They are located along the top of the H-R diagram. If the star’s mass is too small, the central temperature will be too low to sustain fusion reactions. Start studying SOME ANSWERS TO ASTRO. Observations of V404 Cygni during the 2015 outburst by the Nasu telescope array at 1.4 GHz Learn vocabulary, terms, and more with flashcards, games, and other study tools.

USD $35.00 production of magnetic field of the sun; and that sunspots vary over an 11 year periodfirst to detect solar neutrinos -- homestake detectormeasure velocity in the shift of lines, doppler shiftE = mc^2 - discovered energy mass equivalent --- mass loss in nuclear reactionsfirst to observe sun's magnetic field; discovered magnetic fields in sunspotsthe development of a classification system for stars to divide them by spectral type, stage in development and luminosity -- HR diagramsun spot activity --- discovered the minimum long term interval when there were no sunspotsDetector for solar neutrinos and two other types of neutrinos --- showed that there are three types -- electron neutrino is the one in the sun200 years ago proposed what we now call black holes --- he proposed that a star might be so massive and its gravitational pull so massive that light can't escapethat the corona is so hot that it will be forever expanding and carrying the sun away in the solar wind --- proposed solar windspropose the neutrino as an unseen particle moving at nearly the speed of light which carries away beta decaynobel prize of neutrino work -- first to show that neutrinos could be observedshowed that there is a radius of a black hole that is smaller than the Schwarzschild radius --- the radius is the extent of a black holeradius of neutron star; determined that there is an iodized hydrogen cloud around stars; bigger radius means hotter starmagnetic field splitting/polarization of magnetic fields (how to determine strength and direction of magnetic fieldThe collapsing core of a star that has exploded as a Type 2 supernova can become a neutron star or a black hole, depending on its mass. Using this formula, the ages of HII-A, HII-B, and HII-C are estimated to be t age ≃ 1.4 × 10 4, 1.7 × 10 4, and 2.0 × 10 4 yr, respectively. Exactly which reactions take place in a given star depends on its mass, and therefore its core temperature and densityis up there now measuring the transverse velocities and luminosities of starslots of the color images of cosmic stuff like planetary nebulaeto determine nuclear reactions on the sun -- on the surface from the explosionstwo spacecrafts that are both orbiting around the sun in the same orbit which provide a 3D image of coronal mass ejectionswas the first to go over the poles of the sun - found very weird thing that very heavy ions in the coronal holes move faster than the lighter protons moleculespast the giant planets and is at the edge of our solar systemmapped out the detailed X-ray emission of the sun - helped discover coronal loopsin the outer atmosphere of the sun and their wavelengths tell us what are in the sunare a form of forbidden lines and can be seen in emission nebulaechange in wavelength caused by radial motion of objectsforbidden in the terrestrial laboratory -- cannot be made on earthany of the dark absorption lines in the spectrum of the sun that can be seen when sunlight is passed through a prism to separate it into the colors of the rainbow --- the dark lines are where the light passing through the photosphere and chromosphere was absorbedis a cloud in the interstellar medium composed of neutral atomic hydrogen, in addition to the local abundance of helium and other elements (21 CM LINE)a region of interstellar atomic hydrogen that is ionized (IS THE SAME AS THE EMISSION NEBULA)is the red visible spectral line created by a hydrogen atom when an electron falls from the 3rd to the 2nd energy level -- balmer seriesis an indirect method for finding extrasolar planets and brown dwarfs from radial-velocity measurements via observation of Doppler shifts in the spectrum of the planet's parent stara way to look at radio radiation, spin transition of the rotating electron in a hydrogen atom, an unenergetic change in an electron happens when electrons stay in the hydrogen atom but change direction -- when that happens a line is emitted ---- h1 region bc the hydrogen atoms are NOT ionized because the electrons are NOT torn free from the hydrogenhot ball of gas that emits thermal radiation, the radiation is more intense the hotter the gas is -- its thermal radiationwhen an electron is torn free from the sun; free electron radiationare emitted by relatively cold interstellar stars/gasesthe radiation of energized electrons meeting a magnetic field and circling around it; the way radio waves are produced between the stars,is relative, depending on the motion of both the observer and the starradio waves have much longer wavelengths than visible light wavesonly place where the radiation of the sun is manufacturedvery thin layer with a temperature of 10,000 K that lies just above the photospherea boiling area where the gas are transported through convective currentsmillion degree atmosphere above the disk of the sun, the outer atmosphere of the sun and lies above the visible disk of the sun --- it expands to make solar windsmagnetized loop, hold the million degree gas of the corona in placeat poles, corona is wide open, open magnetism, fast solar winds rush outlooking inside the sun using sound waves, can tell where the convective zone issphere of influence of the sun, region in which the sun dominates the motion of charged particlessun gets brighter as time goes on, it was way dimmer when it was first created -- only reason that the earth wasn't therefore cooler then is because there mustve been a larger GHG effectmeasures strength and direction of a magnetic fieldthought to push elements like oxygen in coronal holesno charge, electron neutrinos are produced in the sun as