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Universe: Past, Present & Future

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Universe: Past, Present & Future Northeastern Illinois University Universe: Past, Present & Future Review Greg Anderson Department of Physics & Astronomy Northeastern Illinois University Spring 2018 c 2012-2018G. Anderson Universe: Past, Present & Future – slide 1 / 92 Northeastern Illinois Overview University The Basics Solar System The Sun Stars Galaxies & Cosmology c 2012-2018G. Anderson Universe: Past, Present & Future – slide 2 / 92 Northeastern Illinois Our motion in the Universe University c 2012-2018G. Anderson Universe: Past, Present & Future – slide 4 / 92 Northeastern Illinois University Cosmic Address Our motion in the Universe The Basics Light-Year Light Distance Scales Time-Scales Cosmic Calendar Year Constellations The Basics Angles Solstice, Equinox & Seasons Peri & Apogee Fig: Phases Umbra, Penumbra & Antumbra Lunar Eclipses Solar Eclipses Greek Geocentric Cosmology Copernicus Kepler’s Laws Planet Speeds Galileo Galileo II Newton’s Laws Q: c Free2012-2018G. fall Anderson Universe: Past, Present & Future – slide 5 / 92 Newton’s Law of Northeastern Illinois Light-Year University A light-year is the distance light travels in a year. The speed of light is: c 3 108 meters/second = 300, 000km/s ≈ × In one year, light travels a distance: 1ly = 3 105 km (1year) 365 days 24 hours 3600 seconds × second 1year 1day 1hour = 9, 460, 000, 000, 000km = 9.46 1012 km × The farther away we look in the distance, the farther back we look in time. c 2012-2018G. Anderson Universe: Past, Present & Future – slide 6 / 92 Northeastern Illinois Measuring Distances with Light University Earth-Moon distance 1.3 light-seconds Earth-Sun distance 8.3 light-minutes Pluto semi-major axis 5.5 light-hours Oort Cloud-Sun distance 41-82 light-weeks Alpha Centauri System 4.2 light-years Milky Way diameter 100,000 years Andromeda distance 2.5M years c 2012-2018G. Anderson Universe: Past, Present & Future – slide 7 / 92 Northeastern Illinois Astronomical Distances University Earth’s Orbit (1 Astronomical Unit) 1AU=1.496 108 km × Distance Light Travels in 1 year 1light-year = 9.46 1012 km × Parsec 1parsec (pc) = 3.09 1013 km 3.26 light-years × ≈ Galactic Diameter: 30 100 kpc − 1kiloparsec (kpc) = 1000pc 3.26 103 light-years ≈ × Distance between Galaxies 1megaparsec (Mpc) = 106 pc 3.26 106 light-years ≈ × c 2012-2018G. Anderson Universe: Past, Present & Future – slide 8 / 92 Northeastern Illinois Cosmological Time-Scales University The Earth t =4.54 0.05 billion years ± Our Sun t =4.57 billion years Oldest Stars t = 12.5 1.5 billion years ± The Universe t = 13.6 1.5 billion years c 2012-2018G. Anderson ± Universe: Past, Present & Future – slide 9 / 92 Northeastern Illinois Cosmic Calendar Year University Jan 1: The Big Bang • February: Milky Way forms • Sept 3: Earth forms • Sep 22: Early life on earth • Dec 17: Cambrian Explosion • Dec 26: Rise of Dinosaurs • Dec 31 (9pm): Early hominids • Dec 31 (11:58pm): Modern humans • Dec 31 (11:59:49pm): Pyramids • Dec 31 (11:59:59pm): We learn Earth is a planet orbiting the Sun. • c 2012-2018G. Anderson Universe: Past, Present & Future – slide 10 / 92 Northeastern Illinois Constellations University On a clear night, in a dark place (not Chicago) you • can see a few thousand stars in the night sky. People from nearly every culture gave names to • patterns of stars in the sky. Our familiar constellations originated in Mesopotamia • over 5000 years ago. In 1928, the International Astronomical Union (IAU) • established 88 official constellations with well defined boundaries. c 2012-2018G. Anderson Universe: Past, Present & Future – slide 11 / 92 Northeastern Illinois Degrees, Arcminutes, Arcseconds University Degrees and Radians 360◦ =2π radians 2π 1 1◦ = radians radians 360 ≈ 60 Sixty arcminutes per degree: 1◦ = 60′ C =2πr Sixty arcseconds per arcminute: 1′ = 60′′ c 2012-2018G. Anderson Universe: Past, Present & Future – slide 12 / 92 Northeastern Illinois Solstice, Equinox & Seasons University summer atumn atumnal equinox winter summer solstice solstice vernal equinox winter spring Solstice: Either of two times a the year when the sun is at its • greatest distance from the celestial equator. Equinox: Two times a year when: the sun crosses the celestial • equator, length of day = length of night, tilt of the Earth’s axis is inclined neither away from nor towards the Sun. c 2012-2018G. Anderson Universe: Past, Present & Future – slide 13 / 92 Northeastern Illinois Moon at Perigee & Apogee University c 2012-2018G. Anderson Universe: Past, Present & Future – slide 14 / 92 Northeastern Illinois Fig: Moon Phases University c 2012-2018G. Anderson Universe: Past, Present & Future – slide 15 / 92 Northeastern Illinois Umbra, Penumbra & Antumbra University antumbra umbra penumbra Looking towards the Sun from the... Umbra Penumbra Antumbra Total Eclipse Partial Eclipse Annular Eclipse c 2012-2018G. Anderson