Modelling systems and mechanisms of oscillation excitation

Simple modelling systems and mechanisms of oscillation excitation are presented that may contribute to the revealing of mechanisms of planetary magnetosphere radiosources generation and wave interactions mechanisms in the Earth ionosphere and magnetosphere as well as the excitation of VLF waves in the near-Earth space.An investigation supported by The Bulgarian National Foundation Scientific Research under Contract No. TH-302/92.     

射电源结构对VLBI天体测量的影响

目前利用VLBIMK3系统确定的延迟测量的精度约为30ps,在这样的精度下,改善计算延迟的理论模型,考虑各种微扰改正（包含30ps量级）是非常重要的。在VLBI天休测量和测地计算的各种软件中,至今尚未计及射电源结构对延迟的影响。本文利用两子源模型对源结构延迟的大小及随时间的变化进行了计算,讨论了源结构延迟对VLBI天测和测地参数的影响,指出：（1）除对某些VLBI天测的射电源作长期的监测与研究,给出它们的双频综合图外,对大多数源可采用简单的两子源模型;（2）源结构对延迟的影响主要依赖于基线相对于源形态的主要特征的空间投影;（3）源结构延迟对天测和测地参数的影响达厘米和亚毫角秒量级。     

A plea for better astrophysical and astrometric data in case of double stars of peculiar interest

Summary TheIAU Symposium No. 61 (Perth, 1973, “New Problems in Astrometry’) makes clear that radiosources will play an important role for astrometry in view of the linkage of reference systems. The purposes developed later were to link the various systems from the earth and the solar system to the most inertial possible one. Extragalactic radiosources are the most reliable objects but they are faint. So, intermediate objects are needed. Among them the radiostars, optical objects having radioemission at a certain level and for given frequencies have a fundamental and key position. Most of such radiostars are double or multiple ‘binaries’ as it can be seen from the list of reference stars issued by the Working Group of Commission 24, Working Group created in 1978. The last issue of the core list of radiostars was presented by Ch. de Vegt (Chairman of the WG) on the occasion of the last General Assembly of the IAU (November 1985). A recent study of the system α Scorpii (Antares) has shown that the data concerning the magnitude and the spectral type are not accurate enough, according to the accuracy obtained for the astrometric position (±0 _. ^s 003 for an astrolabe campaign in right ascension). There is also a need for better knowledge about the orbits. In the case of the astrolabe observations, if the distance between the components in <3″ the astrometric position concerns the photocenter and accurate physical properties are needed for comparison with the radio position. Better astrophysical properties are strongly needed for all radiostars to be used as references, during the time the astrometrists have to improve the accuracy of their measurements both in optical and radio fields. Presented by S. Débarbat.     

Mid-Infrared properties of Early-type galaxies

We have conducted a survey of early-type galaxies using the ISOCAMinstrument on board the Infrared Space Observatory (ISO)in order to probe their dustcontent. We present Mid-Infrared photometric properties for a sampleof 20 galaxies observed at 4.5, 7 and 15 μ$m. Using diagnosticcolor-color diagrams, we can delineate the different Mid-Infrared emissioncontribution from evolved stars, non-thermal emission from AGNs/radiosources, and dust.Detailed modelling of the Spectral Energy Distribution (SED)is performed showing that even though theemission from the evolved stellar population may account for a large part of the Mid-Infrared output, emission from the hot dust and the aromatic hydrocarbon bands (e.g. PAHs) is the main contributorin many cases. Modelling of the surface brightness distribution is alsomade, showing that most of the galaxies follow a de Vaucouleurs profile.The physical nature and spatial distribution of the dust that we findfrom our studies of early-type galaxies will help to constrainthe origin of the dust in those galaxies.     

The celestial pole coordinates

The coordinates of the Celestial Ephemeris Pole in the Celestial Reference System (CRS) can advantageously replace the classical precession and nutation parameters in the matrix transformation of vector components from the CRS to the Terrestrial Reference System (TRS). This paper shows that the new matrix transformation using these coordinates in place of the preceding parameters would be conceptually more simple, especially when associated with the use of the non-rotating origin on the instantaneous equator (Guinot 1979, Capitaine et al. 1986) and of a celestial reference frame as realized by positions of extragalactic sources. In such a representation, the artificial separation between precession and nutation is avoided and the practical computation of the matrix transformation only requires the knowledge of the two celestial direction cosines of the pole, instead of the large number of the quantities generally considered. The development of these coordinates is given as function of time so that their use is equivalent (when using the CRS defined by the mean pole and mean equinox of epoch J2000.0, the 1976 IAU System of Astronomical Constants and the 1980 IAU theory of nutation) to the one of the conventional series for the precession (Lieske et al. 1977) and nutation (Seidelmann 1982) parameters. Such a theoretical development should also be used in order to derive more directly the numerical coefficients of the celestial motion of the instantaneous equator from very precise observations such as VLBI.

