Science 3210 001 : Introduction to Astronomy Lecture 3 : Overview of the Solar System, The Sun, and the Inner Planets Robert Fisher Items ❑ Solution sets 1 and 2 have been posted, as well as homework assignment number 4, due next week (2/23) ❑ Syllabus typo -- Spring break is the third week of March, not February. Everything moves up a week, so first midterm is in two weeks time. ❑ Homeworks Review Week 2 ❑ Celestial Sphere ❑ Zenith, Nadir, Meridian, Equinox, Solstice ❑ Retrograde Motion Review Week 3 ❑ Kepler’s Three Laws ❑ Newton’s Three Laws ❑ Spectra -- Continuum, Absorption, Emission Today’s Material ❑ A Few Comments about the Primary Colors and Color Photography ❑ Overview of the Solar System ❑ Planets, Moons, Rings, Asteroids, Comets… ❑ Fundamentals of Planetary Physics ❑ The Inner Solar System ❑ The Cratered Worlds of Mercury and the Moon ❑ Venus and Mars ❑ Earth A Few Comments About Color Theory and Color Photography The Primary Colors ❑ There are three primary colors precisely because the human eye has three types of cone photoreceptor cells, each sensitive to one band of light. Cone Cell Color Response ❑ Each of the the three types of cone cells has a different biochemical makeup with a different color response curve : Solar Spectrum ❑ The reason why our rod cells have a peak absorption at roughly 500 nm in wavelength is simply because the solar spectrum peaks at that same wavelength : First Color Photograph ❑ James Clerk Maxwell produced the first color photograph in 1861 using three images photographed on black and white positive films, filtered through each of the primary colors : Overview of the Solar System Overview of Solar System ❑ The Sun. In a sense, the sun is the solar system. 99.9% of the total mass of the solar system, and also the source of the vast majority of energy. Sun Compared with Planets ❑ A 3D computer rendering of the sun and the planets, all compared to-scale : Overview of Solar System ❑ The Planets ❑ Inner planets are close to the sun -- consisting of relatively warm rocky bodies, and thin to non-existent atmospheres. ❑ Outer planets are further from the sun -- they have rocky cores and enormous gaseous atmospheres which constitute the bulk of the planet. Comparison of Inner Planets ❑ A 3D computer rendering of the inner planets and the moon, all compared to-scale : Comparison of Outer Planets ❑ A 3D computer rendering of the outer planets, compared with the inner planets, all to-scale : Question ❑ Which planet can never be seen on the Meridian at midnight? ❑ A) Mercury ❑ B) Mars ❑ C) Jupiter ❑ D) Saturn Overview of Solar System ❑ Moons / Rings A moon is simply a natural satellite of a planet. There are over 100 known moons -- most around Jupiter and the outer planets. The largest moon in the solar system (Jupiter’s Ganymede, discovered by Galileo) is larger than Mercury. If it were orbiting the sun, it would be classified as a planet. Some of the largest moons (most noteably Saturn’s Titan) have atmospheres. Others show signs of active geological activity, including one (Jupiter’s Io) that shows direct signs of volcanic activity. Ganymede ❑ Ganymede, as photographed by the Galileo space probe. A Theoretical Model of Interior of Ganymede Io ❑ Jupiter’s moon Io is volcanically active, spewing sulfur plumes. Overview of Solar System - Rings ❑ All four of the outer solar system planets have ring systems, though Saturn’s is by far the most spectacular. ❑ These rings are the remnant material left over from the formation of the moons surrounding the planet, and are made up of enormous numbers of icy rocks. ❑ In a sense, the moon/planet systems are a kind of “mini solar system,” and the rings are analogous to a scaled-down version of the asteroid belts in our own solar system (which we will discuss in just a moment). Artist’s Conception of Saturn’s RIngs Saturn Imaged by the Cassini Spacecraft Saturn’s Rings Imaged by Voyager Overview of Solar System - Minor Bodies ❑ Dwarf Planets - a very new category. ❑ According to the new International Astronomical Union (IAU) specification laid down last year, planets are officially defined to meet three criteria : ❑ Major bodies orbiting the sun (or another star). ❑ Large enough to be spherical in shape. ❑ Have swept their neighborhood clear. ❑ Dwarf planets satisfy the first two criteria, but fail the third. Examples include Pluto and the asteroid Ceres. Disk Clearing / Gap Formation ❑ A large enough body will sweep up the material its neighborhood. Here, for instance, is the result of a simulation of the early solar system, before it had been cleared of gas and dust : Star Gap Planet Disk (in greyscale) Overview of Solar System - Minor Bodies ❑ Asteroids ❑ The asteroids were once thought to have been a “broken-up” planet, but they actually contain far too little mass to constitute a planet. They are the left-over products of planet formation. ❑ They range