Finding Extrasolar Planets. I

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Elisabeth Harrington
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1 ExtraSolar Planets

2 Finding Extrasolar Planets. I Direct Searches Direct searches are difficult because stars are so bright.

3 How Bright are Planets? Planets shine by reflected light. The amount reflected is the amount received (the solar constant) - Times the area of the planet - Times the albedo (reflected), or - Times (1-albedo) (emitted) L p = L * /4πd 2 x a x πr p 2 ~ L * (R p /d) 2 For the Earth, (R p /d) 2 ~5 x 10 8 For Jupiter, (R p /d) 2 ~10 8

4 How Bright are Planets? You gain by going to long wavelengths, where the Sun is relatively faint, and the planet is relatively bright.

5 Parallax

6 How Far are Planets from Stars? By parallax, 1 AU = 1 at 1 pc 1 pc (parsec) = 3.26 light years 1 (arcsec) = 1/3600 degree As seen from α Centauri (4.3 LY): Earth is 0.75 arcsec from Sol Jupiter is 4 arcsec from Sol Can we see this? Yes, but it takes special techniques, and is not easy.

7 HR 8799 (A5V)

8 Newton s Laws and the Nature of Matter Democritus (c BCE) posited that matter was composed of atoms Atoms: particles that can not be further subdivided 4 kinds of atoms: earth, water, air, fire (the Aristotelian elements)

9 Bulk Properties of Matter Galileo showed that momentum (mass x velocity) is conserved Galileo experimented with inclined planes Observed that different masses fell at the same rate

10 Kepler s Laws Empirical laws describing planetary orbits 1. Orbits are ellipses, with the Sun at one focus of the ellipse 2. The line connecting the planet to the Sun traces out equal areas in equal times 3. a 3 = P 2

11 Isaac Newton Quantified the laws of motion, and invented modern kinematics Invented calculus Experimented with optics, and built the first reflecting telescope ( )

12 Newton s Laws I. An object in motion remains in motion, or an object at rest remains at rest, unless acted upon by a force This is the law of conservation of momentum, mv = constant

13 Newton s Laws II. A force acting on a mass causes an acceleration. F = ma Acceleration is a change in velocity

14 Newton s Laws III. For every action there is an equal and opposite reaction m 1 a 1 = m 2 a 2

15 Forces Newton posited that gravity is an attractive force between two masses m and M. From observation, and using calculus, Newton showed that the force due to gravity could be described as F g = G m M / d 2 G, the gravitational constant = 6.7x10-8 cm 3 / gm / sec Gravity is an example of an inverse-square law

16 Forces By Newton's second law, the gravitational force produces an acceleration. If M is the gravitating mass, and m is the mass being acted on, then F = ma = G m M / d 2 Since the mass m is on both sides of the equation, it cancels out, and one can simplify the expression to a = G M / d 2 Newton concluded that the gravitational acceleration was independent of mass. An apple falling from a tree, and the Moon, are accelerated at the same rate by the Earth. Galileo was right; Aristotle was wrong. A feather and a ton of lead will fall at the same rate.

18 Forces and the 3 rd Law F = ma = G m M / d 2 If you are m and M represents the mass of the Earth, a represents your downward acceleration due to gravity. Your weight is the upward force exerted on the soles of your feet (if you're standing) by the surface of the Earth. The gravitational force down and your weight (an upwards force) balance and you do not accelerate. You are in equilibrium. Suppose you use M to represent your mass, and m to represent the mass of the Earth. Then, a is the acceleration of the Earth due to your mass. This is small, but real. Your acceleration is some times that experienced by the Earth.

19 Orbits Orbit: the trajectory followed by a mass under the influence of the gravity of another mass. Gravity and Newton's laws explain orbits. In circular motion the acceleration is given by the expression a=v 2 /d where V is the velocity and d is the radius of the orbit. This is the centrifugal force you feel when you turn a corner at high speed: because of Newton's first law, you want to keep going in a straight line. The car seat exerts a force on you to keep you within the car as it turns.

20 Orbital Velocity The acceleration in orbit is due to gravity, so V 2 /d = G M / d 2 which is equivalent to saying V = (GM/d). This is the velocity of a body in a circular orbit. In low Earth orbit, orbital velocities are about 17,500 miles per hour. If we know the orbital velocity V and the radius of the orbit d, then we can determine the mass of the central object M. This is the only way to determine the masses of stars and planets.

