bluuebunny/crossref_metadata_2025_split huggingface dataset:
The Nasa Solar Probe Mission: In Situ Determination of Interplanetary Out-of-The Ecliptic and Near-Solar Dust Environments
Authors: Tsurutani Bruce T. , Randolph James E. 
Published: July 2016

AbstractThe NASA Solar Probe mission will be one of the most exciting dust missions ever flown and will lead to a revolutionary advance in our understanding of dust within our solar system. Solar Probe will map the dust environment from the orbit of Jupiter (5 AU), to within 4 solar radii of the sun’s center. The region between 0.3 AU and 4 Rshas never been visited before, so the 10 days that the spacecraft spends during each (of the two) orbit is purely exploratory in nature. Solar Probe will also reach heliographic latitudes as high as ~ 15 to 28 above (below) the ecliptic on its trajectory inbound (outbound) to (from) the sun. This, in addition to the ESA/NASA Ulysses mission, will help determine the out-of-the-ecliptic dust environment. A post-perihelion burn will reduce the satellite orbital period to 2.5 years about the sun. A possible extended mission would allow data reception for 2 more revolutions, mapping out a complete solar cycle. Because the near-solar dust environment is not well understood (or is controversial at best), and it is very important to have better knowledge of the dust environment to protect Solar Probe from high velocity dust hits, we urgently request the scientific community to obtain further measurements of the near-solar dust properties. One prime opportunity is the July 1991 solar eclipse.
A Cosmic Matter Accretion Event Around 660,000 Years Before Present Found in Two Dated, Central Pacific Cores
Authors: Yamakoshi Kazuo , Nogami Ken’ichi , Omori Rie , Jianguo Ma , Shulan Ma 
Published: July 2016

AbstractIn order to study large-scaled cosmic matter accretion events in the past, Ir enriched layers at C-T and other geological boundaries and dated sedimental cores have been searched by many scientists. In this work, Iridium contents and the ratios of (Co/Fe) in two dated, respective layers of the cores are determined. These samples were dated fortunately with the paleomagnetic and also with the cosmogenic Be-10 methods. Ir enrichments are found at (0.660 ± 0.030) My before present.
Noble Metal Enrichments in Cosmic Spherules
Authors: Nogami K. , Misawa K. , Omori R. , Jianguo M. , Yamakoshi K. 
Published: July 2016

AbstractIn this work, studies on relationships of chemical compositions between fusion crust and nucleus in iron spherules are reported. More than 10% of the iron spherules which were picked out from deep sea sediment, have cores and crusts. We were able to divide three of them into cores and crusts. Each cores and crusts were analyzed individually by INAA. The core mainly consists of iron and nickel. Other trace elements, especially noble metal Au and Ir were concentrated in the core. The mechanism of core formation in the iron spherules shows us the origin of them.
Spatial Distribution and Orbital Properties of Zodiacal Dust
Authors: Kneißel Bernhard , Mann Ingrid 
Published: July 2016

AbstractWithin the recent years the spatial distribution of Zodiacal dust has been subject to a variety of modelling approaches. Whereas models derived from observations in the visual range tend to demand for an increase of interplanetary matter above the solar poles (bulges), models based on infrared measurements and extended to small r seem to favor a decrease there (holes). The models are reviewed, and the dynamical structure implicated in the models is outlined.
The Infrared Zodiacal Light
Authors: Hanner Martha S. 
Published: July 2016

AbstractThermal emission from interplanetary dust is the main source of diffuse radiation atλ5-50 μm. Analysis of infrared sky maps from IRAS and ZIP lead to the result that the average optical properties of the dust change with heliocentric distance. The present uncertainties in calibration should be resolved by COBE. Existence of a dust sublimation zone at 4 solar radii awaits confirmation at the next solar eclipse.
Fine Resolution Brightness Distribution of the Visible Zodiacal Light
Authors: Kwon S. M. , Hong S. S. , Weinberg J. L. , Misconi N. Y. 
Published: July 2016

AbstractApplying time-dependent corrections of the atmospheric diffuse light to the observed night sky brightness, we have determined brightness of the zodiacal light over the region 40° ≤λ − λ⊙ ≤;320ΰand − 20°≤β≤20ΰ. The resulting map of equal brightness contours has an angular resolution of two degrees, and exhibits east-west and north-south asymmetries.
Modeling Dust Fragmentation in Comets
Authors: Konno I. , Huebner W.F. 
Published: July 2016

