Whipple telescope observations of LS I +61 303: 2004–2006

In this paper we present the results of the past two years observations on the galactic microquasar LS I +61 303 with the Whipple 10 m gamma-ray telescope. The recent MAGIC detection of the source between 200 GeV and 4 TeV suggests that the source is periodic with very high energy (VHE) gamma-ray emission linked to its orbital cycle. The entire 50-hour data set obtained with Whipple from 2004 to 2006 was analyzed with no reliable detection resulting. The upper limits obtained in the 2005–2006 season covered several of the same epochs as the MAGIC Telescope detections, albeit with lower sensitivity. Upper limits are placed on emission during the orbital phases of 0→0.1 and 0.8→1, phases which are not included in the MAGIC data set.      

A pictorial comparison of interplanetary magnetic field polarity,solar wind speed,and geomagnetic disturbance index during the sunspot cycle

Observations of interplanetary magnetic field polarity, solar wind speed, and geomagnetic disturbance index (C9) during the years 1962–1975 are compared in a 27-day pictorial format that emphasizes their associated variations during the sunspot cycle. This display accentuates graphically several recently reported features of solar wind streams including the fact that the streams were faster, wider, and longer-lived during 1962–1964 and 1973–1975 in the declining phase of the sunspot cycle than during intervening years (Bame et al., 1976; Gosling et al., 1976). The display reveals strikingly that these high-speed streams were associated with the major, recurrent patterns of geomagnetic activity that are characteristic of the declining phase of the sunspot cycle. Finally, the display shows that during 1962–1975 the association between long-lived solar wind streams and recurrent geomagnetic disturbances was modulated by the annual variation (Burch, 1973) of the response of the geomagnetic field to solar wind conditions. The phase of this annual variation depends on the polarity of the interplanetary magnetic field in the sense that negative sectors of the interplanetary field have their greatest geomagnetic effect in northern hemisphere spring, and positive sectors have their greatest effect in the fall. During 1965–1972 when the solar wind streams were relatively slow (500 km s^-1), the annual variation strongly influenced the visibility of the corresponding geomagnetic disturbance patterns.Visiting Scientist, Kitt Peak National Observatory, Tucson, Arizona.Operated by the Association of Universities for Research in Astronomy, Inc., under contract with the National Science Foundation.     

A detailed comparison of theoretical wave spectra and wave forecasting methods

Conclusion The status of various results on the determination of the appropriate family of theoretical wave spectra to describe wind generated seas and the status of various wave forecasting methods have been reviewed. The spectra of Neumann appear to describe the sea more accurately than other theoretical spectra and the wave forecasting methods of Pierson, Neumann and James appear to be the most nearly correct for the widest variety of possible wave and weather situations.     

Charge distribution on the atmospheric aerosol over the North Atlantic and the Indian Ocean

The distribution of electric charge on the marine aerosol was determined near the sea surface of the Indian Ocean and the North Atlantic during the final stage of the Snellius II-expedition. Mean values for small ion concentrationsn ⁺=455 cm^–3 andn ^–=340 cm^–3 were found over the Atlantic, whilen ⁺=310 andn ^–=250 cm^–3 were the mean values over the Indian Ocean. The ration ⁺/n^– increased from 1.2 to 2.0 with decreasing wind velocity. At wind velocities below 5 m/s 75% of the net space charge near the ocean surface was found to be carried by small ions.     

A mapping of the electron localization function for the silica polymorphs: evidence for domains of electron pairs and sites of potential electrophilic attack

