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Oscillations and Spins of Stars and Life. Alexander Kosovichev Stanford University. My first meeting with Wojtek : European Study Conference Oscillations as a Probe of the Sun's Interior": Catania, 20-24 June 1983. Wojtek.
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Oscillations and Spins of Stars and Life Alexander Kosovichev Stanford University
My first meeting with Wojtek: European Study Conference Oscillations as a Probe of the Sun's Interior": Catania, 20-24 June 1983 Wojtek
First meeting: Oscillations as a Probe of the Sun's Interior": Catania, 20-24 June 1983
Visit of Centrum Astronomiczne im. Mikołaja Kopernika (CAMK) in Warsaw for 3 months in 1986
CAMK was established in 1973 on occasion of 500th anniversary of Nicolaus Copernicus, and opened in 1978
Computer equipment: PDP 11/45IBM PC XTs brought to CAMK by Phil Goode
Low Frequency Oscillations in Slowly Rotating Stars • Dziembowski, W. and A. Kosovichev (1987). "Low Frequency Oscillations in Slowly Rotating Stars - Part One - General Properties." ActaAstronomica37: 313. • Dziembowski, W., A. Kosovichev, and M. Kozlowski (1987). "Low Frequency Oscillations in Slowly Rotating Stars - Part Two - Inertial Modes in the Solar Convective Envelope." ActaAstronomica37: 331. • Dziembowski, W. and A. Kosovichev (1987). "Low Frequency Oscillations in Slowly Rotating Stars - Part Three - Kelvin-Helmholtz Instability." ActaAstronomica37: 341.
Low Frequency Oscillations in Slowly Rotating Stars • Dziembowski, W., A. Kosovichev, and M. Kozlowski (1987). Inertial Modes Trapped in the Solar Convective Envelope, Advances in Helio- and Asteroseismology, Proceedings of the Symposium held 17-11 July 1986, in Aarhus, Denmark. Edited by J. Christensen-Dalsgaard and S. Frandsen. IAU Symposium, No. 123. Dordrecht: D. Reidel Publishing Co., p.117, 1988
Low Frequency Oscillations in Slowly Rotating Stars: Proc. IAU Sym. 123 -shortest paper I ever published
Primary question: What happens to g-modes when their frequencies become comparable with stellar rotation rate? ? W/2p
N2/W2 in Standard Solar Model S W2 > N2
g-modes radial wavenumber inertial modes
rotational splitting r-mode g-modes l(l+1)/2m radial wavenumber inertial modes
Calculations of the frequency spectra and mode eigenfunctions showed that the oscillation amplitude is concentrated at high latitudes.
Dziembowski, W. and A. Kosovichev (1987). "Low Frequency Oscillations in Slowly Rotating Stars - Part Three - Kelvin-Helmholtz Instability." ActaAstronomica37: 341.
Low Frequency Oscillations in Slowly Rotating Stars • Dziembowski, W. and A. Kosovichev (1987). "Low Frequency Oscillations in Slowly Rotating Stars - Part One - General Properties." ActaAstronomica37: 313. • Dziembowski, W., A. Kosovichev, and M. Kozlowski (1987). "Low Frequency Oscillations in Slowly Rotating Stars - Part Two - Inertial Modes in the Solar Convective Envelope." ActaAstronomica37: 331. • Dziembowski, W. and A. Kosovichev (1987). "Low Frequency Oscillations in Slowly Rotating Stars - Part Three - Kelvin-Helmholtz Instability." ActaAstronomica37: 341.
Life twists IoA, Cambridge, 1990-94 SOHO, Stanford, 1994-2010 Solar Dynamic Observatory, Stanford 2010 -
Big Bear Solar ObservatoryNew Solar Telescope 1.6m clear aperture – world largest solar telescope
Great Wojtek’s lessons • Do not afraid solving difficult problems • Never try to solve problems that are too difficult
Santa Fe 2009 Thanks, Wojtek!