On the nature and origin of comets and their contribution to planets

Observations of comets show that they were formed at extremely low temperatures and probably contain amorphous ices that give off exothermal energy on mild heating. The slow rotation period of 5^d.0 for the large comet P/Schwassmann-Wachmann 1 suggests that it was formed in a gravitationally undisturbed region of space. Many smaller typical comets appear to be rotating rapidly, indicating that encounters among them were frequent during formation. As a consequence, the product of the relaxation time for encounters and the mean space density near the end of comet formation was approximately 2×10² g s cm^–3. A time scale of 10⁶ yr for comet accumulation is suggested. Laboratory studies by Patashnick and Rupprecht support the probably amorphous nature of the ices. The evidence mildly favors Cameron's 1977 theory of the primitive accretion disk.Interstellar grains grown to large sizes in extremely cool clouds might pop on mild heating by supernovae or luminous young stars to increase the local opacity and scattering.Some probable and possible contribution of comets to the solar system are summarized.     

The reality of comet groups and pairs

Although the common genetic origin of the Kreutz family of Sun-grazing comets has generally been accepted, there remains uncertainty with regard to genetic identity among other groups of comets whose orbital elements are nearly alike. Porter has listed a number of such grouds and Öpik has made a statistical study of the orbits of 472 comets with aphelion distance beyond Saturn. He lists 97 groups that show similarities among their three angular elements. He calculates an overall probability of some 10^?39 that these similarities could have occurred by chance, and thus concludes that 60% or more of such comets fall into genetic groups containing from two to seven members. This paper explores the statistical reality of Öpik's groups utilizing the Monte Carlo method of statistics as well as ordinary probability theory. The conclusion is reached that except for a few pairs the similarity among orbital elements within the groups is no greater than random expectation.     

On the causes of ice-ages

The distinction between homogeneous black ice and bubbly ice is well-known. Light entering homogeneous ice at normal incidence propagates without scattering until it is absorbed by the ice in a distance of ~10 m or more. Air bubbles serve as scattering centres, and if there are enough of them multiple scatterings turn the light around by a random walk before absorption takes place. Much of the light then reemerges from the ice which shines white in the Sun.A sufficient density of submicron particles of high refractive index in surface waters could produce a similar effect in the sea. Because of the absorbing properties of water itself, the reemergent light would tend to be in the blue to orange region of the visual spectrum. Reflection of sunlight in this spectral region could lower the oceanic temperature sufficiently to cause an ice-age.The origin of a suitably large density of submicron particles of large refractive index is attributed either to bolide impact or to an enhanced density within the zodiacal dust, since normal weathering processes do not generate particles which are small enough for the reflective property to become established.     

Observations of an unusual pair of homologous flares on March 17, 1970

Correlated optical, radio and X-ray observations are presented for a pair of consequently homologous flares which occurred on March 17, 1970. A rich complexity of behavior in a bright sub-flare with maximum at 1444 UT is repeated in a flare of importance 1B with maximum at 22:49 UT. The unusual and interesting aspect of these flares is that the second flare developed at approximately half the rate of the first. A difference in the trigger mechanism of the two flares is suggested as a possible explanation.     

Is there evolution in the infrared Tully–Fisher relation? Comparing two linear regressions

In a recent paper, Puech and co-workers compared K -band Tully–Fisher relations derived for nearby and distant galaxies, respectively. They concluded that the two relations differ, and deduced that there is evolution in the Tully–Fisher relations. The statistical comparison between the two regression lines is re-examined, and it is shown that the statistical test used gives non-significant results. It is argued that better results can be obtained by comparing the 'inverse' Tully–Fisher relations, and it is demonstrated by two different methods that the nearby- and distant-sample relations do indeed differ at a very high significance level. One of the statistical methods described is non-parametric, and can be applied very generally to compare linear regressions from two different samples.     

