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Exploring Our Solar System and Its Origin Chapter 4: Exploring Our Evolving Solar System SN solar system..\..\..\a stronomy\anim ations\starry night files\solar system.snf The planets are tiny compared to the distances between them (a million times smaller than shown here), but they exhibit clear patterns of composition and motion. The patterns are far more important and interesting than numbers, names, and other trivia Sun • Over 99.9% of solar system’s mass • Made mostly of H/He gas (plasma) • Converts 4 million tons of mass into energy each second Mercury • made of metal and rock; large iron core • desolate, cratered; long, tall, steep cliffs • very hot and very cold: 425°C (day), –170°C (night) Venus • nearly identical in size to Earth; surface hidden by thick clouds • hellish conditions due to an extreme greenhouse effect: • even hotter than Mercury: 470°C, both day and night • atmospheric pressure equiv. to pressure 1 km deep in oceans • no oxygen, no water, … • perhaps more than any other planet, makes us ask: how did it end up so different from Earth? Earth and Moon to scale Earth and Moon to scale Earth • An oasis of life • The only surface liquid water in the solar system; about 3/4 of surface covered by water • A surprisingly large moon Mars • Looks almost Earth-like, but don’t go without a spacesuit! • Giant volcanoes, a huge canyon, polar caps, more… • Water flowed in the distant past; could there have been life? Jupiter • Much farther from Sun than inner 4 planets (more than twice Mars distance) • Also very different in composition: mostly H/He; no solid surface. • Gigantic for a planet: 300 Earth mass; >1,000 Earth volume. • Many moons, rings… Great Red Spot SATURN Giant and gaseous like Jupiter • most spectacular rings of the 4 jovian planets • many moons, including cloudcovered Titan • currently under study by the Cassini spacecraft Uranus • much smaller than Jupiter or Saturn, but still much larger than Earth • made of H/He gas, and hydrogen compounds (H2O, NH3, CH4) • extreme axis tilt — nearly tipped on its “side” — makes extreme seasons during its 84-year orbit. • moons also tipped in their orbits… Neptune • Very similar to Uranus (but much smaller axis tilt) • Many moons, including unusual Triton: orbits “backward”; and is larger than Pluto. Wispy white clouds are thought to be crystals of methane. Pluto • A “misfit” among the planets: far from Sun like large jovian planets, but much smaller than any terrestrial planet. • Comet-like composition (ices, rock) and orbit (eccentric, inclined to ecliptic plane, long -- 248 years). • Its moon Charon is half Pluto’s size in diameter • Best current photo above; New Horizons mission launch Jan 2006, arrival at Pluto in 2015… Asteroids *100,000+ rocky objects within the orbit of Jupiter *Also called minor planets *The largest, Ceres, has a diameter of about 900 km or ~ (560 mi) *Orbit the Sun in the same direction as the planets *Most orbit the Sun at distances of 2 to 3.5 AU, in the asteroid belt TNOs - Trans-Neptunian Objects *1,000+ small bodies orbiting beyond the orbit of Neptune *The largest of these are known as dwarf planets *Include Pluto, Eris, Charon, Makemake, etc. *Orbit the Sun in the same direction as the planets *Most orbit within the Kuiper belt at 30 AU to 50 AU Comets •Objects that result when Kuiper belt objects collide •Fragments a few kilometers across, diverted into new and elongated orbits •The Sun’s radiation vaporizes ices, producing tails of gas and dust particles •Astronomers deduce composition by studying the spectra of these tails created by reflected sunlight •Oort cloud comets orbit out to 50,000 AU Clues to the Formation of Our Solar System Our Goals for Learning • What features of our solar system provide clues to how it formed? • What theory best explains the features of our solar system? Common Properties of Planet Orbits in Our Solar System As viewed from