file: masters.97 = Rob Rutten course at CAUP Master's last: Jan 22 1998 course plan ----------- 1 = radiation processes + line broadening 2 = basic radiative transfer, thin line formation 3 = LTE/NLTE thick line formation 4 = classical stellar atmospheres 5 = extended atmospheres, coronae, winds, planetary nebulae lecture notes ------------- RTSA dark-blue notes October 1, 1997 = current WWW version Utrecht: 3rd year astronomy students (30 hours + exercises) one copy to each Masters' student one copy to T. Lago one copy to library Chapter 2 = quantities, processes, basic RT Paragraph 3.3 = line broadening Chapter 5 = classical atmospheres GTR light-blue notes March 1995 = Kiselman paste Peterson translation + Chapts 2, 3 RTSA Utrecht: 2nd year astronomy + physics students (24 hours) no electronic version yet available one copy to library Chapt 2-5 = RTSA Chapt 2 but much more extended (RTSA Chapt 2 = summary of these lecture notes) books (+/- in CAUP library) ----- - Rybicki & Lightman (should be added) + Gray + Boehm-Vitense series + Shu I, II - Novotny (out of print) - Mihalas (out of print) + Minnaert (nice new photographs from a Fin) daily log --------- 1 = Monday Oct 20: radition processes (Chapt 2 RTSA; Chapts 5 + 6 GRT) ---------------------------------------------------------------------- start: sodium D seen by Fraunhofer (engraving Chapt 1 Mg b1) viewgraph stellar spectra photograph Pickering's harem botany versus astrophysics term diagram NaI bb processes line broadening (RTSA 3.3) Doppler collisional natural bf and ff processes Zanstra mechanism planetary nebulae (last sections GRT) Thomson and Rayleigh scattering blue sky, red sun, dark red moon at eclipse photon scattering versus thermal photon creation/destruction non-local versus local nonthermal versus thermal afternoon tasks start on Chapt 2 start on Exercise 1 read RTSA 3.3 = line broadening 2 = Tuesday Oct 21: thin line formation; basic quantities (Chapt 2 RTSA) ------------------------------------------------------------------------ Bunsen-Kirchhoff experiments NaD lines from sun: Schuster-Schwarzschild shell is unlikely need for radiative transfer intensity, quantity per steradian, conserved quantity over distance mean intensity, flux, irradiance emission coefficient, extinction coefficient source function multi-process source function equation of radiative transfer thermal S = B, scattering S = J definition epsilon two-level atom integro-differential nature of the RT problem non-local nature of NLTE RT problem optical path length optical depth radial optical depth formal solution for homgeneous media afternoon tasks: read Chapt 2 at least until RT in atmospheres work out figure: lines from homogeneous media exercise 1 3 = Wednesday Oct 22 = rest Chapt 2 = thick line formation (Chapt 2 RTSA) ------------------------------------------------------------------------- definitions and basic equation repeat thin line formation repeat radio astronomy: thin and thermal Rayleigh-Jeans Wien Stefan-Boltzmann OOPS - forgot Saha-Boltzmann thick line formation constant S nature of S = (1-eps)J + eps B optical depth Eddington-Barbier solar limb darkening TE Kirchhoff LTE assumption LTE line formmation absorption line emission line NLTE line formation Na D scattering line formation CaII K emission peaks formation (all four panels) afternoon tasks listen to RR colloquium study four-panel line formation plots 4 = Thursday Oct 23 = classical stellar atmospheres (Chapt 5 RTSA) ------------------------------------------------------------------ Baschek definitons of classical atmosphere contact binaries chemical composition abundance electron donor metals Boltzmann Saha Cecilia Payne thesis diagram SpT -> T ionization fractions HE RE grey RE Kurucz modeling line blanketing backwarming surface cooling afternoon tasks read Chapt 5 5 = Friday Oct 24 = non-classical atmospheres --------------------------------------------- morning session (split, lecture room needed by poplarization course) review of what we did sofar HE, RE = classical atmosphere = N(h), T(h) optically thick Eddington-Barbier LTE and NLTE source function control optical thickness of the universe high-Z quasars Maarten Schmidt Dopplershift identification CMB 3K COBE inhomogeneity missing mass corona (8.3.1 GTR; Boehm-Vitense) white sky = forward scattering blue sky = dipole phase = nearly isotropic scattering thin shell excitation and deexcitation UV spectrum radiation loss curve afternoon session (after lunch together) extended envelopes emission line from larger size (RTSA exercise 1c) stellar winds (GTR section 8.3.2; Boehm Vitense) P Cygni profile formation radiative driving of hot-star winds Sobolev approximation (graphically) Summary ------- Most of RT physics in only five mornings. Concentrated on principles thin-thick and thermal-scattering. Plus classical atmospheres and a bit on coronae, extended atmospheres, winds, planetary nebulae. Key items: - homogeneous line formation diagrams - stellar atmosphere line formation diagrams - HE-RE atmosphere definition Skipped: - Einstein coefficients - NLTE b's and T representations - diffusion approximation - Eddington approximation - square-root epsilon law (Eddington demonstration) - two-electron processes (dielectronic recombination) - frequency redistribution - rate equations - net rate evaluations - moment definitions and operator definitions - numerical methods - VALIII - Vitense - Kurucz graph interpretations - Cayrel effect Auer-Mihalas