AbstractWe developed a 1-D hydrodynamic model of dusty gas flow with dust fragmentation in a cometary atmosphere and performed calculations for a dust-size distribution with radiia =10−4— 10 cm and densities variable with dust size. A comparison was made with Giotto observations of dust jet intensities within 100 km of the nucleus of Comet Halley. We found that dust fragmentation cannot be solely responsible for the flattening of the dust intensity near the nucleus with respect to the 1/R law. We conclude that a combination of geometric effects and grain fragmentation may explain the observed intensity profiles.
The Contribution of Long Period Comets to the Interplanetary Dust Cloud
Authors: Fulle M. , Cremonese G. 
Published: July 2016

AbstractThe numerical analysis of cometary dust tails (Fulle 1989) allows to obtain the mass loss rate, the size distribution, the ejection velocity and the orbital eccentricity of the dust grains ejected by the parent comets. All these physical quantities are necessary and sufficient to compute the comet mass contribution to the interplanetary dust cloud. We apply this method to three long period comets, namely C∕Bennett 1970II, C∕Bradfield 1987XXIX and C∕Liller 1988V, and obtain that each long period comet injects in bound orbits at least half of the total produced mass. When we consider that a typical long period comet can produce more than 1014g of dust along each perihelion passage, we obtain that the considered long period comets alone injected a input mass rate of about 106g s−1of meteoroids in bound orbits during the last 20 years, a contribution which is very close to that from all short period comets.
Chemical Composition of an Emanation from Comets: Identification of the 3 Micron Comet Feature
Authors: Sakata A. , Wada S. , Tokunaga A.T. 
Published: July 2016

AbstractRecent high resolution observations of comets revealed a detailed spectral shape of the 3.4μfeature. We measured IR spectra of simple 14 hydrocarbon molecules and made ”synthesized comet spectrum”. Peak wavelength and spectral shape of the synthesized spectrum are well in agreement with the observed comet features.
Scattering Properties of Cometary Dust Based on Polarimetric Data
Authors: Mukai Sonoyo , Mukai Tadashi , Kikuchi Sen 
Published: July 2016

AbstractReferring to the dust model in Mukai and Mukai(1990), where the scattering by large rough particles and Mie scattering by small particles are taken into account, a phase function of linear polarization of several comets is examined, especially in a region of phase angles α near a maximum polarization. A lower maximum polarization observed in comet Austin(1989c1) than those in comets West(1975n) and P/Halley leads a speculation that a mixing ratio of rough scattering to Mie scattering in comet Austin increases from a sun-comet distance r of 0.6 AU to 1.2 AU. This implies that a shortage of large particles in comet Austin occured in r &lt;1 AU.
Synchronic Band and its Implication in the Cometary Dust
Authors: Watanabe Jun-ichi , Nishioka Kimihiko 
Published: July 2016

AbstractThe unique morphology of the synchronic band in the cometary dust tail is explained by finite-lifetime fragment model (Nishioka and Watanabe, 1990). However, this model needs a severe restriction on the lifetime of the dust fragments;25-70 days (r = 1 A.U.). This implies that detailed analysis of the synchronic band may reveal physical properties of the cometary dust particles. In this paper, we suggest that the fragments in the synchronic band are relatively pure ice if they are not organic grains.
Penetration of Hypervelocity Projectiles into Low Density Materials
Authors: Fujiwara A. , Kadono T. , Nakamura A. , Ishibashi T. , Fujii N. 
Published: July 2016

AbstractSpherical nylon projectiles of 7mm diameter and up-to 4km/s velocities were penetrated into three types of targets; aluminum multisheet stacks, foamed polystyrene, and 1-atm air. Penetration depth, recovery rate of the projectiles were determined as a function of projectile velocity and target density, and a new type of dust collector is proposed.
An Estimation of Meteoroid Flux at Outer Martian Space for Steady Meteor Streams
Authors: Nagasawa Ko 
Published: July 2016

