Astronomy 340 Fall 2005 6 December 2005 Class #27.
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Transcript of Astronomy 340 Fall 2005 6 December 2005 Class #27.
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Astronomy 340Fall 2005
6 December 2005
Class #27
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Review
What are the orbital differences between classical and resonant KBOs?
How does the distribution of particle size differ between that found in the rings of Saturn and the population of KBOs?
Generating a global magnetic field
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Review
What are the orbital differences between classical and resonant KBOs?
How does the distribution of particle size differ between that found in the rings of Saturn and the population of KBOs?
Generating a global magnetic field Rotation Fluid, conducting region covection
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Planetary Magnetic Field
Flavors of global magnetic field
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Planetary Magnetic Field
Flavors of global magnetic field Remnant solidified rocks (e.g. magnetite) Dynamo Induced by solar wind
Terrestrial Planets
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Planetary Magnetic Field
Flavors of global magnetic field Remnant solidified rocks (e.g. magnetite) Dynamo Induced by solar wind
Terrestrial Planets Moon’s B-field associated with crater basins
(youngest material) Mars residual did it once have a dynamo? Venus lacks current B-field slow rotation?
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Earth’s Dynamo
Differentiation Solid inner core, liquid outer ccore Viscosity – need liqud H2O for liquid Fe at those
conditions Convective velocity ~10 km s-1
Cooling of the Core Convection still partially driven by chemical
convection conduction
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Earth’s Dynamo
B-field amplified via twisting (convection + rotation) at core-mantle boundary B ~ (2ρΩ/σ)1/2
Other planets? Probably similar Note alignment what’s up with Uranus? Jupiter
Rotation yes Convection yes Conducting medium yes metallic H
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Jupiter’s Magnetic Field
Planck Function & Tb
B = 2kT/λ2
Tb = c2Bν/2kν2
Jupiter’s emission T = 130 K 10-35 W m-2 Hz-1
Real emission is 10-19 W m-2 Hz-1 1018K!!!
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Jupiter’s Magnetic Field
Planck Function & Tb B = 2kT/λ2
Tb = c2Bν/2kν2
Jupiter’s emission T = 130 K 10-35 W m-2 Hz-1
Real emission is 10-19 W m-2 Hz-1 1018K!!! Non-thermal emission
Relativistic particles + B-field synchrotron emission at radio frequencies accounts for most of the radio emissoin
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Jupiter’s Magnetic Field
Shielding from solar wind magnetic pressure
B2/8π = nemv2/ 2RJ2
V = 400 km/s, n = 10 cm-3
V = velocity of solar wind, n = density of solar windRJ = distance to Jupiter from Sun
Pressures balance at 33 Jupiter radii
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Jupiter’s Magnetic Field
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Extrasolar Planets
Detection Methods
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Extrasolar Planets
Detection Methods Radial velocity variation Astrometry Direct imaging transients
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Imaging
Detection of “point source” image reflected stellar light Lp/L* = p(λ,α)(Rp/a)2
α angle between star and observer as seen from planet
p geometric albedo Ratio ~ 10-9 for Jupiter
Difficulties Planets are overwhelmed by starlight Separations are tiny need space
interferometry, adaptive optics
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Dynamical Perturbation
Motion of planet causes reflex circular motion in star about the center of mass of star/planet system
Observables:
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Dynamical Perturbation
Motion of planet causes reflex circular motion in star about the center of mass of star/planet system
Observables: Radial velocity variations Variations in position (astrometry) Variation in the time of arrival of some reference
signal (generally used for pulsars)
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Radial Velocity Variations
Just use Newton and Kepler….we’ll do this on the board…
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Radial Velocity Variations
Just use Newton and Kepler….we’ll do this on the board…
For Jupiter-Sun system K = 12.5 m s-1 with a period of 11.9 years
For Earth-Sun system K = 0.1 m s-1
Only measure Mpsin i, not Mp
All extrasolar planets were initially detected using radial velocity variations Resolution of 15 m s-1 are possible but keep in mind the
orbit times! Might get down to 1 m s-1
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Astrometric Position
Star moves a bit as it orbits about the center of mass
Angular semi-major axis:
α = (Mp/M*) (a/d) Units: a (AU), d (pc) Jupiter-Sun system viewed from 10 pc away 500μas Earth-Sun 0.3μas
Need space interferometry impossible from the ground
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Timing
1st “planet” detected was around a pulsar hard to believe!
Planet causes a tiny wobble which would affect timing of pular Τp = 1.2 (Mpulsar/Mplanet)(P/1 year)2/3 ms
Discovery of few Earth mass sized objects around pulsar PSR 1257+12
Where did they come from? Survived the SNe? Captured Formed after the formation of the neutron star
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Transits/Reflections
How does planetary motion affect the apparent brightness of the star?
In suitable geometry, planet blocks out part of the star 2% for a Sun-Jupiter system ΔL/L ~ (Rp/R*)2
Tiny fractions for terrestrial planets 10-5
Timing – transits are short! Τ = (P/π)(R*cosδ + Rp)/a = 13(M*)-1/2(a)1/2(R*) h
In units of solar masses, solar radii, and AU 25 hours for jupiter 13 hours for Earth
Maybe a large survey of large numbers of possible stars?