Universe: Past, Present & Future – slide 16 / 92 Northeastern Illinois Lunar Eclipses University c 2012-2018G. Anderson Universe: Past, Present & Future – slide 17 / 92 Northeastern Illinois Solar Eclipses University c 2012-2018G. Anderson Universe: Past, Present & Future – slide 18 / 92 Northeastern Illinois Greek Geocentric Cosmology University ⋆ Stars Saturn Y X Jupiter Mars ♂ ☼ Sun Venus ♀ ' Mercury Moon $ ♁ Earth Aristotle’s crystalline spheres c 2012-2018G. Anderson Universe: Past, Present & Future – slide 19 / 92 Northeastern Illinois Nicolaus Copernicus (1473 - 1543) University Polish astronomer, Nicolaus Copernicus (1473 - 1543) published De Revolutionnibus Orbium Coelestium: a detailed Heliocentric Model of the universe just before his death in 1543 (See also: Aristarchus, 310-230 BC). ♂ ♁ Heliocentric Model 73 years would pass before De Revolutionibus was listed as a forbidden work by the Church. c 2012-2018G. Anderson Universe: Past, Present & Future – slide 20 / 92 Northeastern Illinois Kepler’s Laws University Based on the meticulous observations of Tycho de Brahe (1546-1601), Kepler formulated the three laws which bear his name: Law of Ellipses (1609) • The orbit of every planet is an ellipse which the Sun located at one focus. Law of Equal Areas (1609) • a A line connecting the Sun and a planet 2 sweeps out equal areas in equal times. Harmonic Law (1618) • p2 = a3 c 2012-2018G. Anderson Universe: Past, Present & Future – slide 21 / 92 Northeastern Illinois Orbital Speeds of Planets University 12 vp =2πr v =2π r =2π r ⇒ p r3/2 10 bc Mercury 8 bc Venus bc 2π GM 6 v = = ⊙ bc √r q r Mars (AU/years) v 4 Jupiterbc Saturn bc Uranus 2 bc Neptunebc 0 0 10r (AU) 20 30 c 2012-2018G. Anderson Universe: Past, Present & Future – slide 22 / 92 Northeastern Illinois Galileo Galilei (1564-1642) University Made substantial contributions to the scientific method by the use of mathematics and experiment. Argued for the Heliocentric Copernican model. Devised experiments and observations which refuted Aristotle and • Plato: Moving objects remain in motion unless acted on by a force. 1610 built a telescope, and discovered: • 1. four moons of Jupiter 2. phases of Venus 3. Sun spots 4. Craters and mountains on the Moon Argued stars are too disant for observable parallax • c 2012-2018G. Anderson Universe: Past, Present & Future – slide 23 / 92 Northeastern Illinois Galileo Galilei (II) University 1623: Dialogue Concerning the Two Chief World Systems compared the Copernican and Ptolemaic systems. Ordered to stand trial by the Catholic church in 1633, found “vehemently suspect of heresy”, forced to recant by the Inquisition, and was placed in house arrest for the rest of his life. c 2012-2018G. Anderson Universe: Past, Present & Future – slide 24 / 92 Northeastern Illinois Newton’s Laws of Motion University From Newton’s Principia 1687: I. An object moves at a constant velocity if no net force is acting. II. Force equals mass times acceleration. F = ma III. For every force, there is an equal and opposite reaction force. Fa b = Fb a on − on c 2012-2018G. Anderson Universe: Past, Present & Future – slide 25 / 92 Northeastern Illinois Why are astronauts weightless in space? University c 2012-2018G. Anderson Universe: Past, Present & Future – slide 26 / 92 Northeastern Illinois Newton’s Law of Gravitation University Newton’s Law of Universal Gravitation (1687). M2 Gravitational force: F M1M2 F = G 2 d d Universal Gravitational constant: F 11 2 2 M1 G =6.67 10− Nm kg− × m , m : masses of two bodies in kilograms (kg). • 1 2 d: distance between m and m in meters (m). • 1 2 F force between bodies in Newtons (N). • c 2012-2018G. Anderson Universe: Past, Present & Future – slide 27 / 92 Northeastern Illinois Tides and the Moon University Mm F = G r2 Moon’s gravitational attraction: weaker Low Tide High High Tide Tide Low Tide Moon’s gravitational attraction: stronger Tidal bulges toward and away from Moon • High tide occurs 50 min later each day. • c 2012-2018G. Anderson Universe: Past, Present & Future – slide 28 / 92 Northeastern Illinois Spring and Neap Tides University Spring Tides to Sun New Moon Full Moon c 2012-2018G. Anderson Universe: Past, Present & Future – slide 29 / 92 Northeastern Illinois Spring and Neap Tides University Third Quarter Neap Tides to Sun First Quarter c 2012-2018G. Anderson Universe: Past, Present & Future – slide 29 / 92 Northeastern Illinois Electromagnetic Spectrum University Region Wavelength Frequency(Hz) Radio m – 10 cm 0 – 3 109 ∞ × Microwave 10 cm – 0.1 mm 3.0 109 – 3 1012 × × Infrared 0.1 mm – 0.7 µm 3.0 1012 – 4.3 1014 × × Visible 700 nm – 400 nm 4.3 1014 – 7.5 1014 × × Ultraviolet 400 nm – 1 nm 7.5 1014 – 3 1017 × × X-Rays 1 nm – 10−2 nm 3 1017 – 3 1019 × × Gamma-Rays 0 – 10−2 nm – 3 1019 ∞ × 1 10−1 10−2 10−3 10−4 10−5 10−6 10−7 10−8 10−9 10−10 10−11 m λ Radio micro-waves IR UV X-rays γ-rays Hz f 108 109 1010 1011 1012 1013 1014 1015 1016 1017 1018 1019 1020 c 2012-2018G.
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