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| Atoms that have the same number of PROTONS but different number of NEUTRONS |
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| an atom that has gained or lost electrons |
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| attraction of electrons btwn their negative and positive charge on the nucleus |
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| energy holding the electron to the atom |
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| visible surface of the star |
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| the radiation emitted by a heated object. Emitted by hot objects but also by cold ones. the hotter an object is the more blackbody radiation it emits |
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| Wavelength of Maximum Intensity |
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| wavelength @ which the object emits the most intense radiation, occurs at some intermediate wavelength |
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| used as a thermometer to find the temperature of stars |
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| apparent change in the wavelength of radiation caused by the motion of the source |
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| The average distance between the Earth and the Sun- approx. 150 Million KM |
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| distance at which one AU is seen as one arcsecond. Unit of LENGTH. 3.26 lightyears/ 19 trillion miles |
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| unit of angle, 1/60 of one minute of one angle |
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| describes electromagnetic radiation emitted from a black body at absolute temperature T. Lambda(max)= 2.9 x 10 6^/ T (nmxk) |
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| Temperature of the universe |
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| Approximate age of our Solar System |
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| What part of an element defines it in the periodic table? |
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| number of NEUTRONS -determines weight |
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| in nucleus of atom, mass of 1, positive electric charge |
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| mass of 1, NO electric charge |
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| Number of protons + number of neutrons in nucleus |
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| nucleus with at least one electron orbiting it |
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| force that binds electron cloud around nucleus |
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| The farther away galaxies are, ________ |
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| The Faster they are traveling. We know this because they are more redshifted |
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| 10 -6^ Second after Big Bang |
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Definition
| quarks combine into protons/neutrons and their antimatter equivalents. Most come together and annihilate each other |
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| 1. force that holds particles in the nucleus together (protons/protons; protons/neutrons), operates over very short distance |
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| 1/137 of strong force. Force that holds electrons to nucleus, operates over long distance (infinity) |
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| 10 -5^ of strong force. Holds individual sub-atomic particles together, operates over very short distance, responsible for beta decay |
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| 6 x 10-38^ of strong force; attractive force between anything with mass; operates over long distance – infinity |
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| galaxies are receding away from us at a speed proportional to their distance. i.e. further away = moving faster; i.e. far galaxies = more redshifted. |
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| Which galaxy is the closest to us? |
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| How do we know that the farther the galaxies, the faster they are receding away from us? |
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| their spectral lines are more red shifted |
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| Extra-Galactic collisions |
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| when galaxies collide, creating shockwaves that compress molecular clouds. These are common while star collisions are extremely uncommon. |
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| repulsion between nuclei in nuclear fusion |
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| series of 3 nuclear reactions that builds a helium nucleus by adding together protons. Can only occur at temperatures greater than 4 million K. It is most efficient at temperatures greater than 10 million K. The sun makes 90% of its energy using the proton proton chain |
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| positively charged electron |
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| subatomic particle having an extremely low mass and a velocity nearly equal to the velocity of light |
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| heavy hydrogen nucleus containing a proton and neutron |
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| Reaction 1 of Proton-Proton Chain |
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| two hydrogen nuclei combine and form a positron |
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| reaction 2 of proton-proton chain |
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| heavy hydrogen nucleus absorbs another proton, with emission of gamma ray it becomes a lightweight nucleus |
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| reaction 3 of proton-proton chain |
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| two lightweight helium nuclei combine to form nucleus of normal helium and 2 hydrogen nuclei |
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| What is the net result of proton proton chain? |
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| Transformation of 4 hydrogen nuclei into 1 helium nucleus and energy. |
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| expressed in units of arcseconds per year. it is the movement of the stars (very slight) against the background of other stars |
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| half the total shift of the sta. the shift as seen over 1 AU baseline |
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| total amount of light the star emits |
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| energy in joules per second falling on 1 square meter (apple falling off the table) |
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| absolute visual magnitude |
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| expression of the intrinsic brightness of a star |
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| total energy one star radiates in one second, luminosity = (surface area) x (energy radiated per square meter) |
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| absolute bolometric magnitude |
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| absolute magnitude the star would ahve fi you could see all wavelengths |
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| bottom end of main sequence of HR diagram, small, cool, low luminosity |
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| lies in lower left of HR diagram, low luminosity, high temperatures. one of the most common stars. it is a compact object ( remnant of a burnt star) |
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| measurement of stellar parallax estimated from star's spectral type, luminosity class, apparent magnitude |
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| carbon/nitrogen/oxygen. Fusion reaction by which stars convert hydrogen to helium. This process is utilized by massive main-sequence stars because they are hot enough to fuse hydrogen to helium. |
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| a star becomes a giant star, helium nuclei fuse together to make carbon. |
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| when a gas is so dense that its electrons are not free to change their energy |
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| any star that changes its brightness in a periodic way. Can be an eclipsing binary but many others are single stars |
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| process causing mass loss in giant stars -periodic eruptions in helium fusion shell. |
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| implies a star more massive than 1.4 solar masses cannot become a white dwarf unless it sheds mass in some way |
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| new star appearing in the sky, growing brighter, then fading away after a few weeks, an explosion involving a white dwarf. |
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| longer lasting/ more luminous nova. caused by violent, explosive death of a massive star |
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| violent re-ignition of a thermonuclear fusion in a dead star. produces a wide range of heavier nuclei |
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| very massive stars with very short lifespans formed rapidly. |
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| Stars generate energy by nuclear _____? |
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| Fusion: combining two light nuclei to make a heavier one |
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| central energy and gravity balances the outward pressure and prevents collapse |
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| 50% more massive than our Sun. basically a gigantic nucleus: protons and electrons have combined to form nucleus |
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forms when the first slow-ejected gases
from the red giant become heated by fast-ejected stellar winds |
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| using the apparent change in position of a star due to the position of the Earth observer. |
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| Evidence for the big bang? |
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| Doppler "Redshift" of the galaxies; cosmic microwave background radiation |
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| How many km in a light year? |
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| # of waves that pass a stationary point in one second |
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| a particle of electromagnetic radiation. a bundle of waves. amount of energy carried is inversely related to its wavelength |
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| The electromagnetic spectrum in order from longest to shortest |
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Definition
| Radio, Microwave, Infrared, Visible, Ultraviolet, Xray, Gamma Ray (Ready? Many Infants Vomit Upon eX-Girlfriends) |
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Definition
| primary/objective lens bends light as it passes through the glass and brings it to a focus to form a small inverted image |
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| primary/objective mirror forms and image by reflecting the light |
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| the motion of molecules/ atoms in any object |
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| the flow of thermal energy |
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| average speed of the movement of particles w/i an object |
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