory, prediction, and observation
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The fundamental 3 elements in the scientific method are
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in the same part of the sky
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Stars in a constellation are
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spring, occurs around March 21-22
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vernal equinox
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gravitation pull of both the Moon and the Sun
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Precession of the Earth's axis is caused by
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wanning gibbous
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what is the name of the Moon's phase is 3/4 visible on left side
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about every six months at new moon
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solar eclipse happens
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decreases if the object is farther away
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angular diameter of an object
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why retrograde motion occurred
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epicycles were used in Ptolemy's model to explain
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the Sun revolved around the Earth
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How did the geocentric model account for day and night on Earth?
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Sun is the center of the solar system
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heliocentric model assumes
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Satellites of Jupiter
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Which of Gelilei's initial observations was most challenging to established geocentric beliefs?
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he assumed planets moved in cycles
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Copernicus' heliocentric model was flawed because
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period
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Kepler's third lawy relates a planet's distance from the Sun to its orbital...
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Galileo Galilei
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Who published the first astronomical observations with a telescope?
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Johannes Kepler
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Who published three empirical laws of planetary motion?
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increase with the mass of the object
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Newton's laws of gravity states that the force between two objects
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wavelength
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distance between successive wave crests defines the ________ of a wave
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sound
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Which of the following waves is NOT a form of electromagnetic radiation
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temperature
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frequency at which a star's intensity is greatest depends directly on its
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toward higher frequencies
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the blackbody curve of a star moving towards earth would have its peak shifted
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visible light and radio waves
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which two types of electromagnetic radiation from space reach the surface of Earth
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at the same speed
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Compared with red light, blue wavelengths of visible light travels
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are moving very fast
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temperature of an object has a specific meaning for its atoms. A very hot objects have atoms that
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increase 16 times
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Stefan's law implies that if the Sun's temperature were to double, its energy emission would
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hotter than
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Rigel appears as a bright bluish star, whereas Betelgeuse appears as a bright reddish star. Rigel is _______ than Betelgeuse
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are identical to its absorption lines
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Wavelengths of the emission lines produced by an element
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a photon is emitted
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when an electron in an atom moves from a higher energy level to a lower energy level
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of a different composition
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compared with a star having many blue absorption lines, a star with many red and blue absorption lines must be
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its spectral lines are shorter in wavelength
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if a light source is approaching you, you will observe
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transverse velocity (side-to-side)
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what can analyzing a star's spectral lines not tell us ?
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reflecting telescopes aren't affected by the atmosphere as much
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one reason why modern telescopes use mirrors rather than lenses
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larger telescopes and shorter wavelengths
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resolution of a telescope is improved by using
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HST orbits above the atmosphere
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Hubble Space Telescope offers sharper images than ground telescopes primarily because
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advantages of CCDs over photographic film
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they don't require chemical development, digital data is easily stored and transmitted, CCDs are more light sensitive than film, CCD images can be developed faster
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the image quality due to air turbulence
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"seeing" in astronomy is a measurement of
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reducing atmospheric blurring using computer control
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adaptive optics refer to
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observations can be made day and night
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radio telescopes are useful because
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cool stars and star-forming regions
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infrared telescopes are very useful for observing
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because of turbulence in the atmosphere
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Why do stars twinkle?
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increase the range of waves they can collect
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Radio dishes are large in order to
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angular resolution
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interferometry can greatly improve
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Mercury, Venus, Earth, Mars, Jupiter, Saturn, Uranus, Neptune
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What is the correct order of the planets according to increasing distance from the Sun?
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Mercury, Venus, Earth, Mars
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What are the terrestrial planets?
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high average density
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What is NOT a characteristic of Jovian planets?
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no
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is pluto a Jovian planet?
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Oort Cloud
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What is the name of the most outer region of the Solar System, where many comets reside
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no
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Does the theory of the origin of the Solar System that the direction that planets orbit the sun is opposite to the Sun's spin correct?
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ancient material from the formation of the solar system
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Asteroids are evidence of
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terrestrial planets are different from Jovian planets
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Condensation theory explains why
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faster due to conservation of angular momentum
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as rotating gas cloud contracts, it spins:
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growth of an object by the accumulation of matter
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What is the process of accretion?
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ultraviolet radiation
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planetary atmosphere with ozone could protect surface dwellers from
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troposphere
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within Earth's atmosphere, in which layer does convection occur?
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synodic month
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time required for the Moon to complete a full cycle of phases
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