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It would be fine to discuss. Unfortunately I can't give you a link, cause I read it in a physical medium. I didn't take the time to search it over the net. <font size=-1>[ This Message was edited by: Argos on 2002-04-09 06:37 ]</font> |
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Do you know the date of the paper? Astronomy and Astrophysics has an online version (articles are only available to print subscribers though), but the magazine seems to have changed publishers, and they only have the last two years online.
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GRANER F, DUBRULLE B ASTRONOMY AND ASTROPHYSICS 282 (1): 262-268 FEB 1994 Document type: Article Language: English Cited References: 31 Times Cited: 15 Abstract: According to the Titius-Bode law, the planetary distances to the sun follow a geometric progression. We review the major interpretations and explanations of the law. We show that most derivations of Titius-Bode law are implicitely based on the assumption of both rotational and scale invariance. In absence of any radial length scale, linear instabilities cause periodic perturbations in the variable chi = ln(tau/tau(0)). Since maxima equidistant in chi obey a geometric progression in the variable tau, Titius-Bode type of laws are natural outcome of the linear regime of systems in which both symmetries are present; we discuss possible nonlinear corrections to the law. Thus, if Titius-Bode law is real, it is probably only a consequence of the scale invariance of the disk which gave rise to the planets. Author Keywords: PLANETS AND SATELLITES, GENERAL, SOLAR SYSTEM, FORMATION, HYDRODYNAMICS, INSTABILITIES KeyWords Plus: INSTABILITY, PLANETARY, DISK Addresses: GRANER F, UNIV PARIS 06,ENS,CNRS,PHYS STAT LAB,24 RUE LHOMOND,F-75231 PARIS 05,FRANCE UNIV PARIS 07,F-75231 PARIS 05,FRANCE OBSERV MIDI PYRENEES,CNRS,URA 285,F-31400 TOULOUSE,FRANCE Publisher: SPRINGER VERLAG, NEW YORK IDS Number: MW312 ISSN: 0004-6361 TITIUS-BODE LAWS IN THE SOLAR-SYSTEM .2. BUILD YOUR OWN LAW FROM DISK MODELS DUBRULLE B, GRANER F ASTRONOMY AND ASTROPHYSICS 282 (1): 269-276 FEB 1994 Document type: Article Language: English Cited References: 11 Times Cited: 5 Abstract: Simply respecting both scale and rotational invariance, it is easy to construct an endless collection of theoretical models predicting a Titius-Bode law, irrespective to their physical content. Due to the numerous ways to get the law and its intrinsic arbitrariness, it is not an useful constraint on theories of solar system formation. To illustrate the simple elegance of scale-invariant methods, we explicitly cook up one of the simplest examples, an infinitely thin cold gaseous disk rotating around a central object. In that academic case, the Titius-Bode law holds during the linear stage of the gravitational instability. The time scale of the instability is of the order of a self-gravitating time scale, (G rho(d))(-1/2), where rho(d) is the disk density. This model links the separation between different density maxima with the ratio M(D)/M(C) of the masses of the disk and the central object; for instance, M(D)/M(C) of the order of 0.18 roughly leads to the observed separation between the planets. We discuss the boundary conditions and the limit of the WKB approximation. Author Keywords: PLANETS AND SATELLITES, GENERAL, SOLAR SYSTEM, GENERAL, HYDRODYNAMICS, INSTABILITIES Addresses: DUBRULLE B, OBSERV MIDI PYRENEES,CNRS,URA 285,14 AV E BELIN,F-31400 TOULOUSE,FRANCE UNIV PARIS 06,ENS,CNRS,PHYS STAT LAB,F-75231 PARIS 05,FRANCE UNIV PARIS 07,F-75231 PARIS 05,FRANCE Publisher: SPRINGER VERLAG, NEW YORK IDS Number: MW312 ISSN: 0004-6361 |
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Full articles available on ADS:
http://adsabs.harvard.edu/cgi-bin/np...d39ae933f15536 http://adsabs.harvard.edu/cgi-bin/np...d39ae933f15536 |
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