above, all of the planets orbit the Sun in a counter-clockwise direction. The planets orbit in nearly the same plane. All planets except Pluto have an orbital inclination of less than 7°. Terrestrial Smaller Mass and size Jovians Larger mass and size higher density low density made of rock and metal mostly H, He, & hydrocarbon compounds Have solid surfaces few moons no rings Closer to Sun and closer together No solid surface many moons rings Farther from sun and farther apart Rocky asteroids between Mars & Jupiter Icy comets in vicinity of Neptune and beyond Asteroids and comets far outnumber the planets and their moons A successful theory of solar system formation must allow for exceptions to general rules Summary: Four Major Features of our Solar System Classifying the Planets The planets (except Pluto) fit into two groups: The Terrestrials or Inner Planets: The Jovians or Outer Planets: Mercury Jupiter Venus Saturn Earth Uranus Mars Neptune 10 Size, Mass, and Density The Jovian planets have much bigger diameters and even larger masses than the terrestrial planets. Though less massive than the Jovians, Terrestrial planets are much more dense. Again, with the exception of ODD BALL Pluto, the rotation rates of Jovian planets on their axes are much faster than the Terrestrial planets. Despite these fast rotation rates, the diameters of the Jovian planets are tremendously larger than those of the Terrestrial Planets. What theory best explains the features of our solar system? According to the nebular theory our solar system formed from a giant cloud of interstellar gas (nebula = cloud) The lightest and simplest elements, hydrogen and helium, are abundant in the universe. Heavier elements, such as iron and silicon, are created by thermonuclear reactions in the interiors of stars, and then ejected into space by those stars. Ejection of Matter from Stars LARGE STAR NEAR THE END OF ITS LIFE FORMATION OF PLANETARY NEBULA SUPERNOVA EXPLOSIONS Great clouds of gas and dust ejected from old stars are gathered into regions from which new stars can be made. This region in the constellation of Orion shows new stars still surrounded by the nebula from which they were formed. Summary of the Nebular Model for formation of the solar system. Other Star Systems Forming We can look at young star systems developing today. The planets orbiting these stars are formed from the surrounding disks of gas and dust, called protoplanetary disks or proplyds. PLANET FORMATION Within the disk that surrounds the protosun, solid grains collide and clump together into planetesimals. The terrestrial planets are built up by collisions and the accretion of planetesimals by gravitational attraction. The Jovian-like planets are formed by gas accretion. Common Properties of Planet Orbits in Our Solar System As viewed from above, all of the planets orbit the Sun in a counter-clockwise direction. The planets orbit in nearly the same plane. All planets except Pluto have an orbital inclination of less than 7°. Why are there two types of planets? 1. Outer planets get bigger because abundant hydrogen compounds condense to form ICES. 2. Outer planets accrete and keep H & He gas because they’re bigger. 3. Inner planets too hot, gases evaporate Fig 9.5 Inside the frost line: too hot for hydrogen compounds to form ices. Outside the frost line: cold enough for ices to form. Inner parts of disk are hotter than outer parts. Rock can be solid at much higher temperatures than ice. Four Unexplained Features of our Solar System √ Why do large bodies in our solar system have orderly motions? √ Why are there two types of planets? --> 3) Where did the comets and asteroids come from? 4) How can we explain the exceptions the the ‘rules’ above? Comets and asteroids are leftover planetesimals. • Asteroids are rocky because they formed inside the frostline. • Comets are icy because they formed outside the frostline Four Unexplained Features of our Solar System √ Why do large bodies