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EART160 Planetary Sciences Logistics • HW 4 due Monday • Mid-term on Wednesday – Mix of qualitative and quantitative problems – Equation “cheat sheet” will be given to you – Covers material on HWs 1-4, and up to slide 7 of Atmospheres lecture. – Study advice: review all lecture slides, HWs, and major in-class derivations. • First draft of paper due soon. Last Week • Planetary mass and radius give us bulk density • Bulk density depends on both composition and size • Larger planets have greater bulk densities because materials get denser at high pressures • The increase in density of a material is controlled by its bulk modulus • Planets start out hot (due to accretion) and cool • Cooling is accomplished (usually) by either conduction or convection • Vigour of convection is controlled by the Rayleigh number, and increases as viscosity decreases • Viscosity is temperature-dependent, so planetary temperatures tend to be self-regulating This Week - Atmospheres • What determines the surface temperature of a planet? • What determines the temperature and pressure structure of planetary atmospheres? • What are the atmospheres made of, and where do they come from? • What determines the wind strengths? • How do planetary atmospheres evolve? Surface Temperature (1) • What determines a planet’s surface temperature? Incident energy Reflected energy Energy re-radiated from warm surface Absorbed energy warms surface rE 2 E r Ein (1 A)R F 2 R Sun Erad 4 R T 2 4 A is albedo, FE is solar flux at Earth’s surface, rE is distance of Earth to Sun, r is distance of planet to Sun, is emissivity, is Stefan’s constant (5.67x10-8 Wm-2K-4) • Balancing energy in and energy out gives: 1/ 4 rE FE (1 A) Teq r 4 2 a Surface Temperature (2) • • • • Solar constant FE=1300 Wm-2 1/ 4 2 rE FE (1 A) Earth (Bond) albedo A=0.29, =0.9 Teq r 4 Equilibrium temperature = 263 K is Stefan’s constant How reasonable is this value? 5.67x10 in SI units -8 Body Mercury Venus Earth Mars A 0.12 0.75 0.29 0.16 Teq 446 238 263 216 Actual T 100-725 733 288 222 • How to explain the discrepancies? • Has the Sun’s energy stayed constant with time? Lunar subsurface temperatures Greenhouse effect • Atmosphere is more or less transparent to radiation (photons) depending on wavelength – opacity • Opacity is low at visible wavelengths, high at infra-red wavelengths due to absorbers like water vapour, CO2 • Incoming light (visible) passes through atmosphere with little absorption • Outgoing light is infra-red (surface temperature is lower) and is absorbed by atmosphere • So atmosphere heats up • Venus suffered from a runaway greenhouse effect – surface temperature got so high that carbonates in the crust dissociated to CO2 . . . Albedo effects • Fraction of energy reflected (not absorbed) by surface is given by the albedo A (0<A<1) • Coal dust has a low albedo, ice a high one • The albedo can have an important effect on surface temperature • E.g. ice caps grow, albedo increases, more heat is reflected, surface temperature drops, ice caps grow further . . . runaway effect! • This mechanism is thought to have led to the Proterozoic Snowball Earth • How did the Snowball disappear? • How did life survive? • How might clouds affect planetary albedo? Atmospheric Structure (1) • Atmosphere is hydrostatic: • Gas law gives us: P RT dP dz ( z) g ( z) • Combining these two (assuming isothermal structure) dP g P( z ) dz RT a Here R is the gas constant, is the mass of one mole, and RT/g is the scale height of the (isothermal) atmosphere (~10 km) which tells you how rapidly pressure increases with depth • Result is that pressure decreases exponentially as a function of height (if the temperature stays constant) Scale Heights • The scale height tells you how far upwards the atmosphere extends • Scale height H = RT/g. Does this make physical sense? • Also, H=P0/(0g) (where’s this from?) • It turns out that most planets have similar scale heights: Venus Earth Mars Jupiter Saturn Uranus Neptune Tsurf (K) 733 288 215 165* 135* 76* 72* Albedo 0.75 0.29 0.16 0.34 0.34 0.29 0.31 H (km) 16 8.5 18 18 35 20 19 * Temperature measured at 1bar pressure Atmospheric Structure (2) • Of course, temperature actually does vary with height • Why does the atmosphere get heated? – Near-surface – High atmosphere heating due to ozone - stratosphere Atmospheric Structure (2) • Of course, temperature actually