AbstractThis work was done to estimate meteoroid fluxes of steady meteor streams at places far away from the sun, for example, beyond Martian orbit. For the estimation, a Normal Distribution Model is introduced. This model assumes that the flow of meteoroids is steady and the meteoroids are distributed in the form of a normal distribution around the orbit of their parent comet. Keplerian motion of each meteoroid is also assumed. Some parameters, necessary for determining a practical model, can be obtained through observations. The model will give the overall structure of meteor streams and their fluxes can be calculated for any points on the orbits of their parent comets. Calculations show that fluxes of streams sharply decrease as the solar distance increases and that meteoroids scatter chiefly along the orbital planes of the parent comets. The model seems to be useful to deduce rough structure of meteor streams.
Mass Distribution and Bulk Density Distribution of Interplanetary Dust
Authors: Hajduk A. 
Published: July 2016

AbstractMass distribution of the interplanetary dust is reexamined taking into account bulk density distribution of the dust and larger particles. It can be shown that the mass index of particles depends on the evolutionary stage of the population and changes along the mass scale. The flattening of the mass distribution at the higher mass range may explain the problem of the equilibrium between the source and sink of the interplanetary dust.
The International Meteor Organization
Authors: Gyssens M. , Knöfel A. , Rendtel J. , Roggemans P. 
Published: July 2016

AbstractFounded in 1988, the International Meteor Organization (IMO) is an international scientific non-profit association with members all over the world. The IMO was created in response to an ever growing need for international cooperation of amateur work. As such, the main objectives of the IMO are to encourage, support and coordinate meteor observing, to improve the quality of amateur observations, to make global analyses of observations received world-wide, to develop contacts between amateurs and professionals, and to disseminate the observations and results obtained to other amateurs and to the professional community.
Physical Processes on Circumplanetary Dust
Authors: Burns Joseph A. 
Published: July 2016

AbstractThe life cycles of grains in circumplanetary space are governed by various physical processes that alter sizes and modify orbits. Lifetimes are quite short, perhaps 102-104years for typical circumplanetary grains of 1 micron radius. Thus particles must be continually supplied to the circumplanetary complex, probably by the grinding down of larger parent bodies in collisions. Dust is eroded gradually through sublimation and through sputtering by the magnetospheric plasma but also is catastrophically destroyed through hypervelocity impacts with interplanetary micrometeoroids. Orbits evolve through momentum transfer (light drag, plasma or Coulomb drag, and atmospheric drag), and through resonant gravitational and electromagnetic forces. Plasma drag is generally the most effective evolution mechanism, with the possible exceptions of exospheric drag at Uranus and of electromagnetic schemes for some conditions. Since grains become charged (with typical electric potentials of a few volts), they undergo associated orbital perturbations: variable electromagnetic forces can cause the systematic drain of energy (orbital collapse) or, at specific (resonant) orbital locations can force large orbital inclinations/eccentricities. Solar radiation induces a periodic orbital eccentricity that can reach substantial values for 1 micron particles distant from the giant planets.
Jets of Fragments from Catastrophic Break-up and their Astrophysical Implications
Authors: Martelli G. , Rothwell P. , Smith P.N. , Giblin I. , Martinsson J. , Ducrocq E. , Wettstein M. , Martino M. Di , Farinella P. 
Published: July 2016

AbstractWe present some preliminary results of a series of catastrophic break-up experiments carried out in the open, against targets of natural and artificial rock, with and without a harder core. These experiments were aimed at investigating the outcomes of hypervelocity impact disruption phenomena, designed to understand the influence of large-scale collisions on the evolution of asteroids and other small solar system bodies. For the first time in this kind of experiments, evidence was found of collimated jets, i.e. the ejection of a statistically significant number of fragments all closely aligned about some preferential planes. Moreover, the presence of some groups of fragments lying close to each other on the ground was also detected.
Cometary and Asteroidal Sources of Interplanetary Dust
Authors: Sykes Mark V. 
Published: July 2016

AbstractThe Infrared Astronomical Satellite has provided extensive observations of the zodiacal cloud at high spatial resolution which will not be matched in the forseeable future. Within the zodiacal cloud, IRAS discovered extended dust structures providing the link between the interplanetary dust complex and the asteroids and comets which are its source. These are the asteroid dust bands and the cometary dust trails.
On the Accuracy of Solar Modelling
Authors: Turck-Chièze S. 
Published: July 2016