in our solar system have orderly motions? √ Why are there two types of planets? √ Where did the comets and asteroids come from? How do we explain the existence of our Moon and other “exceptions to the rules”? --> 4) Earth’s moon was probably created when a big planetesimal slammed into the newly forming Earth Remember! Early in history of solar system, such impacts far more common Other large impacts may be responsible for other exceptions like rotation of Venus and Uranus Review of nebular theory Fig 6.27 Four Features of our Solar System Explained √ Why do large bodies in our solar system have orderly motions? √ Why are there two types of planets? √ Where did the comets and asteroids come from? √ How do we explain the existence of our Moon and other “exceptions to the rules”? When did the planets form? We cannot find the age of a planet, but we can find the ages of the rocks that make it up We can determine the age of a rock through careful analysis of the proportions of various atoms and isotopes within it The decay of radioactive elements into other elements is a key tool in finding the ages of rocks Age dating of meteorites that are unchanged since they condensed and accreted tell us that the solar system is about 4.6 billion years old. Since 2008, the oldest rock on earth has been discovered by McGill University in the Nuvvuagittuq greenstone belt on the coast of Hudson Bay, in northern Quebec, and is dated from 3.8 to 4.28 billion years old, based on isotopes of neodymium and samarium Other Planetary Systems Our Goals for Learning • How do we detect planets around other stars? • What have other planetary systems taught us about our own? Most common Extrasolar planets are usually too dim or too close to the stars they orbit to observe directly, however Kepler craft can see many transient events. However, we can detect the effect they have on the spectra from their star to confirm their existence. newest Kepler mission The gravitational fields of a star and its planet will cause passing light to change direction. The focusing of light by gravity is called microlensing. We detect planets around other stars by looking for a periodic motion of the stars they orbit. We measure the motion through the Doppler shift of the star’s spectrum –very small shifts ~ 0.000044 nm The size of the wobble tells us the planet’s mass Earth mass .00314 The period of the wobble tells us the radius of its orbit (Kepler’s 3rd law) We can also detect planets if they eclipse their star Fraction of starlight blocked tells us planet’s size These are only a few of the many ways in which our planet is special and perhaps unique 1. Orbits in habitable zone (liquid water exists) 2. Has a large, fairly close moon 3. Orbits right type star @ right time 4. Solar system is in right region of the galaxy 5. Planet is right size, not too big or too small 6. Has plate tectonics 7. Solar system has a Jupiter size planet, not too close 8. Stable, nearly circular orbits 9. Etc . . . We do know there are currently 1056 extrasolar planets found in 802 planetary systems as of Jan.10,2014. Source : www.exoplanet.eu 539 planets in 405 systems by astrometry/radial velocity 430 planets in 327 systems by transiting planets 26 planets in 24 systems by microlensing 46 planets in 42 systems by imaging 15 planets in 12 systems by timing (pulsar planets) Let’s see how many of these are even remotely earthlike. We will observe first of all that the Earth’s orbit and mass are quite unusual 16 planets out of 1056 with masses within 100% of the Earth Stars with low metallicity (elements > He) are unlikely to have rocky planets. In plot below The sun is the reference @ 0 Earth’s Mass (.00314 MJ) Earth’s orbit 16 planets out of 1056 with masses within 100% of the Earth The majority of extrasolar planets orbit inside Earth’s orbit, very close to their host star. All known extrasolar planets with masses from 0 to 0.01 Mjup Earth Earth Mass Earth All known extrasolar