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Résumé Les coordonnées du Pôle Céleste des Ephémerides dans le Systeme de Référence Céleste (CRS) pourraient remplacer avantageusement les paramètres classiques de precession et de nutation dans la matrice de transformation entre le CRS et le Système de Référence Terrestre (TRS). Cet article montre que la nouvelle matrice de transformation utilisant ces coordonnées à la place des paramètres classiques serait ainsi conceptuellement plus simple, en particulier lorsque l'on utilise l'origine non-tournante sur l'équa-teur instantané (Guinot 1979, Capitaine et al. 1986), ainsi que le repère de référence céleste réalisé par les positions des radiosources extragalactiques. Une telle representation évite la séparation artificielle entre précession et nutation et le calcul de la matrice de transformation correspondante ne nécessite que la connaissance des deux cosinus directeurs du pole dans le repère céleste, au lieu du grand nombre de paramètres considérés généralement. Le dèveloppement de ces coordonnées en fonction du temps est donné de façon à ce que leur usage soit équivalent (lorsque l'on se rapporte au CRS défine par le pôle et l'équinoxe moyens de l'époque J2000.0, au Système de Constantes Astronomiques IAU-1976, ainsi qu'au modèle UAI-1980 de la nutation) à celui des séries conventionnelles de la precession (Lieske et al. 1977) et de la nutation (Seidelmann 1982). Un tel développement théorique devrait également être utilise pour déterminer plus directement les coefficients numériques du déplacement céleste de l'équateur instantané, à partir des observations très précises, comme par exemple, les observations VLBI.

     

On the proposals of Chapman and of Barth for O(1S) formation in the upper atmosphere

It is argued that Chapman's process is too slow to explain the green line emission in the nightglow but that Barth's two-stage mechanism is fast enough. The key to the difference in their efficiencies is that the life-time of Chapman's intermediate [O₃] complex is very much shorter than that of Barth's intermediate [O₃] complex because of its greater internal energy. Consequently the chance of the representative mass point passing from the initial surface to the required final surface is very much less in the former case than the latter where O(¹S) is one of the products in a quite considerable fraction of the decays of the complex.     

On the relationship of 6300 Å airglow to parameters of the F-region of the ionosphere

It is shown that variations in 6300 Å airglow intensities can, under certain assumptions, be simply related to $\text{?}{}_0\text{F2}$ and its time derivative. In deriving the relationship it is not necessary to assume that the concentration of the neutral atmosphere remains constant and so the relationship is useful on occasions when changes in the neutral atmosphere do occur making it difficult to obtain agreement between observed and calculated 6300 Å intensities; An example is given of a night in which a post-midnight enhancement occurred in the airglow and for which the observations could not be reproduced using a neutral atmosphere constant with time. It is shown that the airglow variations can be explained in terms of the variations of f₀F2, implying that the airglow is due to recombination and that, during the night, changes occurred in the concentrations of the constituents of the neutral atmosphere.     

Combined Analysis of Solar Neutrino and Solar Irradiance Data: Further Evidence for Variability of the Solar Neutrino Flux and Its Implications Concerning the Solar Core

A search for any particular feature in any single solar neutrino dataset is unlikely to establish variability of the solar neutrino flux since the count rates are very low. It helps to combine datasets, and in this article we examine data from both the Homestake and GALLEX experiments. These show evidence of modulation with a frequency of 11.85 year⁻¹, which could be indicative of rotational modulation originating in the solar core. We find that precisely the same frequency is prominent in power spectrum analyses of the ACRIM irradiance data for both the Homestake and GALLEX time intervals. These results suggest that the solar core is inhomogeneous and rotates with a sidereal frequency of 12.85 year⁻¹. From Monte Carlo calculations, it is found that the probability that the neutrino data would by chance match the irradiance data in this way is only 2 parts in 10 000. This rotation rate is significantly lower than that of the inner radiative zone (13.97 year⁻¹) as recently inferred from analysis of Super-Kamiokande data, suggesting that there may be a second, inner tachocline separating the core from the radiative zone. This opens up the possibility that there may be an inner dynamo that could produce a strong internal magnetic field and a second solar cycle.     