AbstractThe confrontation between theoretical predictions and observations requires an estimate of the uncertainties of these predictions. Recent results on nuclear reaction rates and photospheric abundances are analysed, in a classical model framework. The role of opacities in the determination of the helium content, the neutrino fluxes prediction and the adiabatic sound speed is discussed. Comments on extra phenomena as mass loss, turbulent mixing and WIMPS are also presented, in the light of very recent seismological results.
Solar Neutrino Projects
Authors: Spiro M. , Vignaud D. 
Published: July 2016

AbstractAn overview of the solar neutrino projects is given, with an emphasis on the complementarity of the different experiments (gallium, indium, heavy water,...) to solve the solar neutrino problem that was raised by the chlorine and the Kamiokande results. The separation of the different sources of neutrinos in the Sun would contribute significantly to the astrophysical understanding of the Sun. Some of the planned experiments could be able to pinpoint neutrino oscillations (within a wide range of parameters) almost independently of solar models. Projects which are particularly sensitive to a variation of the neutrino flux with time are also discussed.
Report on the Homestake Chlorine Solar Neutrino Experiment
Authors: Davis R. , Lande K. , Lee C.K. , Cleveland B.T. , Ullman J. 
Published: July 2016

AbstractA report on the results obtained from the chlorine radiochemical solar neutrino experiment in the Homestake mine, Lead, SD. Over the period 1970-1988 a neutrino capture rate of 2.3 ± 0.3 SNU was observed. This rate is discussed in relation: to the theoretical standard solar model, the results from the Kamiokande II experiment, and variations in the solar neutrino flux.
Matter Effects in Neutrino Propagation
Authors: Smirnov A. Yu. 
Published: July 2016

AbstractConditions and dynamics of the resonant neutrino conversion are described. We discuss the applications of the effect to the solar neutrinos as well as present status of the conversion inside the Sun. The influence of different matter density perturbations on the conversion is considered, and in this connection the possible effects of parametric and stochastic enhancement of the influence are remarked.
Recent Helioseismological Results from Space: Solar p-mode Oscillations from IPHIR on the PHOBOS Mission
Authors: Fröhlich C. , Toutain T. , Bonnet R.M. , Bruns A.V. , Delaboudinière J.P. , Domingo V. , Kotov V.A. , Kollath Z. , Rashkovsky D.N. , Vial J.C. , Wehrli Ch. 
Published: July 2016

AbstractIPHIR (Interplanetary Helioseismology by IRradiance measurements) is a solar irradiance experiment on the USSR planetary mission PHOBOS to Mars and its satellite Phobos. The experiment was built by an international consortium including PMOD/WRC, LPSP, SSD/ESA, KrAO and CRIP. The sensor is a three channel sunphotometer (SPM) which measures the solar spectral irradiance at 335, 500 and 865 nm with a precision of better than 1 part-per-million (ppm). It is the first experiment dedicated to the investigation of solar oscillations from space. The results presented here are from a first evaluation of data gathered during 160 days of the cruise phase of PHOBOS II, launched on July, 12th 1988. The long uninterrupted observation produces a spectrum of the solar p-mode oscillations in the 5-minute range with a very high signal-to-noise ratio, which allows an accurate determination of frequencies and line shapes of these modes.
Helioseismic Investigation of Solar Internal Structure
Authors: Christensen-Dalsgaard Jørgen 
Published: July 2016

AbstractThe solar oscillation frequencies provide our only means of obtaining detailed information about conditions inside the Sun. Here I give a brief overview of the relevant properties of solar models and solar oscillations, and present examples of the dependence of the oscillation frequencies on the structure of the model. Furthermore I discuss some results obtained so far from analysis of observed frequencies.
Stellar Seismology
Authors: Däppen Werner 
Published: July 2016