planets with orbits between 0.8 AU and 1.2 Au and masses between Earth (.00314 MJ ) and at least 100 Earth masses (.314 MJ ). Mass Radius a (MEarth) (REarth) (AU) Planet △ PSR 1257 12 b 0.022248 — 0.19 — KOI-1843 b 0.31783 0.582867 Kepler-70 c 0.667443 0.8743 KOI-2700 b 0.86 1.06 Kepler-42 d 0.95349 0.571658 alf Cen B b 1.144188 Kepler-307 c 1.207754 2.802245 1.69 1.2 Kepler-177 b 1.700391 2.903126 — Kepler-88 b 1.756456 4.219845 — Kepler-11 b 1.9 1.8 0.091 Kepler-42 c 1.90698 0.728584 0.006 Kepler-78 b Gl 581 e 1.938763 0.0076 — 0.0154 — 0.04 — 0.01 — 3 2.05 0.15 Kepler-20 e 3.082951 0.8743 0.0507 HD 215152 c 3.082951 — 0.0852 3.1783 — 0.66 HD 40307 e 3.49613 — 0.1886 HD 85512 b 3.49613 — 0.26 HD 39194 b 3.718611 — 0.0519 3.81396 — 0.46 MOA-2007-BLG192-L b KOI-82 d KOI-115 d 2 1.91 0.077 Kepler-65 d 2 1.513212 0.084 Kepler-11 f 2 2.49 0.25 HD 20794 c 2.415508 0.2036 Kepler-307 b 2.510857 HD 20794 b 2.701555 — 0.1207 GJ 667C f 2.701555 — 0.156 GJ 667C e 2.701555 — 0.213 HD 215152 b 2.765121 — 0.0652 3.205768 KOI-111 c PSR 1257 12 d 0.028 — 50 lightest planets known — Kepler-42 b 2.86047 0.784629 0.0116 Kepler-11 c 2.9 2.87 0.106 KOI-117 b 3 1.58 0.045 KOI-82 c 3 1.34 0.086 4 0.69 — 0.067 HD 40307 b 4.004658 0.0468 Kepler-62 c 4.004658 0.538031 0.0929 Kepler-79 e 4.100007 3.497202 0.386 4.13179 — 0.36 HD 156668 b 4.163573 — 0.05 GJ 667C c 4.258922 — 0.1251 Kepler-70 b 4.44962 GJ 676A d 4.44962 PSR 1257 12 c 0.762211 — 0.006 0.0413 Kepler-36 b 4.46 1.48 0.1153 Kepler-10 b 4.6 1.46 0.01687 — GJ 667C g 4.608535 Kepler-68 c 4.76745 HD 20794 d 4.76745 Kepler-114 d 4.799233 2.533229 0.09 5 4.819861 0.066 KOI-115 C 0.549 0.907927 — 0.09059 0.3499 50 planets with lowest masses from 0.86 to 5 ME How many of these have a mass between 0.1ME and 10ME ? Exactly 29 planets Of these 29 planets how many have an orbit radius between 0.8 to 1.2 AU ? 0 3 lightest planets in ME PSR 1257 12 b, 0.0225 Orbits at 0.19 AU KOI-1843 b 0.3178 orbits at ?? AU Kepler-70 c 0.6674 orbits at .0076 AU 4 planets closest to ME KOI-2700 b, 0.86ME at ??? Kepler-42 d, 0.953 at 0.015 AU alf Cen B b, 1.144 at 0.04 AU Kepler-307 c, 2.80 at ?? www.exoplanet.eu Typical Extrasolar system compared with our solar system Solar system masses in terms of Jupiter mass I would weigh more than 900 pounds 6 x ME Mercury a = .00017 Venus b = .00256 Earth c = .00315 Mars d = .00034 Jupiter e = 1.0 Our solar system a b c d e Based on the 1056 known extrasolar planets as of Jan. 2014, what can we conclude? First, most are more massive than Jupiter and closer to their star than Earth is to Sun. Our solar system is unusual. Revisions to the nebular theory are necessary! Planets can apparently migrate inward from their birthplaces. Highly eccentric orbits are the norm Secondly, the sun is not an average star, it ranks in the top 10% of all stars in size. The average star is a small, very cool M class star. The sun also has a high metal content. Stars with low metal content will not have rocky planets. The sun is also unusually stable for a main sequence star, whose luminosity (brightness) has increased only a few % over the last 2 billion years, providing a very long term stable environment for life to flourish and develop Survey of stars in the solar neighborhood heavier Very few have masses greater than the sun Mass weighted avg. of the 319 stars is 0.45 M/Mo most common stars are 0.1 to 0.2 M/M0` Our Sun lighter Is Earth Unusual? • No Earth-like planets found yet. • Data aren’t good enough to tell if they are common or rare • Kepler mission has provided more data on Earth size planets. • Earth probably IS unusual conclusion Based on the multiple lines of evidence from a variety of scientific areas ( and I have only presented a very small sample of a large body of evidence) what is one to conclude ? Based on almost any reasonable criteria that one could devise, the existence of intelligent life on Earth and perhaps in the Universe as well is an ENIGMA.... without GOD