The evolution of a beamed gamma-ray-burst afterglow: the non-relativistic case

There has been increasing evidence that at least some gamma-ray bursts (GRBs) are emission beamed. The beamed GRB-afterglow evolution has been discussed by several authors in the ultrarelativistic case. It has been shown that the dynamics of the blast wave will be significantly modified by the sideways expansion, and there may be a sharp break in the afterglow light curves under certain circumstances. However, this is only true when the fireball is still relativistic. Here we present an analytical approach to the evolution of the beamed GRB blast wave expanding in the surrounding medium (density     in the non-relativistic case, our purpose is to explore whether the sideways expansion will strongly affect the blast-wave evolution as in the relativistic case. We find that the blast-wave evolution is strongly dependent on the speed of the sideways expansion. If it expands with the sound speed, then the jet angle θ increases with time as     which means that the sideways expansion has little effect on the afterglow light curves, the flux     for     and     for     It is clear that the light curve of     is not always steeper than that of     as in the relativistic case. We also show that if the expansion speed is a constant, then the jet angle     and the radius     in this case the sideways expansion has the most significant effect on the blast-wave evolution, the flux     independent of s , and we expect that there should be a smooth and gradual break in the light curve.     

The distribution of sodium in Io's cloud: Implications

Models for the distribution of sodium in Io's vicinity and in a disk in Io's orbital plane, compared with observational data, support arguments (1) that Io is the source of the sodium, (2) that sodium is ejected from the inside hemisphere and most of the high velocity sodium which is observed is ejected from the leading inside quadrant, (3) that most of the sodium leads Io in Io's vicinity but follows Io at distances of more than 7R_j from Jupiter, (4) that a significant fraction of the sodium flux is ejected at large angles with respect to Io's orbital plane, (5) that the source velocity distribution has a pronounced high-velocity tail, and (6) that impact ionization by electrons is significant at large distances from Io.     

Radiation pressure supported stars in Einstein gravity: eternally collapsing objects

Even when we consider Newtonian stars, that is, stars with surface gravitational redshift   z ≪ 1  , it is well known that, theoretically, it is possible to have stars supported against self-gravity almost entirely by radiation pressure. However, such Newtonian stars must necessarily be supermassive. We point out that this requirement for excessively large M in the Newtonian case is a consequence of the occurrence of low   z ≪ 1  . However, if we remove such restrictions, and allow for the possible occurrence of a highly general relativistic regime,   z ≫ 1  , we show that it is possible to have radiation pressure supported stars (RPSSs) at an arbitrary value of M . Since RPSSs necessarily radiate at the Eddington limit, in Einstein gravity, they are never in strict hydrodynamical equilibrium. Further, it is believed that sufficiently massive or dense objects undergo continued gravitational collapse to the black hole (BH) stage characterized by   z =∞  . Thus, late stages of BH formation, by definition, would have   z ≫ 1  , and hence would be examples of quasi-stable general relativistic RPSSs. It is shown that the observed duration of such Eddington limited radiation pressure dominated states is   t ≈ 5 × 10⁸ (1 + z ) yr  . Thus,   t →∞  as BH formation  ( z →∞)  takes place. Consequently, such radiation pressure dominated extreme general relativistic stars become eternally collapsing objects (ECOs) and the BH state is preceded by such an ECO phase. This result is also supported by our previous finding that trapped surfaces are not formed in gravitational collapse and the value of the integration constant in the vacuum Schwarzschild solution is zero. Hence the supposed observed BHs are actually ECOs.     