AbstractStellar acoustic oscillation frequencies will likely be accurately observed in the near future, in analogy to the well-known solar five-minute oscillation frequencies. Of course, we will never expect the wealth of solar data, which is a result of spatial resolution. We will therefore not be able to solve the inverse problem, that is to probe physical quantities as functions of depth, and the low number of anticipated observed frequencies will make an unambiguous mode identification difficult. Despite this restriction to the forward problem, however, observed stellar oscillation frequencies will become valuable constraints for the determination of stellar parameters. One should not forget that the present knowledge of stellar ages and compositions relies on the calibration of theoretical models (matching effective temperature and luminosity). Additional observational constraints will improve these calibrations, even if the theoretical models themselves are not questioned. We hope, however, that the observation of stellar oscillation frequencies will also lead to improvements in the physics of stellar models, in analogy to the solar case. Again, of course, stellar seismologists will be less ambitious than helioseismologists, since there are more open parameters in stellar models. However, stellar observations will allow tests of models with different age and composition.
Angular Momentum Transport and Magnetic Fields in the Solar Interior
Authors: Spruit H.C. 
Published: July 2016

AbstractThe possible mechanisms of angular momentum transport in convectively stable regions of a star are reviewed, with emphasis on transport by magnetic torques. The strength and configuration of the field in such layers is quite uncertain, because it is not known if the field can reach a dynamically stable configuration. A lower limit to the field strength is obtained by assuming that the field is always dynamically unstable, and decaying at the (rotation modified) dynamical time scale. The present field in the sun would then be of the order 1G, with poloidal and toroidal components of similar strength. The differential rotation in the core, if due only to the solar wind torque, would be very small for this field strength, and instead would more likely be governed by magnetic coulpling to the differential rotation of the convection zone. If small scale hydrodynamic transport mechanisms are present, their properties would also be influenced by a field of this strength.
Galactic Distribution and Outburst Frequency of Classical Novae
Authors: Duerbeck Hilmar W. 
Published: July 2016

AbstractThe observed rate and spatial distribution of galactic novae can be explained with the concept of two nova populations, the disc novae of faster outburst development, and the slower bulge novae. Similar populations seem to exist in nearby galaxies. The space density of galactic novae depends strongly on the recurrence time, which is unknown and may lie between 500 and 20 000 years. If the recurrence time is long, the population of quiescent novae must be identified; the hibernation scenario may or may not be a solution.
CP Puppis: Another V1500 Cyg?
Authors: O’Donoghue D. , Warner B. , Wargau W. , Grauer A.D. 
Published: July 2016

As first pointed out by Warner (1985), the overall properties of CP Pup and V1500 Cyg are very similar: both were very fast, very large amplitude novae with ~ 0.3 mag photometric humps at roughly the orbital period. Neither variation is strictly periodic (Patterson 1979; Warner 1985). Variable circular polarization (with period slightly different from the orbital period) has been found in V1500 Cyg showing that its white dwarf is strongly magnetic and has broken synchronism with the secondary star (Stockman, Schmidt & Lamb 1988). In contrast, no circular polarization has been found in CP Pup. Nonetheless, does the slight difference between the photometric and spectroscopic periods indicate it is also a magnetic system (Warner 1985; Bianchini et al. 1985a)?New photometric and spectroscopic data for CP Pup are reported which resolve the aliases and confusion in the periods found by Bianchini et al. (1985a,b), Warner (1985) and Duerbeck et al. (1987) and allow an examination of the evidence for its magnetic nature.
Chemistry of Nova Envelopes
Authors: Boyarchuk A.A. , Antipova L.I. 
Published: July 2016

Novae form a very interesting class of non-stationary objects. A considerable amount of observational data, both photometric and spectroscopic, covering different stages of nova outbursts, have been stored up by observers for many years. Processing and systematization of these data has lead to a better understanding of the physical processes taking place in the nova outbursts.The first spectra of novae at maximum brightness proved to be similar to the spectra of supergiants; their distinctive feature was the presence of the strong lines of lines from C, N and O (McLaughlin, 1936). This fact lead to suspect that these elements must be overabundant in the nova envelopes.
Simultaneous Optical and UV Spectra of the Two LMC Novae 1988
Authors: Drechsel H. , Andreae J. , Starrfield S. , Sonneborn G. 
Published: July 2016

AbstractThe two classical novae of 1988 in the LMC are the first extragalactic novae, which have been studied in the UV range. IUE spectra were taken under the Nova Target of Opportunity program, and quasi-simultaneous optical spectra were obtained by the authors. The spectral development in the UV and visual ranges is discussed for both objects.