Problems of Solar and Stellar Oscillations: Proceedings of the 66th IAU Colloquium held at the Crimean Astrophysical Observatory, U.S.S.R., 1–5 September, 1981 PDF
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PROBLEMS OF SOLAR AND STELLAR OSCILLATIONS Problems of Solar and Stellar Oscillations Proceedings of the 66th lAU Colloquium held at the Crimean Astrophysical Observatory, U.S.S.R., 1-5 September, 1981 Edited by D.O. GOUGH Institute of Astronomy, Cambridge Reprinted from Solar Physics, Vol. 82, Nos.l/2 D. Reidel Publishing Company Dordrecht : Holland / Boston: U.S.A. ISBN-13: 978-94-009-7090-8 e-ISBN-13: 978-94-009-7088-5 DOl: 10.1007/978-94-009-7088-5 All Rights Reserved Copyright © 1983 by D. Reidel Publishing Company, Dordrecht, Holland Softcover reprint of the hardcover 1s t edition 1983 No part of the material protected by this copyright notice may be reproduced or utilized in any form or by any means, electronic or mechanical including photocopying, recording or by any informational storage and retrieval system, without written permission from the copyright owner T ABLE OF CONTENTS Problems of Solar and Stellar Oscillations (Proceedings of the 66th IA U Colloquium) D. O. GOUGH / Foreword 7 V. A. KOTOV, A. B. SEVERNY, T. T. TSAP, I. G. MOISEEV, V. A. EFANOV, and N. S. NESTEROV / Manifestation of the 160-min Solar Oscillations in Velocity and Brightness (Optical and Radio Observations)(Invited Review) 9 V. A. KOTOV, S. KOUTCHMY, and O. KOUTCHMY / Observation of Global 160-min Infrared (Differential) Intensity Variation of the Sun 21 PHILIP H. SCHERRER and JOHN M. WILCOX / Structure of the Solar Oscil- lation with Period near 160 Minutes 37 ROBIN STEBBINS and CHRISTOPHER WILSON / The Measurement of Long- Period Oscillations at Sacramento Peak Observatory and South Pole 43 GERARD GREC, ERIC FOSSAT, and MARTIN A. POMERANTZ / Full-Disk Observations of Solar Oscillations from the Geographic South Pole: Latest Results (Invited Review) 55 M. WOODARD and H. HUDSON / Solar Oscillations Observed in the Total Irradiance 67 P. H. SCHERRER, J. M. WILCOX, J. CHRISTENSEN-DALSGAARD, and D. O. GOUGH / Detection of Solar Five-Minute Oscillations of Low Degree 75 RANDALL J. Bos and HENRY A. HILL / Detection of Individual Normal Modes of Oscillation of the Sun in the Period Range from 2 hr to 10 min in Solar Diameter Studies 89 F. L. DEUBNER / Helioseismology with High Degree p-Modes (Invited Review) 103 EDWARDJ. RHODES,JR., JOHN W. HARVEY, and THOMAS L. DUVALL,JR. / Recent Observations of High-Degree Solar p-Mode Oscillations at the Kitt Peak National Observatory (Invited Review, Abstract) 111 S. E. FORBUSH, M. A. POMERANTZ, S. P. DUGGAL, and C. H. TSAO / Statistical Considerations in the Analysis of Solar Oscillation Data by the Superposed Epoch Method 113 G. KovAcs / On the Accuracy of Frequency Determination by an Auto- regressive Spectral Estimator 123 HENRY A. HILL, RANDALLJ. Bos, and THOMAS P. CAUDELL / On the Origin of Oscillations in a Solar Diameter Observed through the Earth's Atmos- phere: A Terrestrial Atmospheric or a Solar Phenomenon 129 J. ROSCH and R. YERLE / Solar Diameter(s) 139 F.-L. DEUBNER and J. LAUFER / Short-Period Oscillations 151 V. E. MERKULENKO, V. I. POLYAKOV, L. E. PALAMARCHUK, and N. V. 3 4 TABLE OF CONTENTS LARIONOV / Spectral-Spatial Analysis of Wave Motions in the Region of the Temperature Minimum of the Sun's Atmosphere 157 R. T. STEBBINS, PHILIP R. GOODE, and HENRY A. HILL / Observation of Five-Minute-Period Gravity Waves in the Solar Photosphere (Invited Review, Abstract) 163 JORGEN CHRISTENSEN-DALSGAARD and SOREN FRANDSEN / Radiative Transfer and Solar Oscillations (Invited Review) 165 G. R. ISAAK / A New Method for Determining the Helium Abundance in the Solar Atmosphere (Invited Review) 205 E. A. GAVRYUSEVA, Yu. S. KoPYsov, and G. T. ZATSEPIN / 160-min Oscillations of the Sun as a Means of Studying of Its Internal Structure 209 S. V. VORONTSOV and