Introduction to Electromagnetism
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Transcript Introduction to Electromagnetism
Physics of Astronomy- spring
Dr. E.J. Zita, The Evergreen State College, 29.Mar.2004
Lab II Rm 2272, [email protected], 360-867-6853
http://academic.evergreen.edu/curricular/ PhyAstro/home.htm
Outline
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Logistics and time budget
Special events & info
Review of last quarter’s content
Preview of spring quarter
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Introduction to Modern Astrophysics Ch.9
Spring weeks 1-2
Minilecture signup
Astronomy signup
Logistics and time budget
Seminar: Read, preseminar, and write (or rewrite) one paper per week.
Research: Spend 12-16 hours per week carrying out your plan, reading, and
doing calculations.
Texts, classes, and homework:
Please present in Astronomy & Cosmologies (AC) every other week
Each team minilecture once per week in Physics of Astronomy (PA)
(homework-focussed)
NEW: P&Q (Points and questions) at least once a week in PA
Total ~ 48-60 hours/week, so be sure to schedule in R&R, to stay healthy
Special events & info
Spring Science Fair at Evergreen – you will definitely present a poster of your
research there: May 28-29 (week 9)
APS-NW = American Physical Society – Northwest Section meeting
Moscow, Idaho / Pullman, WA 21-22 May (Fri.Sat end of week 8)
Do you want to go? Present a poster of your research
Deadline for registration and Abstracts: 23 April (week 4)
Calculus tutorials with Matt (details TBA)
TAs = Emily Himmelright and Jenni Walsh
Office hours: Wednesday 5-6 in fishbowl
Review of winter quarter content
Intro to Modern Astrophysics
Carroll and Ostlie = CO
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Basic astronomy
Gravity + orbits
Light + spectra
Modern physics, QM
Electromagnetism
• Sun and Stars
• Thermal + radiation
• Cosmology
Physics and Astronomy
Physics: What fundamental, quantitative principles explain the
structure and evolution of the natural world?
Astronomy: What do we see in the sky, and how do things move and
change?
Astrophysics: How can Physics explain what Astronomy observes?
Four realms of physics
Classical Mechanics
Quantum Mechanics
(big and slow:
everyday experience)
(small: particles, waves)
Special relativity
Quantum field theory
(fast: light, fast particles)
(small and fast: quarks)
Ch.1: The Celestial Sphere
(Figures from Freedman and Kaufmann, Universe)
1.1: The Greek Tradition; Team 1: Celestial Sphere
1.2 The Copernican Revolution; Team 2: Periods; prob.1.3
1.3 Positions on the Cel.Sph.
Team 3.a: Altitude+ Azimuth (p.10-13), prob. 1.5
Team 3.b: Right Ascension and Declination (p.13-15), prob.1.4
Team 3.c: Precession and motion of the stars (p.15-19), prob.1.6
1.4 Physics and Astronomy
Ch.1: Key concepts
arclength D = d a when a is in radians
Alt-Az above, RA-Dec below
1 1
1
S
P P
Ch.2: Celestial Mechanics
2.1 Elliptical Orbits
2.2 Newtonian Mechanics: F
GmM
rˆ
2
r
and conservation of angular momentum
2.3 Kepler’s Laws: we derived K3 from N2: 4p2r3 = GMT2
We derived the Schwarzschild radius for a black hole;
we weighed Jupiter and the Sun using orbital satellites, and
we discovered dark matter in Galaxies from non-Keplerian
velocity curves
2.4 The Virial Theorem: E = U/2 in a central field.
Keplerian orbits: closer = faster
Spherical coordinates
Ch.3: The continuous spectrum of Light
3.1
3.2
3.3
3.4
3.5
Parallax distance brightness
Magnitude
Wave nature of light
Radiation
Quantization of Energy
3.6 Color (wavelength)
temperature, power output,
absolute brightness…
Spectra tell us all this about stars:
• Color temperature: l(m) = 3x10-3/T(K)
• Temperature Power output per unit area: flux =
intensity of radiation = F=sT4
• Power output = Luminosity = L
• Intensity = power / area: F= L/4pR2
• Greater radiation flux brighter star: F ~ b
• Brightness is perceived on a logarithmic scale.
Apparent magnitude difference m2-m1=Dm= 1
brightness ratio b1/b2 = 100 1/5 = 2.512
• Absolute magnitude M is what a star would have if it
stood at a distance of d=10 pc from Earth.
Ch.5: Interaction of Light & Matter
5.1 Spectral lines
5.2 Photons
5.3 Bohr model
5.4 QM and wave-particle duality
Spectral lines tell us more about stars:
•Spectral lines composition &
atmosphere, stellar type and age,
•Shifts in spectral lines proper
motion, rotation, magnetic fields
(Zeeman),
• oscillations internal structure,
internal rotation, planets…
Emission and absorption lines
text
Planck quantizes light energy: photons
• E = hc/l = hn pc
• Interference + diffraction: light = wave
• Photoelectric effect: Light particles (photons) each
carry momentum p= hc/l
(Giancoli Ch.38)
• Maxwell’s theory + Hertz’s experiment: EM waves
Modern Physics
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Plancks’s light quanta!
explain the photoelectric effect (Einstein);
supported by Compton effect;
explain the H atom (Bohr)
with deBroglie’s matter waves
hf = Kmax + F
Bohr model
• DeBroglie: electrons as waves
• Planck: light as particles
• Derived H energies match observed spectra
Break time! then Spring syllabus:
Overview of Ch.9
Stellar Atmospheres
9.1: The radiation field
9.2: Stellar opacity
9.3: Radiative transfer
9.4: The structure of
spectral lines
Spring weeks 1-2: HW & ML
Astrophysics (Carroll & Ostlie) Ch.9
Astronomy (Freedman & Kaufmann)
19: The Nature of Stars
20: The Birth of Stars
21: Stellar Evolution
22: Deaths of stars
Physics (Giancoli) 17: Thermal
19: Heat
Mathematical Methods (Boas + Spiegel): review differentiation
& integration with Matt in QRC
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Minilecture signup for Astro & Cosmo
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Supper time … then, Seminar in Lib 4004