Astronomy 1020 Ch. 5 Study Guide: Light-Matter Interactions & EM Spectrum, Study notes of Astronomy

Download Astronomy 1020 Ch. 5 Study Guide: Light-Matter Interactions & EM Spectrum and more Study notes Astronomy in PDF only on Docsity! Astronomy 1020 Study Guide – Chapter 5(4th Ed.) Chapter 5 page Column Keywords 146 right power – watt right spectrum 147 left red, orange, yellow, green, blue, violet diffraction grating light interacts with matter in four general ways right orange dots emission absorption transmission reflection light may be scattered transparent opaque 148 left experiments performed by Isaac Newton in the 1660s particles right waves – peaks & troughs particle is a thing wave is a pattern wavelength 149 left frequency –> unit = cycle/s = hertz(Hz) wavelength x frequency = speed photon field right electromagnetic wave speed of light in vacuum = 3 x 108 m/s shorter wavelength = higher frequency = higher energy longer wavelength = lower frequency = lower energy 150 left light particles = photons light = particles & waves 151 right visible light electromagnetic radiation electromagnetic spectrum 1 nm = 1 x 10-9 m = 10Å infrared radio waves 152 microwaves ultraviolet X-rays gamma rays 153 right certain types of matter tend to interact more strongly with certain types of light Democritus 154 left atoms element atomic structure electrons, protons, neutrons nucleus electrical charge atomic number 155 left atomic mass number isotopes molecules right compounds phases of matter solid, liquid, gas chemical bond 156 left phase changes in water right sublimation evaporation molecular dissociation 157 left ions ionization plasma pressure right sea level – 14.7 pounds 158 right energy levels in atoms energy levels electron-volts ground state excited state 159 left energy level transitions quantum physics – quantum mechanics right spectroscopy intensity 160 left continuous spectrum emission line spectrum absorption line spectrum energy levels of electrons in each chemical element unique – spectral fingerprint more electrons = more complicated spectrum 162 left absorption line spectra absorption at location of emission line right chemical fingerprint ions of elements produce different spectra 163 left molecular bands 164 left average kinetic energy characterizes temperature thermal radiation thermal radiation spectrum right two simple rules describe the spectrum of a thermally emitting object 165 reflected light spectrum 166 left Doppler effect Doppler effect causes shift in wavelength of light 167 left moving towards us -> shorter wavelength moving away from us -> longer wavelength