Evaluating planetesimal bow shocks as sites for chondrule formation

Abstract— We investigate the possible formation of chondrules by planetesimal bow shocks. The formation of such shocks is modeled using a piecewise parabolic method (PPM) code under a variety of conditions. The results of this modeling are used as a guide to study chondrule formation in a one‐dimensional, finite shock wave. This model considers a mixture of chondrule‐sized particles and micron‐sized dust and models the kinetic vaporization of the solids. We found that only planetesimals with a radius of ?1000 km and moving at least ?8 km/s with respect to the nebular gas can generate shocks that would allow chondrule‐sized particles to have peak temperatures and cooling rates that are generally consistent with what has been inferred for chondrules. Planetesimals with smaller radii tend to produce lower peak temperatures and cooling rates that are too high. However, the peak temperatures of chondrules are only matched for low values of chondrule wavelength‐averaged emissivity. Very slow cooling (<?100s of K/hr) can only be achieved if the nebular opacity is low, which may result after a significant amount of material has been accreted into objects that are chondrule‐sized or larger, or if chondrules formed in regions of the nebula with small dust concentrations. Large shock waves of approximately the same scale as those formed by gravitational instabilities or tidal interactions between the nebula and a young Jupiter do not require this to match the inferred thermal histories of chondrules.     

Fast reconnaissance of carbonate dissolution based on the size distribution of calcareous ooze on Walvis Ridge, SE Atlantic Ocean

We present a new index of carbonate fragmentation based on the size distribution of bulk sediments in core MD962094 from Walvis Ridge (SE Atlantic Ocean). The carbonate fragmentation index is constructed by taking a ratio of the two coarsest fractions in the grain size distributions of the bulk calcareous ooze. The coarsest two fractions (25–90 μm and >90 μm) of the bulk sediments consist primarily of complete shells and fragments of adult foraminifera shells, and juvenile foraminifera shells and fragments, respectively. The ratio of the proportions of the two fractions is interpreted as a measure of fragmentation of the foraminifera shells caused by carbonate dissolution. Downcore changes in our carbonate fragmentation index compare very well with those in the coarse-carbonate fragmentation index in sediments from a nearby core on Walvis Ridge. The latter commonly used fragmentation index is defined as a ratio of foraminifera fragments over whole foraminifera in the >150-μm fraction as seen with a light microscope. Fragmentation is relatively high during glacial stages and relatively low during interglacial stages during the last 300 kyr, caused by the combined effect of wind-driven upwelling of corrosive water and increased production of organic matter, decreasing the preservation potential of carbonates both during and after deposition. The carbonate fragmentation index we present here provides a precise and fast method to establish a downcore fragmentation record. It can be applied to bulk sediments that are carbonate-rich (CaCO₃>68%) and to all other deep-marine sediments of which the grain size distribution of the carbonate-free fraction is available.     

Drivers of interannual and intra‐annual variability of dissolved organic carbon concentration in the River Thames between 1884 and 2013

The world's longest record of river water quality (River Thames—130 years) provides a unique opportunity to understand fluvial dissolved organic carbon (DOC) concentrations dynamics. Understanding riverine DOC variability through long‐term studies is crucial to capture patterns and drivers influencing sources of DOC at scales relevant for decision making. The Thames basin (United Kingdom) has undergone massive land‐use change, as well as increased urbanisation and population during the period considered. We aimed to investigate the drivers of intra‐annual to interannual DOC variability, assess the variability due to natural and anthropogenic factors, and understand the causes for the increased DOC variability over the period. Two approaches were used to achieve these aims. The first method was singular spectrum analysis, which was used to reconstruct the major oscillatory modes of DOC, hydroclimatic variables, and atmospheric circulation patterns and to visualise the interaction between these variables. The second approach used was generalised additive modelling, which was used to investigate other non‐natural drivers of DOC variability. Our study shows that DOC variability increased by 80% over the data period, with the greatest increase occurring from the beginning of World War II onwards. The primary driver of the increase in DOC variability was the increase in the average value of fluvial DOC over the period of record, which was itself linked to the increase in basin population and diffuse DOC sources to the river due to land‐use and land‐management changes. Seasonal DOC variability was linked to streamflow and temperature. Our study allows to identify drivers of fluvial intra‐annual and interannual DOC variability and therefore empowers actions to reduce high DOC concentrations.     

The future evolution of white dwarf stars through baryon decay and time varying gravitational constant

Motivated by the possibility that the fundamental “constants” of nature could vary with time, this paper considers the long term evolution of white dwarf stars under the combined action of proton decay and variations in the gravitational constant. White dwarfs are thus used as a theoretical laboratory to study the effects of possible time variations, especially their implications for the future history of the universe. More specifically, we consider the gravitational constant G to vary according to the parametric relation G=G ₀(1+t/t _? )^?p , where the time scale t _? is the same order as the proton lifetime t _P . We then study the long term fate and evolution of white dwarf stars. This treatment begins when proton decay dominates the stellar luminosity, and ends when the star becomes optically thin to its internal radiation.