does vary with height • If a packet of gas rises rapidly (adiabatically), then it will expand and, as a result, cool, and fall again (stable). – If a tiny amount of energy is input initially, it can keep rising. • Work done in expanding = energy lost to cooling VdP= (m/)dP mCpdT m is the mass, is the density of the gas Cp is the specific heat capacity of the gas at constant pressure • Combining these two equations with hydrostatic equilibrium, we get the dry adiabatic lapse rate: g dT a dz Cp • Earth’s lapse rate? What is the temp out side an airplane? • What happens if the air is wet? What about latent heat? Atmospheric Structure (3) • Lower atmosphere (opaque) is dominantly heated from below and will be conductive or convective (adiabatic) • Chemistry can affect temperature structure. • Uppermost atmospheric layer: the thermosphere – temperature increases due to short wavelength solar radiation – little total energy though Lapse rate appx. 1.6 K/km – why? adiabat Stable against convection Chemistry affects temperature Measured Martian temperature profiles Giant planet atmospheric structure • Note position and order of cloud decks Venus Does the Moon have an atmosphere? Ballistic Regime: Exospheres What causes sodium to be released from the surface? Atmosphere Color • Why is the sky blue? Atmosphere Color • Why is the sky blue? • Rayleigh scattering by particles smaller than the wavelength of the incoming light. Atmosphere Color • What color do we predict for Mars? Atmosphere Color • What color do we predict for Mars? • Predict dark blue due to effect of some scattering + blackness of space • In reality, dust dominates. One of the first photos from Viking 1,1976. The Viking photo was overcorrected, the above photo was taken by the rover Spirit. Atmospheric dynamics q is latitude, v particle velocity, w planet rotational velocity North pole • Coriolis effect – objects moving on a rotating planet get deflected (e.g. cyclones) • Why? Angular momentum – as an object moves further away from the pole, r increases, so to conserve angular Deflection to right momentum w decreases in N hemisphere • Coriolis parameter f = 2 w v sin(q) Note the unit vector to the east gets a velocity component to the north. For non-equatorial cases, velocities to the east result in deflections to the south. æ ê ö ç ÷ ç n̂ ÷ ç ÷ è r̂ ø r Rossby number • How important is the Coriolis effect? v Lf Rossby number is a measure of its importance, L is the length scale of interest. • Small Rossby number: system is strongly affected by Coriolis forces e.g. Jupiter v~100 m/s, L~10,000km we get: ~0.03 (important) e.g. Playing catch, v~20 m/s, L = 10 m: ~10,000 (not important) Hadley Cells • Coriolis effect is complicated by fact that parcels of atmosphere rise and fall due to buoyancy and the equator is hotter than the poles. High altitude winds Surface winds • The result is that the atmosphere is broken up into several Hadley cells (see diagram) • How many cells depends on the First look at Rossby number (i.e. rotation rate) side view Slow rotator e.g. Venus Medium rotator e.g. Earth Ro~0.02 (assumes v=100 m/s) Ro~4 Fast rotator e.g. Jupiter Ro~30 On Earth Surface flows converge. Zonal Winds • The reason Jupiter, Saturn, Uranus and Neptune have bands is because of rapid rotations (periods ~ 10 hrs) • The winds in each band can be measured by following individual objects (e.g. clouds) • Winds alternate between prograde (eastwards) and retrograde (westwards) Geostrophic balance • In some situations, the only significant forces acting are due to the Coriolis effect and due to pressure gradients 1 P • The acceleration due to pressure gradients is x • The Coriolis acceleration is 2 w v sinq Why? (Which direction?) 1 P • In steady-state these balance, giving: v 2 w sin q x High High wind Does this make sense? Coriolis pressure Low isobars • The result is that winds flow along isobars and will form cyclones or anti-cyclones Where do planetary atmospheres come from? • Three primary sources – Primordial (solar nebula) – Outgassing (trapped gases) – Later delivery (mostly comets) • How can we distinguish these? – Solar nebula composition well known – Noble gases are useful because they don’t react – Isotopic ratios are useful because they may indicate gas loss or source regions (e.g. D/H) – 40Ar (40K decay product) is a tracer of outgassing Atmospheric Compositions Earth Venus Mars Pressure 1 bar 92 bar 0.006 bar Titan 1.5 bar N2 O2 H2O Ar CO2 CH4 40Ar H/D 14N/15N 77% 21% 1% 0.93% 0.035% 1.7ppm 6.6x1016 kg 3000 272 3.5% 0.01% 0.007% 96% 1.4x1016 kg 63 273 2.7% 0.006% 1.6% 95% ? 