K. I. MARCHENKOV / Adiabatic Oscillations of Solar Models with a High-Z Convective Zone 215 P. A. KUZURMAN and A. A. PAMYATNYKH / Solar Models with Low Opacity 223 H. SHlBAHASHI and Y. OSAKI/Theoretical Eigenfrequencies of Solar Oscil- lations of Low Harmonic Degree I in Five-Minute Range (Invited Review, Abstract) 231 A. CLA VERIE, G. R. ISAAK, C. P. McLEOD, H. B. VAN DER RAA Y, and T. ROCA CORTES / Rotational Splitting of Solar Five-Minute Oscillations of Low Degree (Invited Review, Abstract) 233 G. R. ISAAK / Is There an Oblique Magnetic Rotator Inside the Sun? (Invited Review, Abstract) 235 N. I. KOBANOV / The Study of Velocity Oscillations in the Solar Photosphere Using the Velocity Subtraction Technique 237 EDWARD J. RHODES, JR., ROBERT F. HOWARD, ROGER K. ULRICH, and EDW ARD J. SMITH / A New System for Observing Solar Oscillations at the Mount Wilson Observatory. I: System Design and Installation 245 W. DZIEMBOWSKI / Resonant Coupling between Solar Gravity Modes (Invited Review) 259 JEAN-PIERRE POYET / Derivation of the Amplitude Equations of Acoustic Modes of an Unstable Semi-Infinite Poly trope (Invited Review) 267 J. PERDANG / Kolmogorov Unstable Stellar Oscillations 297 A. G. KOSOVICHEV and A. B. SEVERNY / On the Exitation of Oscillations of the Sun (Numerical Models) 323 M. KNOLKER and M. STiX / A Convenient Method to Obtain Stellar Eigen- frequencies 331 GAETANO BELVEDERE, DOUGLAS GOUGH, and LUCIO PATERNO / On the Influence of Nonlinearities on the Eigenfrequencies of Five-Minute Oscil- lations of the Sun 343 L. M. B. C. CAMPOS / On Waves in Non-Isothermal, Compressible, Ionized and Viscous Atmospheres 355 Y. D. ZUGiDA, V. LocANs, and J. STAUDE / Seismology of Sunspot Atmos- pheres 369 TABLE OF CONTENTS 5 S. V. VORONTSOV / Adiabatic Oscillations of a Differentially Rotating Star. Second-Order Perturbation Theory 379 S. I. BLINNIKOV and M. Yu. KHLOPOV / Excitation of the Solar Oscillations by Objects Consisting of y-Matter 383 JEAN LATOUR, JURI TOOMRE, and JEAN-PAUL ZAHN / Nonlinear Anelastic Modal Theory for Solar Convection (Invited Review) 387 D. O. GOUGH and J. TOOMRE / On the Detection of Subphotospheric Convective Velocities and Temperature Fluctuations 401 FRANK HILL, JURI TOOMRE, and LAURENCE J. NOVEMBER / Variability in the Power Spectrum of Solar Five-Minute Oscillations (Invited Review) 411 V. A. DOGIEL / Maunder Convection Mode on the Sun and Long Solar Activity Minima 427 ROBERT HOWARD/Torsional Oscillations of the Sun (Invited Review, Abstract) 437 I. K. CSADA / Evidence for the Phi-Dependent Rotation-Oscillation of the Sun (and for the Driving Mechanism of the Asymmetric Dynamo) 439 V. S. BASHKIRTSEV, N. I. KOBANOV, and G. P. MASHNICH / The Obser- vations of 80-min Oscillations in the Quiescent Prominences 443 A. M. GALPER, V. G. KIRILLOV-UGRYUMOV, N. G. LEIKOV, and B. I. LUCHKOV / Atmospheric Internal Gravity Waves as a Source of Quasi periodic Variations of the Cosmic Ray Secondary Component and their Likely Solar Origin (Invited Review) 447 B. M. VLADIMIRSKY, V. P. BOBOVA, N. M. BONDARENKO, and V. K. VERETENNIKOVA / 160-min Pulsations in the Magnetosphere of the Earth Possibly Caused by Oscillations of the Sun 451 ICKO IBEN, JR. / An Essay on Stellar Oscillations and Evolution 457 J0RGEN CHRISTENSEN-DALSGAARD and S0REN FRANDSEN / Stellar 5 min Oscillations 469 R. M. BONNET / Helioseismology in the Future (Invited Review) 487 FOREWORD D.O.GOUGH Institute of Astronomy. Madingley Road. Cambridge. U.K. IAU Colloquium 66 on 'Problems of Solar and Stellar Oscillations' was held at the Crimean Astrophysical Observatory, U.S.S.R., on 1-5 September, 1981. The principal purpose of the colloquium was to study the low-amplitude oscillations of the Sun and, to a lesser extent, to consider similar oscillations of other stars. Much of the emphasis of the discussions was on the diagnostic value of the oscilla tions. In the last few years we have become aware that the frequencies of the