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Chapter 28 – Stars and Galaxies Page 610 Why is this galaxy so bright? What shape is this galaxy? How do we obtain images like this? Chapter 28.1 A Closer Look at Light What is light? Light is a form of electromagnetic radiation (EM) Other types of EM listed from longest to shortest wavelengths Radio Microwave Infrared Visible light Ultraviolet X-rays Gamma rays This is known as the EM spectrum All EM energy travels in waves and at the speed of light Can travel through empty space (vacuum) Spectroscope Visible white light is actually made up of light of various colors each with a different wavelength The various color can be observed In a rainbow Passing light through a prism Or an astronomers instrument known as a spectroscope The colors ROY G. BIV are aligned from longest to shortest (violet) Longer wavelengths refract less Chapter 28.2 Types of spectra from spectroscopes Continuous spectrum – unbroken band of colors which are emitted by Glowing solids (filament) Glowing liquids (molten iron) Hot compressed gases (inside stars) Emission spectrum – lines of different colors Produced by glowing thin gases Each element has its own spectra therefore scientists can identify the gas Absorption spectrum – a continuous spectrum crossed by dark lines Elements in the thin gas that surround a star absorb the same wavelength they would emit The stars absorption spectrum indicates the composition of the stars outer layer The sun radiates a continuous spectrum, however, the gases in the atmosphere absorb some wavelengths. By analyzing the absorbed bands, scientists can figure out the composition of the sun’s outer layer. Absorption spectrum can also determine a planets atmosphere Doppler Effect By observing how the spectral lines are shifting, scientists can tell how a star is moving compared to the earth Move to the red end, “red shift,” the star is moving away Move to the blue end, “blue shift,” star is getting closer By using spectrums from the lab and the stars, they can determine how fast they are moving Chapter 28.3 Stars and Their Characteristics Constellations – name given to groups of stars There are 88 of them Big dipper – best known asterism (small star grouping) is actually part of a larger grouping known as Ursa Major We can use the dipper to find other constellations The stars appear to move in two ways Nightly variation – due to earth’s rotation Yearly due to earth’s revolution – winter constellation Lyra – summer constellation Orion Apparent magnitude Is the brightness of the star as seen from earth The lower the number, the brighter it is Sun is –26.7 Faintest is +6 Distance to stars Astronomical Unit (AU) distance from earth to sun – 150 million km Proxima Centauri – next nearest star is 260,000AU Therefore, astronomers use light-years – a unit of measure that light travels in one year. Light travels about 300,000km/sec 1 year = 9.5×1012 Proxima Centauri is about 4.2 light years away Elements in Stars Stars are mostly of super-hot gases – mostly H & He Mass, Size and Temperature of Stars Mass is something that can not be observed directly. It can only be calculated based on other observations Stellar mass is expressed as multiples of the sun’s mass Betelgeuse’s mass – 20 solar masses Temperature and Color Blue stars are hot Red stars are cool Luminosity The actual brightness of the star is luminosity If two stars have the same surface temperature, the larger star would be more luminous If the same size, hotter one would be brighter Types of magnitude Absolute – as if all stars were same distance from earth Apparent – as they appear in the nighttime sky Variable Stars Some stars show regular variation of brightness over cycles that last from days to years Cepheid Variables – yellow supergiants whose cycles range from 1 to 50 days If a Cepheid is located in another galaxy, astronomers can find the distance to these galaxies by comparing absolute and apparent magnitudes Other stars change in brightness because they revolve around another star. This is known as a ‘binary star system.’ Chapter 28.4 Life Cycles of Stars Hertzsprung-Russel Diagram A diagram to help explain a stars life Most stars fall into 4 distinct groups Main sequence – 90% of stars Our sun Giants – 10-100x bigger than our sun – more luminous Supergiants – more than 100x bigger than our sun White dwarves – stars near the end of their lives Birth of a Star Stars begin their life as a nebula Huge cloud of gas Death of a Star 2 paths Nebula protostar main sequence red giant planetary nebula white dwarf Nebula protostar massive star red supergiant supernova blackhole or neutron star Our sun will swell into a red giant, then its outer layers will get blown away and only an earth-sized fiery hot carbon-oxygen core will remain (white dwarf) Remnants of Massive Stars Massive star goes supernova, the core that is left behind is so massive that the electrons of elements are pulled into the nucleus forming a neutron star. Some neutron stars spin rapidly, burst of radio waves, these are known as pulsars Black hole – so dense that their gravity will not even let light escape Chapter 28.5 Galaxies and the Universe What are galaxies A system of millions of stars that appear as a single star in our sky There is between 50-100 billion galaxies There are millions of light years between galaxies Sun belongs to the Milky Way Galaxy which is a spiral galaxy Milky Way belongs to the Local Group of about 30 galaxies Types of galaxies Spiral – like the Milky Way Elliptical – spherical to lens shaped Irregular – much smaller and fainter with no shape Active Galaxies Galaxies that emit more energy than their combined stars are said to be active Currently it is thought that super massive black holes are at the center of these galaxies