4.5x1014 kg 1100 170 98.4% 0.004% ~1ppb 1.6% 3.5x1014 kg 3600 183 Isotopes are useful for inferring outgassing and atmos. loss Not primordial! • Terrestrial planet atmospheres are not primordial (How do we know?) • Why not? – Gas loss (due to impacts, rock reactions or Jeans escape) – Chemical processing (e.g. photolysis, rock reactions) – Later additions (e.g. comets, asteroids) • Giant planet atmospheres are close to primordial: Solar Jupiter Saturn Uranus Neptune H2 84 86.4 97 83 79 He 16 13.6 3 15 18 CH4 0.07 0.2 0.2 2 3 Values are by number of molecules Atmospheric Loss • Atmospheres can lose atoms from thermosphere, especially low-mass ones, because they exceed the escape velocity (Jeans escape) • Escape velocity ve= (2 g R)1/2 (where’s this from?) • Mean molecular velocity vm= (2kT/m)1/2 (equipartition) • Boltzmann distribution – small numbers of atoms with velocities > 3 x vm Atmospheric Loss • Atmospheres can lose atoms from thermosphere, especially low-mass ones, because they exceed the escape velocity (Jeans escape) • Escape velocity ve= (2 g R)1/2 (where’s this from?) • Mean molecular velocity vm= (2kT/m)1/2 (equipartition) • Boltzmann distribution – small numbers of atoms with velocities > 3 x vm • Molecular hydrogen, 900 K, 3 x vm= 11.8 km/s • Jupiter ve=60 km/s, Earth ve=11 km/s, Moon = 2.4 km/s • H cannot escape gas giants like Jupiter, but is easily lost from lower-mass bodies like Earth or Mars • A consequence of Jeans escape is isotopic fractionation – heavier isotopes will be preferentially enriched Isotopic fractionation. Comet contribution to Earth’s atmosphere/water? High rel. H Some water? Jupiter H/D ratio • Jupiter H/D ratio measured by the Galileo probe: 3 x 10-5 Galileo probe, 1995. 47 km/s entry speed. 230 g’s. Parachute deployed, 58 min of data. Magnetic fields • The solar wind is a plamsa flowing from the sun. – Can help strip away a mid-size planet’s atmosphere. (Venus?) • Global magnetic field offers some protection. • Did Mars lose its atmosphere when it lost its dynamo, and thereby its surface water? • MAVEN mission and the history of water on Mars. MAVEN carries ion detectors and a UV spectrometer to measure the atmospheric properties of Mars and its interaction with the sun and solar wind. Launch: Nov. 2013 Atmospheric Evolution • Earth atmosphere originally CO2-rich, oxygen-free. • Nitrogen was released by volcanism, and primordial H2 was lost by escape. • CO2 was progressively transferred into rocks by the Urey reaction (takes place in presence of water): MgSiO3 CO2 MgCO3 SiO2 • Rise of oxygen began ~2 Gyr ago (photosynthesis) • Venus never underwent similar evolution because no free water present (greenhouse effect, too hot) • Venus and Earth have ~ same total CO2 abundance • Urey reaction probably occurred on Mars (water present early on), small carbonate deposits detected Mars Carbonates • Why so hard to find? – Small outcrops? – Dust contamination? Spirit rover image. Comanche contains carbonate. Mars reconnaissance orbiter images of Nili Fossae. Summary • Surface temperature depends on solar distance, albedo, atmosphere (greenhouse effect) • Scale height and lapse rate are controlled by bulk properties of atmosphere (and gravity) • Terrestrial planetary atmospheres are not primordial – affected by loss and outgassing • Coriolis effect organizes circulation into “cells” and is responsible for bands seen on giant planets • Isotopic fractionation is a good signal of atmospheric loss due to Jeans escape • Significant volatile quantities may be present in the interiors of terrestrial planets Key Concepts • • • • • • • • • • • • Albedo and opacity Greenhouse effect Snowball Earth Scale height H = RT/g Lapse rate Tropopause Coriolis effect 2 w v sin(q) Hadley cell Geostrophic balance Jeans escape Urey reaction Outgassing Thermal tides • These are winds which can blow from the hot (sunlit) to the cold (shadowed) side of a planet Solar energy added = FE R (1 A) 2 t r 2 t=rotation period, R=planet radius, r=distance (AU) Atmospheric heat capacity = 4R2CpP/g Where’s this from? Extrasolar planet (“hot Jupiter”) So the temp. change relative to background temperature T gFE (1 A) t 2 T 4 PTC p r Small for Venus (0.4%), large for Mars (38%)