five-minute modes of high degree, which constitute the major component of the oscillations discovered twenty years ago by Evans and Michaud, can be used to put quite tight bounds on the stratification of the solar convection zone. These permit a calibration of solar models computed from so-called standard evolution theory. Modes of low degree penetrate beneath the convection zone to the core of the Sun, and can in principle test the evolution theory. Therefore there was considerable interest in the reports of the latest observations of such modes. Broadly speaking, those observations confirm the cali bration by the high-degree modes, but there remain some systematic discrepancies that demand some revision of the theory. Besides the gross aspects of evolution theory, there are also more intricate details to be understood. For example, how are oscillations influenced by sunspots, or the large scale convective flow? And, of course, what is the 160m oscillation? The mechanism by which dynamical oscillations are excited is of considerable interest. It is likely that nonlinear interactions between the modes and the convection, and between the modes themselves, playa crucial role in determining the oscillation ampli tudes. Some progress in this difficult area of investigation is reported in these proceed ings. The aim of the observer is to resolve some aspects of the dynamics of the stellar atmosphere. When many modes are present, this can be a formidable task, demanding careful diagnostic techniques. Advances in the study of the interaction between radiative transfer and the dynamics of the oscillations, which has a direct bearing on the inter pretation of the data, and in the statistical analyses of the raw data, are reported here. In principle, full-disk measurements, whether they be of the radiation intensity or of spectrum-line shifts, can be made for other stars. There is already observational evidence that other late-type main sequence stars undergo oscillations similar to the five-minute oscillations of the Sun, but the individual modes have never been resolved. Issues concerning stellar evolution theory upon which the eventual resolution of such modes may bear are discussed in these proceedings. Furthermore, theoretical estimates of the amplitudes of the oscillations are reported, to guide the observers in their initial selection of suitable stars. Finally, there is a look to the future, in a summary of plans for observations, and what one might hope to be achieved. Solar PhYSics 82 (1983) 7-8. 0038-0938/83/0821-0007$00.30. Copyright © 1983 by D. Reidel Publishing Co .. Dordrecht. Holland. and Boston. U.S.A. 8 FOREWORD I am very grateful to my colleagues on the Scientific Organising Committee: R. M. Bonnet, F.-L. Deubner, W. A. Dziembowski, I. Iben, Jr., P. Ledoux, A. B. Severny, and J. M. Wilcox, for their support. Every visiting participant of the Colloquium is indebted to the Local Organising Committee: A. B. Severny, E. Ergma, v. S. Imshennik, v. A. Kotov, A. Massevich, and N. v. Steshenko, for their efforts in arranging our interesting visit to the Crimea. We are also grateful to A. Selina, who was always available to cope with administrative problems. Financial support was given by the International Astronomical Union, the Crimean Astrophysical Observatory, and the Soviet Academy of Sciences. MANIFEST ATION OF THE 160-min SOLAR OSCILLATIONS IN VELOCITY AND BRIGHTNESS (OPTICAL AND RADIO OBSERV ATIONS)* (Invited Review) V. A. KOTOV,A. B. SEVERNY,T. T. TSAP, I. G. MOlSEEV, V. A. EFANOV, and N. S. NESTEROV Crimean Astrophysical Observatory, P.O. Nauchny, Crimea 334413, U.S.S.R. Abstract. All evidence of the solar origin of 160-min period oscillations is collected, and the present state of observations of this oscillation in optical and radio-ranges is considered. The main results are summarized: (a) the 160-min oscillation was observed in 1981 as well as before, (b) an attempt to find a nonradial component with I = 2 has failed, (c) the intensity and circular polarization of radioemission show with statistical significance the presence of this l60-min periodicity. 