in size from the spherically-shaped Ceres (almost 1000 km in radius) down to much smaller bodies barely a few kilometers across. The Asteroid Belt - Minor Bodies ❑ Most asteroids are clustered between the orbits of Mars and Jupiter. It is thought that Jupiter’s enormous gravitational force kept these bodies from coalescing into a rocky planetary core. Vesta, Ceres, and the Moon ❑ Side-by-side comparison of two of the largest asteroids (Vesta and Ceres) and the Earth’s moon : Question ❑ Why are the larger bodies in previous image rounder than the smaller ones? The Asteroid Eros ❑ Eros was visited by the spaceprobe NEAR Shoemaker, which began its orbit around the asteroid on February 14, 2000. Eugene Shoemaker (1928 - 1997) Barringer (or Meteor) Crater in Arizona ❑ Shoemaker’s great legacy was to establish that catastrophic impacts do occur throughout the solar system. Overview of Solar System - Minor Bodies ❑ In addition to the asteroid belt, another belt of bodies orbits the sun beyond the orbit of Neptune -- the Kuiper Belt. ❑ It is thought that Pluto is in fact a Kuiper belt object -- one of the largest. ❑ Because of their great distance from the sun, Kuiper Belt Objects are much harder to detect than asteroids. 800 objects have been detected to date. Kuiper Belt Objects ❑ Like the case of the asteroid belt, the Kuiper Belt is “debris” left over from the early solar system. In this case, they have been missed by Neptune’s “sweeping” of its neighborhood. Overview of Solar System - Meteoroids, Dust, and the Solar Wind ❑ Meteoroids, Dust, Solar Wind ❑ The trail of comets is filled with tiny meteoroids. When the Earth’s orbit intersects a comet’s trajectory, we experience a meteoroid shower on Earth. These happen at regular dates on the calendar each year. ❑ The collision of rocky bodies over the course of history of the solar system produces smaller bodies, down to dust-sized particles. These dust-like particles are responsible for the zodiacal light effect. ❑ The outer layers of the sun continuously blow away a stream of charged particles, referred to as the solar wind. Magnetic Field ❑ The magnetic field surrounding a magnet can be visualized using iron filings. Solar Atmosphere ❑ The outer layers of the sun are incredibly active, powered by the Sun’s intense magnetic field. TRACE Satellite Image Fundamentals of Planetary Physics ❑ The properties of the planets are largely determined by a few crucial physical parameters -- its mass, rotational rate/inclination, and surface temperature. ❑ The combination of mass and surface temperature, for instance, will determine the atmospheric content of the planet. ❑ Larger bodies tend to be more geologically active than smaller bodies. ❑ More rapidly rotating bodies tend to have stronger magnetic fields. Planetary Magnetic Fields ❑ The interior of the planets contains electrically conducting iron and nickel, which flow like fluids over very long timescales. ❑ Planetary rotation sets these fluids in motion and generates currents, which in turn generate magnetic fields surrounding the planet. Earth’s Magnetic Field ❑ Earth has the strongest magnetic field of the inner planets in the solar system. ❑ This is believed to be important in protecting life on Earth from harmful charged particles from the Sun and elsewhere. Earth’s Aurora Charged particles from the solar wind become trapped in the Earth’s magnetic field and stream down to the poles, generating the phenomenon we see on earth as the Aurora. Why are Some Moons and Planets Geologically Active and Others Dormant? ❑ Geological activity requires a source of energy. ❑ That source of energy is the heat interior to a body. ❑ The amount of heat energy contained in a body is proportional to its volume. ❑ The rate at which heat energy is lost is proportional to its surface area. ❑ Consequently, smaller bodies cool more rapidly than larger ones. As a result, smaller bodies tend to be less geologically active. Examples of Planetary / Lunar Interiors Atmospheric Physics ❑ In a gas in thermal equilibrium each molecule shares the same kinetic energy. This means that lighter molecules must be moving faster on average to have the same kinetic energy as heavier molecules. O2 H2 Does Gravity or Heat Win? ❑ Gravity exerts an inward pull on atmospheric molecules. Kinetic energy (in the form of heat) causes them to want to escape. O2 Gravity H2 Atmospheric Physics and the Giant Planets ❑ The fate of a molecule is determined by the planet’s mass and the temperature of the atmosphere -- the larger the mass, the more species it can retain. ❑ What about the most common element, hydrogen, and its molecular counterpart H2? ❑ The Earth, and all inner solar system planets, lack the sufficient mass to retain H2. ❑ The outer solar planets do have sufficient mass to retain H2. ❑ This observation explains how the outer solar system planets grew to become giant planets.