Mars CO2 cycle: Effects of airborne dust and polar cap ice emissivity

Mars General Circulation Model (GCM) simulations are presented to illustrate the importance of the ice emissivity of the seasonal CO₂ polar caps in regulating the effects of airborne dust on the martian CO₂ cycle. Simulated results show that atmospheric dust suppresses CO₂ condensation when the CO₂ ice emissivity is high but enhances it when the CO₂ ice emissivity is low. This raises the possibility that the reason for the repeatable nature of the CO₂ cycle in the presence of a highly variable dust cycle is that the CO₂ ice emissivity is “neutral” - the value that leads to no change in CO₂ condensation with changing atmospheric dust. For this GCM, the “neutral” emissivity is approximately 0.55, which is low compared to observed cap emissivities. This inconsistency poses a problem for this hypothesis. However, it is clear that the CO₂ ice emissivity is a critical physical parameter in determining how atmospheric dust affects the CO₂ cycle on Mars.     

On the completeness of the lists of Compact Galaxy Groups

It is shown that the lists of Shakhbazian Compact Galaxy Groups (SCGGs) are not complete. The number of the detected groups in the strip between b = ±30° and b = ±20° is by four to five times smaller than expected. The most probable reason is that during the search for SCGGs it was hard to distinguish images of compact galaxies from that of stars on the POSS prints in dense areas of the sky at lower galactic latitudes. There is some deficit of the detected groups between 60° and 40° of the north galactic latitudes. The surface density of SCGGs in the southern galactic hemisphere between b = −50° and b = −30° is by about three times less than it is expected. Obviously, the southern sky has not been searched properly. The list of Hickson's groups is complete down to galactic latitude ±30°. However, some excess of HCGs is found in the southern hemisphere, where the surface density of the found groups is by about two times higher than that of in the northern hemisphere.     

The infrared properties of barium stars

The infrared properties of barium stars are studied using published data in the K band and from IRAS . At 12 and 25 μm the emission from barium stars shows no excess over photospheric emission. Thus the claim made by Hakkila that some barium stars show evidence of the presence of warm (∼300  K ) circumstellar material is not supported. The 60-μm properties of barium stars are studied using survival analysis methods, and it is found that very few (3.7 ± 2.6 per cent) barium stars exhibit far-infrared excesses. Furthermore, it is found that the incidence of excess emission at 60 μm is lower in barium stars than for normal G and K giants. This may indicate that the mass-transfer event that is assumed to have taken place in barium stars has removed any cool circumstellar material that may have existed in these systems. Alternatively, it is suggested that the incidence of infrared excesses in normal G and K giants may have been over-estimated as a result of not fully accounting for foreground contamination by interstellar cirrus.     

More on the narrowing of impact broadened radio recombination lines at high principal quantum number

Recently Alexander and Gulyaev have suggested that the apparent decrease in impact broadening of radio recombination lines seen at high principal quantum number n may be a product of the data reduction process, possibly resulting from the presence of noise on the telescope spectra that is not present on the calculated comparison spectra. This is an interesting proposal. However, there are serious problems with their analysis that need to be pointed out. Perhaps the most important of these is the fact that for principal quantum numbers below n=200, where the widths are not in question, their processed generated profile widths do not fit the widths of the processed lines obtained at the telescope. After processing, the halfwidths of the generated and telescope profiles must agree below n=200 if we are to believe that the processed generated linewidths above n=200 are meaningful. Theirs do not. Furthermore, we find that after applying the linewidth reduction factors found by Alexander and Gulyaev for their noise added profiles to our generated profiles to simulate their noise adding effect, the processed widths we obtain still do not come close to explaining the narrowing seen in the telescope lines for n values in the range 200<n<250. It is concluded that what is needed to solve this mystery is a completely new approach using a different observing technique instead of simply a further manipulation of the frequency-switched data.     

Purely physical separation of a small fraction of the Allende meteorite that is highly enriched in noble gases

Abstract— Fine material that floats during freeze-thaw disaggregation of the Allende meteorite is greatly enriched in noble gases compared to the bulk meteorite. Not only the elemental concentrations, but also most isotopic ratios of the noble gases in this fraction, strongly suggest that this material is very similar to the gas-rich carbonaceous residue isolated from the bulk meteorite by chemical treatment. The only significant difference in noble gas signature between our separated fraction and the chemical residues is that the ¹²⁹Xe/¹³²Xe ratio in the former is significantly lower than that in the latter, which suggests readsorption of ¹²⁹Xe released from the dissolved minerals during the chemical treatment. This is the first time that a gas-rich residue of a meteorite has been separated by a purely physical method alone. We also show that noble gases in phase Q and presolar diamond may be separable physically, although both are closely associated.     