1. On the Solar Origin of 1OO-min Oscillations The 160-min periodicity has the same phase at different sites of the Earth's globe: Crimea, Stanford, and South Pole (see Figure 1); the last observations lasting for about 5 days without interruptions caused by night-time intervals as is inevitable in usual ground-based observations show also that the I-day sampling effect does not play any role. Moreover, the 160-min peak in the power spectrum (computed for 1974-1980) is the highest (see Figure 2). A possible influence of the differential transparency of the terrestrial atmosphere (difference in transparency between east and west limbs) can, in principle, bring some modulation, but this effect, on average, was reported to be at least 10 times smaller than the observed one (see Severny et al., 1980) and does not produce the systematic shift of the phase from year to year. Besides that, the changes of transparency do not show the 160-min variations, as follows from the work by Clarke (1980). The apparent absence of the 160-min oscillations in velocity when one uses a telluric line, as well as the indication for the 27.2-day periodicity in the variations of an amplitude of this 160-min oscillation (Kotov et al., 1982), are also worth noticing. One should also note that the synchronous, in parallel with the line-of-sight velocity, variations in the intensity and circular polarization of radioemission from the Sun are observed (see below), which can not be ascribed to fluctuations in the ionosphere of the Earth. The 160-min variations in IR limb-darkening were observed by Koutchmy's and Kotov (1980). A full analysis of possible non-solar sources and errors is in Kotov et al. (1982). * Proceedings of the 66th lAU Colloquium: Problems in Solar and Stellar Oscillations, held at the Crimean Astrophysical Observatory, U.S.S.R., 1-5 September, 1981. Solar Physics 82 (1983) 9-19. 0038-0938/83/0821-0009$01.65. Copyright © 1983 by D. Reidel Publishing Co., Dordrecht, Holland, and Boston, U.S.A. 10 V. A. KOTOV ET AL. • CRIMEA, 1974 -1980 'en 0 E • • -1 0.4 I STANFORD, 1976-1979 0.2 "7en 0.0 E - 0.2 0.5 SOUTH POLE, 1979-1980 • 'en 0.0 E • • • - 0.5 0.0 0.5 1.0 PHASE ( 160r:'01O ) Fig. 1. Superposed epoch plot of the Crimean, Stanford, and South Pole observations with a folding period of 160.010 min. Zero phase corresponds to UT oohoom on I January, 1974. The sinusoids represent the best fitted harmonic waves computed for three observatories separately. Vertical lines indicate rms error for each point. 2. Present State of Optical Observations (1974-1980) A summary of the Crimean measurements of solar velocity is presented in Table I. The results of superposed epoch analysis for the Crimea, Stanford, and South Pole are illustrated by Figure 1 showing good agreement in phases of mean line-of-sight velocity curves; some difference in amplitudes can be easily ascribed to the differences in methodes of measurements (different areas for averaging of velocity over the solar disk) and, in some part, - to difference in calibration. There is also a good agreement between the dependences of the moments of observed maximum (of outward velocity) upon the time (year) of observation (Figure 3); both Crimea and Stanford clearly show a year-to-year progressive drift of this moment provided that the period of the oscillations, in superposed epoch plots, is precisely 160.000 min; this phase drift is found to be in quite a good agreement with South Pole result too (see label N on Figure 3). This drift of the velocity maximum, determined for each individual year with exactly 160.000 min period, points to a true period of 160.010 min, corresponding to a yearly shift of the phase by about 32 min, on average.
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