a product of nuclear fusion, they were first hypothesized to explain radioactive decay, almost speed of lightvisible disk of the sun, oscillated due to sound waves inside the sun that can't get outa brief eruption of intense high energy radiation from the sun's surface, associated with sunspots and harms earth a lotgenerated in the convective zone --- cause the sun to pulsate11 year variation in sunspot number and position -- bands move down from mid latitudes when the amount decreasessunspots come in pairs with opposite magnetic polaritieslocation where the suns magnetic field is originated, below the convective zone, magnetic field made below in the tachocline, the tachocline is the transition region of the sun between the radiative interior and the differentially rotating outer convective zonethe first detector to show that neutrinos come from the sunshow that there are more than one type of neutrino and that there are fewer than expected in the sunradioactive elements such as uranium, hypothesized to explain why neutrinos are neutrinosproposed to exist but doesn't actually exist, hypotheses to tell why the corona is so hotenergetic charged particles, come into earth, generated from exploding stars called super novaplanets revolving around other stars, "hot jupiter"substance on the sudbury neutrino, showed that there are three different kinds of neutrinos2 protons, 2 neutrons, 2 electrons, made in the sundistance in relation to a star in which liquid water can existthe region of space, encompassing the solar system, in which the solar wind has significant influenceare a class of exoplanets that are inferred to be physically similar to Jupiter but that have a very short orbital radiiany mass greater than jeans mass will undergo gravitational collapseprocess that makes the corona hot, when coronal loops of different orientations combine into a different magnetic configurationmagnetic field of earth dominates charged particlesreason sun shines, mass loss converted to energy in nuclear reactionssubatomic particles produced by the decay of radioactive elements and lack chargeneutral uncharged particle, about as massive as a protoncan shine the same way that the sun does (hydrogen to helium by the proton proton chain) or they can shine by the CNO cyle or by consuming heliumdestruction of positrons and electrons when they meetname of first neutrino detector, detector was put next to man made nuclear reactor that was sending out man made neutrinosthe positron or antielectron is the antiparticle or the antimatter counterpart of the electron, the positron has an electric charge of +1 e, a spin of 1/2, and has the same mass as an electronthe emission of ionizing radiation or particles caused by the spontaneous disintegration of atomic nucleiappear to emit short pulses of radio radiation with pulse periods between 1.4 ms and 8.5 secondsprotons go through each other, allows for fusion to occurwhen a star uses up all its nuclear fle, its core will collapse into a neutron star or a black hole and its outer parts will explode, outer parts explode and expand, --- supernova remnants are the exploding partsWhat is the difference between thermal and non-thermal radiation?different bc of the different wavelengths of the radiation emittedNon thermal waves have longer or shorter wavelengths?overcoming electrical repulsion between two protons near the sun centerIn the core -- moves out through the radiation zone and convective zonefrom inside the sun, at the base of the convective zone at the tacholinemagnetic reconnection or coronal loops, magnetic carpetann explosive emission of energetic particles and intense radiationWhere do solar flares occur and how do we see them?In solar active regions, we see them using x-rays or radio waves (NOT VISIBLE)flares and CMEs are more frequent and powerful at maximum of activity cycle, when the cosmic rays at earth are lesshow much stellar energy is radiated by the star every secondcarbon acts as a catalyst in converting four protons into a helium nucleusHow do you determine the age of a globular star clusterfrom its turn off point on the main sequence; older clusters have lower turn off pointsThe first generation stars had no elements heavier than helium and they could only burn hydrogen by the proton proton chain, they are the oldest known stars; The second generation stars were formed after heavy elements were made inside other previous starsWhat are nebula, emission nebulae and spiral nebulae?Nebula means cloud, emission nebulae display emission lines, spiral nebulae are galaxiesIonized hydrogen, forbidden ionized oxygen and ionized nitrogenHow do electrons radiate when they encounter protons in an emission nebula?Bremstrahlung/braking radiation - free free radiation OR recombination -- free-bound radiationH2 regions, the regions between stars that are lit up by nearby starsthe sphere of ionization of emission nebula around a star --- it is determined by how dense the surrounding interstellar material is (the more dense, the smaller radius) and by how hot the inside of the star is (hotter=bigger radius)is synchrotron radiation thermal or nonthermal radiation?White dwarf (lowest mass), Neutron stars (middle mass), black hole (largest mass)the electrons can't exist in a state where they are too close together --- why stars run outPhoton energy of radio waves more or less than visible light?The collapse becomes hottest at the center -- when it becomes hot enough it prevents the collapse because radiation is emittedthe radius where something needs to move faster than the speed of light to escape -- it marks the event horizon of a black hole within nothing can be seenBy the x-ray emission from a massive member of a close binary star system
Size of H II region, r, set by rate of emission of ionizing photons, Q. Carbon, oxygen, and nitrogen are synthesized inside giant or supergiant stars.

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