Weak and intense substorms

It is shown that there is no qualitative difference between weak and intense substorms. In this paper, the growth of the electrojet across the Canada meridian chain and plasma behaviors at the synchronous distance are compared in detail for a weak and intense substorm which occurred successively on 14 July 1970. The present study, together with earlier ones, shows clearly that it is incorrect to distinguish weak substorms from more intense substorms by calling the former “local” substorms or a growth phase of more intense substorms.     

The floccule theory for planetary formation

The accumulation of floccules into protoplanets is discussed, and it is pointed out that the simplifications which have been introduced into recent numerical models may result in the incorrect conclusion being reached.     

The enigma of the Uranian satellites' orbital eccentricities

Using recently published determinations of the diameters and orbital elements of the uranian satellites and assuming reasonable dissipation functions and rigidities for icy satellites, the eccentricity decay times for the satellites were calculated. For the inner three, decay times are on the order of 10⁷–10⁸ years, making it difficult to understand why these satellites still have their observed eccentricities. The three inner satellites have a near-commensurability in their mean motions that may be able to force their eccentricities at some time in the future, but cannot force them now. Several possible explanations exist: (1) The reported eccentricities are incorrect, and are in fact near-zero. (2) The reported mean motions are incorrect, and an exact commensurability exists. (3) The physical properties that we have assumed for the satellites are grossly in error (e.g., dissipation function Q is in reality very large). (4) The system is evolving very rapidly, perhaps from a previous state of higher eccentricity. Cases 1 and 2 are unlikely when one considers the quality of existing data. Case 3 would be more consistent with non-icy compositions. Cases 2 and 4 would imply some tidal heating of the satellites, particularly Ariel. A new lower bound of ～ 1.7 × 10⁴ on the Q of Uranus is calculated from the mass of Ariel and its proximity to Uranus.     

On the effect of error correlation on linear inversions

We have examined the effect on linear helioseismic inversions of correlations in data errors, taking an example from one-dimensional rotational splitting inversion. Artificial data with correlated errors were generated and then inverted with or without using the proper covariance matrix. The effects of using incorrect covariance matrices, on solutions as well as on trade-offs, are discussed. It is found that improper account of the correlations can be deleterious to the faithfulness of the inversions, and yields incorrect error estimates, which under some circumstances can lead to misleading inferences.     

What Can the Redshift Observed in EXO 0748-676 Tell Us？

The mass-radius relations for bare and crusted strange stars are calculated with the bag model. Comparing these relations with the observed one derived from the redshift of EXO 0748-676, we come to the conclusion that it is incorrect to say that EXO 0748 676 cannot be a strange star. Various strange star models can show that EXO 0748-676 could have a mass of (1.3 - 1.7)M⊙ and a radius of(8.4 - 11.4) km. It is proposed that a proportion of nascent strange stars could be bare and have masses - 0.1 M⊙, and their masses increased over a long period of accretion.     

Precession instability models of SS433

Several models are available to describe precession instability of SS433: 6- and 7-parameter models, sinusoidal and damped sinusoidal models etc. From the available observation data, it appears that 6- and 7-parameter models are most likely to be incorrect. We have analyzed and compared the sinusoidal and damped sinusoidal models in terms of figures of phase residual, and then proposed and improved a damped sinusoidal model. The data from the three models (sinusoidal, damped sinusoidal, and improved damped sinusoidal model) have been subjected to regression analysis for the purpose of determining the differences among the models.     

A rigorous Hamiltonian approach to the rotation of elastic bodies

When the problem of the rotation of a non-rigid body is studied, the usual procedure consists of adding perturbations to the Hamiltonian of the rigid solid. In some cases, as occurs with the centrifugal deformation, the new perturbations contains potentials which depend on the velocity, but usually one alter neither the definition of the canonical variables nor the method for obtaining the Hamiltonian. Although this procedure gives good estimates and its formulation is simpler, it is incorrect from a theoretical point of view.In this paper we rigorously develop a Hamiltonian formulation of the problem, considering potentials that depend on the velocity. Thus the differences between the two procedures are clearly shown, giving special emphasis to the case of the elastic Earth, for which we show that the differences obtained cannot be ignored within the accuracy limits at present required.     

A comment on an analytical stellar model

Recently, an analytical stellar model was presented. We show that the results are incorrect as they stand.     

Robertson-Walker Lyttleton-Bondi universe with cosmological constant — A comment

It is shown that the exterior solutions of the Robertson-Walker metric in the Lyttleton-Bondi universe with cosmological constant are, in general, those space-times which represent stiff matter fluids in general relativity theory. This shows that a result stated by Varma and Roy is incorrect.     

The Misnomer of “Post-Flare Loops”

Attention is drawn to the fact that the term “post-flare loops” is incorrect and should be avoided, because the loops are parts of the flare itself. Two other names for these loop systems are suggested. Originally this was the sixth of a series of essays, published in Eos, Transactions of the American Geophysical Union on terms used in solar – terrestrial physics that are thought to be in need of clarification. The topics and writers were selected by an IAU Division II Terminology Committee. However, because of a change in EOS ’s publication policy, this contribution could no longer be published there. Therefore, following the advice of the Committee, it has been submitted to Solar Physics.     

Performance characteristics of the advanced stokes polarimeter

Recently Zirin (1995) published a response to our paper of last year (Lites, Martínez Pillet, and Skumanich, 1994), in which we quantified some limitations of vector magnetometry by the use of a generic filter magnetograph. Zirin's Letter makes specific reference to the Advanced Stokes Polarimeter (ASP), and in so doing he makes incorrect statements regarding the performance characteristics of the ASP. The intent of this paper is to rectify those erroneous representations and to clarify several other issues raised by Zirin which might give the reader of his Letter an incorrect picture of the ASP.The National Center for Atmospheric Research is sponsored by the National Science Foundation.     