21 What Keeps Things in Orbit? There is no mysterious force which keeps bodies in orbit. Bodies in orbit are continuously falling. What keeps them in orbit is their sideways velocity. The force of gravity changes the direction of the motion by enough to keep the body going around in a circular orbit. An astronaut in orbit is weightless because he (or she) is continuously falling. Weight is the force exerted by the surface of the Earth to counteract gravity. The Earth, the Sun, and the Moon have no weight! Your weight depends on where you are - you weigh less on the top of a mountain than you do in a valley. Your mass is not the same as your weight.

22 Newtonian Mechanics Newton s laws, plus the law of gravitation, form a theory of motion called Newtonian mechanics. It is a theory of masses and how they act under the influence of gravity. Einstein showed that it is incomplete, but it works just fine to predict and explain motions on and near the Earth.

23 Energy Laws Energy is conserved Energy can be transformed Linear Momentum is conserved mv Angular Momentum is conserved mvd

24 Deriving Kepler s 3 rd Law P 2 = d 3 (Kepler s 3 rd law, P in years and d in AU) V = (GM/d) (from Newton) The circumference of a circular orbit is 2πd. The velocity (or more correctly, the speed) of an object is the distance it travels divided by the time it takes, so the orbital velocity is V orb = 2πd/P Therefore (GM/d) = 2πd/P Square both sides: GM/d = 4π 2 d 2 /P 2 Or P 2 = (4π 2 /GM)d 3 QED 4π 2 /GM = 1 year 2 /AU 3, or 2.96 x seconds 2 / cm 3 This works not only in our Solar System, but everywhere in the universe!

25 Deriving Kepler s 2 nd Law You can use either conservation of energy, or conservation of angular momentum In orbit, K+U is a constant (and is less than zero) If the planet gets closer to the Sun, d decreases and the potential energy U (= -G m M / d) decreases, so K must increase. K=1/2 mv 2. So the velocity must increase. Orbital velocities are faster closer to the Sun, and slower when further away. By conservation of angular momentum, mvd is constant Orbits with negative total energy are bound. If K=-U, the total energy is 0. This gives the escape velocity, V esc = (2G M / d)

26 Deriving Kepler s 2 nd Law

27 Orbital Energy K+U > 0 K+U = 0 K+U < 0

28 Finding Extrasolar Planets. II Transits

29 Transits Artist s Conception Transits requires an edge-on orbit. Jupiter blocks 2% of the Sun's light the Earth blocks about 0.01%. Venus, 8 June 2004

30 How Transits Work

31 Finding Extrasolar Planets. III Astrometric Wobble

32 Finding Extrasolar Planets. IV Most planets have been found by Doppler Wobble (radial velocity variations). This selects for massive planets close to the star.

33 Orbits Planets do not orbit the Sun - they both orbit the center of mass. The radius of the orbit is inversely proportional to the mass The radius of the Sun s orbit with respect to the Earth is 1/300,000 AU, or 500 km R 1 M 1 = R 2 M 2 ; a = R 1 + R 2 This is Newton s law of equal and opposite reactions.

34 Orbital Velocity V = 2πr/P r is the radius of the orbit P is the orbital period V is the orbital velocity How fast does the star wobble? Kepler s 3 rd law: P 2 = a 3 a ~ r p (M * >> M p ) r * = m p /m * r p (center of mass) V * = 2π m p /m * / (r p ) 1/2 V = 2 cm/s; V J = 3 m/s

35 Doppler Effect Emission from a moving object is shifted in wavelength. The emission is observed at longer wavelengths (red shift) for objects moving away, and at shorter wavelengths (blue shift) for objects moving towards us. dλ/λ=v/c dλ is the shift is wavelength, λ: the wavelength v: is the velocity of the source, c: is the speed of light. If we can identify lines, then we can determine how fast The source is moving towards or away from us.

36 Doppler Shifts

37 Solar Spectrum

38 Doppler Shifts

39 Finding Extrasolar Planets. IVa Timing The Doppler Effect applied to pulse arrival times. Applicable to pulsar planets

40 Finding Extrasolar Planets. V Gravitational Lensing Foreground objects focus (and magnify) light because they distort space.

Newton s Laws and the Nature of Matter

Newton s Laws and the Nature of Matter The Nature of Matter Democritus (c. 470-380 BCE) posited that matter was composed of atoms Atoms: particles that can not be further subdivided 4 kinds of atoms: earth,