On the linear transformation and resonant absorption of Alfvén p-modes in sunspots

We analyse the linear transformation of Alfvén p-modes into quasisurface waves and the resonant absorption of Alfvén p-waves in a slowly varying medium with a density gradient, parallel to the ambient homogeneous magnetic field. It is pointed out, that the energy transfer from Alfvén p-waves to quasisurface waves appear to take place in sunspots. The results obtained also suggest that Alfvén p-waves generated by overstability in sunspots may be absorbed in deep layers under sunspots. Moreover, it is very likely that part of the downward wave flux is reflected and hence it is possibble that essentially the energy from sunspots is transported outward by magnetogravitational waves, to which Alfvén p-waves are transformed.     

Alfvén waves in umbral flux tubes

Savage has suggested that an energy flux of 2 × 10¹⁰ erg cm^–2 s^–1 passes through the umbra of a sunspot in the form of hydromagnetic waves. In this paper some of the consequences of this flux are considered. It is first shown that it is not inconsistent with the energy requirements for the heating of umbral dots and for solar wind storms, assuming in the latter case that the flux tubes emerging from about one tenth of the area of a large spot are open-ended.However, the hypothesis also requires that Alfvén waves travel along the closed flux tubes linking the umbra either with the umbra of another spot or with the surrounding faculae and passing through regions of variable field strength and density. It is shown that, for a very simplified model, standing waves are possible in a symmetrical field configuration. For velocities of 3 km/s in the umbra, the maximum particle velocity in the loop is of order 80 km/s which strains the perturbation assumption severely. However, it is pointed out that periodic velocities of this order are observed in the chromosphere near sunspots.It is further shown that mechanical dissipation of these waves in local regions of the flux tube may contribute to the heating of faculae.     

On the fine structure of the evershed effect

The fine structure of the Evershed effect was studied using spectrograms obtained on 3 July 1969 at the Pulkovo Observatory. The results of the study of Fei and Cai lines show that the outward motion in the penumbra is concentrated only in dark filaments. It is supposed that interfilamentary spaces are parts of the photosphere not covered by dark filaments. The velocity variation along a few dark filaments shows that maximum velocity is at a distance 0.8 Rs from the center of the sunspot. The mean velocity in the interfilamentary elements is of the same order as that in the photosphere directly adjoining the penumbra. The results of measurement in Ti ii, Fe ii and CH lines show that in the colder upper part of the penumbra (CH) the velocity is greater than the velocity measured in the deeper layers (Feii and Tiii). The mean velocity at the outer boundaries of the dark filaments (Tii) is 1.5–2.0 km/s.     

Large seasonal variations in Triton's atmosphere

Triton's seasons differ materially from those of Pluto owing to four important differences in the governing physics: First, the obliquity of Triton is significantly less than Pluto's obliquity. Second, Triton's inclined orbit precesses rapidly about Neptune so that a complicated seasonal variation in the latitude of the Sun occurs for Triton. Third, Neptune's orbit is much more circular than Pluto's orbit so that the sunlight intercepted by Triton's disk does not vary seasonally. Finally, Triton's atmosphere cannot be saturated at the lower latitudes so that the mass of the atmosphere is controlled by the temperature of the high-latitude ices or liquids (polar caps), as for CO₂ on Mars. The consequences of Triton's entire surface being covered with volatile substances have been examined. It is found that the circularity of Neptune's orbit then implies that Triton would have hardly any seasonal variation at all in surface temperature or atmospheric bulk, in spite of the complicated precessional effects of Triton's orbit. The only seasonal effect would be the migration of surface ices and liquids. This scenario is ruled out because it implies a column CH₄ abundance much higher than that observed and because it quickly depletes the lower latitudes of volatiles. It is concluded that Triton's most volatile surface substances are probably relegated to latitudes higher than 35° and probably form polar caps. The temperature of the polar caps should be nearly equal, even during midwinter/midsummer when the insolation of the summer pole is greatest. If the summer pole completely sublimates during one of the “major” summers, Triton's atmosphere may begin to freeze out over the winter caps. It is therefore expected that Triton's atmosphere undergoes large and complex seasonal variations. Triton is currently approaching a “maximum southern summer”, and over the remainder of this century, a dramatic increase in CH₄ abundance above the current upper limit of 1 m-Am may be witnessed.