Cataclysmic variables and the amplitude-cycle length relationship

After a survey of the latest state of knowledge on cataclysmic variables in general (Chapter 1) and recurrent novae in particular (Chapter 2), the amplitude-cycle length relationship (A-C relation) is rederived (Chapter 3) after statistical correction for published incorrect values of C. While the A-C relationship of dwarf novae is of the form A = -0.40 + 2.50 log C, it is, presumably for physical reasons less sharply defined for the few known recurrent novae.     

Note on the extreme values of the earth-moon distance

The extreme Earth-Moon distances during the period 1970–1979 are given. Some values stated by Gupta (1975) are incorrect.     

The solar activity in the seventeenth century re-assessed in the light of sunspot records in the local gazettes of China

21 naked-eye sunspot records in the 17th century, hitherto unknown, have been gleaned from a large collection of local gazettes of China. Based on these data, together with the telescopic records of contemporary Europe, we discuss in detail the solar activity during the 17th century. We have re-examined Wolf's years of maxima and minima and given improved values. We re-evaluate the question of the “Maunder Minimum” and conclude that it is an incorrect inference due to insufficient data.     

Microwave sources of solar flares: Loop top or foot points?

The microwave images of solar flares obtained with the VLA are reviewed from a standpoint that the microwave source is near the top or foot point(s) of a flaring loop. The review is focused on whether extended structure is missed due to the lack of short baseline components leading to an incorrect interpretation of the processed images. We conclude that at short cm (< 2 cm) there is no conclusive evidence for the source near the loop top whereas at longer cm (6, 20 cm) the source tends to occupy a significant portion of a loop. The observed bipolar structure could be unambiguously interpreted as evidence for the source at the loop top, only when it is confirmed that a more extended structure has not been missed.Proceedings of the Second CESRA Workshop on Particle Acceleration and Trapping in Solar Flares, held at Aubigny-sur-Nère (France), 23–26 June, 1986.     

How to compare the surface of Io to laboratory samples

Since one does not know the photometric functions of various parts of Io, one cannot convert the observed geometric albedo of the satellite to a parameter more directly measurable in the laboratory. One must therefore convert laboratory reflectances to geometric albedos before quantitative comparisons between Io's surface and a laboratory sample are made. This procedure involves determining the wavelength dependence of the sample's photometric function. For substances such as sulfur, whose reflectance varies strongly with wavelength, it is incorrect to assume that the photometric function, and hence the ratio (laboratory reflectance/geometric albedo) is independent of wavelength. To illustrate this point, measurements of the color dependence of this ratio for sulfur are presented for the specific case in which the measured laboratory reflectance is the sample's normal reflectance. In general, unless the laboratory reflectance is precisely the geometric albedo, a wavelength-dependent correction factor must be determined before the laboratory sample can be compared quantitatively with Io's surface.     

Slowly rotating superdense configurations in Rosen's bimetric theory of gravitation

In the limits of the Bimetric Theory of Gravitation the equations of axial-symmetric gravitational field, describing the field of rotating configurations, are obtained and examined. The analytical solutions of these equations out of configurations are found. The equations are solved numerically in the first approximation in the angular velocity for the configurations consisting of the real baryon gas (cf. Sahakian, 1972). The moments of inertia of these configurations in BTG are calculated. It is shown that the equations and the appropriate solution, obtained by Falik and Opher (1979), are incorrect.     

On inertial drifts in pulsar magnetospheres

It is pointed out that, in a number of papers, Ardavan has obtained incorrect results because of his invalid neglect of inertial drifts in attempting to obtain an integral of the motion for steadily rotating pulsar magnetospheres.     

Magnetic field evolution in simulations with Euler potentials

Using two- and three-dimensional hydromagnetic simulations for a range of different flows, including laminar and turbulent ones, it is shown that solutions expressing the field in terms of Euler potentials (EP) are in general incorrect if the EP are evolved with an artificial diffusion term. In three dimensions, standard methods using the magnetic vector potential are found to permit dynamo action when the EP give decaying solutions. With an imposed field, the EP method yields excessive power at small scales. This effect is more exaggerated in the dynamic case, suggesting an unrealistically reduced feedback from the Lorentz force. The EP approach agrees with standard methods only at early times when magnetic diffusivity did not have time to act. It is demonstrated that the usage of EP with even a small artificial magnetic diffusivity does not converge to a proper solution of hydromagnetic turbulence. The source of this disagreement is not connected with magnetic helicity or the three-dimensionality of the magnetic field, but is simply due to the fact that the non-linear representation of the magnetic field in terms of EP that depend on the same coordinates is incompatible with the linear diffusion operator in the induction equation.     

Bidirectional reflectance spectroscopy: 6. Effects of porosity

It is well known that the bidirectional reflectance of a particulate medium such as a planetary regolith depends on the porosity, in contrast to predictions of models based on the equation of radiative transfer as usually formulated. It is shown that this failure to predict porosity dependence arises from an incorrect treatment of the light that passes between the particles. In this paper a more physically correct treatment that takes account of the necessity of preventing particles from interpenetrating is used together with the two-stream approximation to solve the radiative transfer equation and derive improved expressions for the bidirectional and directional-hemispherical reflectances. It is found that increasing the filling factor (decreasing the porosity) increases the reflectance of low and medium albedo powders, but decreases it for ones with very high albedos. The model agrees qualitatively with measured data.