The electron localization function, η, evaluated for first-principles geometry optimized model structures generated for quartz and coesite, reveals that the oxide anions are coordinated by two hemispherically shaped η-isosurfaces located along each of the SiO bond vectors comprising the SiOSi angles. With one exception, they are also coordinated by larger banana-shaped isosurfaces oriented perpendicular to the plane centered in the vicinity of the apex of each angle. The hemispherical isosurfaces, ascribed to domains of localized bond-pair electrons, are centered ～0.70 Å along the bond vectors from the oxide anions and the banana-shaped isosurfaces, ascribed to domains of localized nonbonding lone-pair electrons, are centered ～0.60 Å from the apex of the angle. The oxide anion comprising the straight SiOSi angle in coesite is the one exception in that the banana-shaped isosurface is missing; however, it is coordinated by two hemispherically shaped isosurfaces that lie along the bond vectors. In the case of a first-principles model structure generated for stishovite, the oxide anion is coordinated by five hemispherically shaped η-isosurfaces, one located along each of the three SiO bond vectors (ascribed to domains of bonding-electron pairs) that are linked to the anion with the remaining two (ascribed to domains of nonbonding-electron pairs) located on opposite sides of the plane defined by three vectors, each isosurface at a distance of ～0.5 Å from the anion. The distribution of the five isosurfaces is in a one-to-one correspondence with the distribution of the maxima displayed by experimental Δρ and theoretical ??²ρ maps. Isosurface η maps calculated for quartz and the (HO) ₃ SiOSi(OH) ₃ molecule also exhibit maxima that correspond with the (3,?3) maxima displayed by distributions of ??²ρ. Deformation maps observed for the SiOSi bridges for the silica polymorphs and a number of silicates are similar to that calculated for the molecule but, for the majority, the maxima ascribed to lone-pair features are absent. The domains of localized nonbonding-electron pair coordinating the oxide anions of quartz and coesite provide a basis for explaining the flexibility and the wide range of the SiOSi angles exhibited by the silica polymorphs with four-coordinate Si. They also provide a basis for explaining why the SiO bond length in coesite decreases with increasing angle. As found in studies of the interactions of solute molecules with a solvent, a mapping of η-isosurfaces for geometry-optimized silicates is expected to become a powerful tool for deducing potential sites of electrophilic attack and reactivity for Earth materials. The positions of the features ascribed to the lone pairs in coesite correspond with the positions of the H atoms recently reported for an H-doped coesite crystal.     

Structure and dynamics of the Bok globule B335

CO maps of the Bok globule B335 are presented and used to derive its density profile, mass distribution, and rotational velocity structure. It is found that the cloud is in nearly hydrostatic equilibrium with a density profile that varies roughly as r^?1 in the core and r^?3 in the envelope. The observed rotation is unimportant in the force balance at the present stage of evolution.     

Petrochemical Study of Lherzolitic Rocks from the Western Alps

An integrated geologic and petrochemical comparative study offive peridotite complexes in the western Alps has been undertaken.Investigated bodies are exposed at Alpe Arami in southern Switzerland,and at Finero, Balmuccia, Baldissero and Lanzo in northwesternItaly. The Alpe Arami mass has been tectonically emplaced withinthe Lepontine gneiss terrane of the in part subducted, morenortherly European lithospheric plate, whereas the other fourultramafic masses represent original portions of the non-subductedSouth Alpine plate. Eighty samples were examined petrographically. Most are lherzolites,but a few are clinopyroxene-bearing harzburgites, olivine websteritesor clinopyroxenite. Alpe Arami peridotites locally contain primarygarnet (± minor spinel); in contrast, the South Alpinelherzolites are spinel bearing, and in addition, the Lanzo massifcontains widespread plagioclase. All masses display strain effectssuch as bent lamellae in pyroxenes, gradational or sectoraloptical extinction, and minor recrystallization. Twenty-fourbulk XRF analyses demonstrate that the investigated rocks fairlyclosely match pyrolite composition, but are slightly impoverishedin alumina. The normative olivines of all analyzed specimenshave Fa contents ranging between 8 and 10 mole per cent. Electronmicroprobe analyses for 26 olivines, 27 orthopyroxenes, 23 calcicpyroxenes, three garnets, 18 spinels, three plagioclases, 13calcic amphiboles, two chlorites and two phlogopites are presented.Phases in a particular sample are remarkably homogeneous, anobservation consistent with an inferred close approach to chemicalequilibrium. Use of various two-pyroxene geothermometers allows the followingassignments of grand average apparent temperatures for the fiveperidotite complexes: Alpe Arami, 966±78°C; Finero,893 ± 94°C; Balmuccia, 973 ± 50°C; Baldissero,1002 ± 37°C; and Lanzo, 1069 ± 85°C. Pressureestimates, determined using the lherzolitic petrogenetic grid,Al₂O₃^cpx and Al₂O₃^opx isopleths, involve large uncertainties.The Alpe Arami ultramafic body evidently crystallized at a pressureof 40 ± 10 kilobars, the nominal value depending on themethod of computation. In contrast, the South Alpine spinellherzolites seem to have last equilibrated at pressures of approximately5–20 kb. The deep upper-mantle source region of the AlpeArami body apparently was subjected to a subcontinental-typegeothermal gradient, consistent with solid-state rise of thismass and Late Alpine tectonic insertion in the old Lepontinesialic crust of the European lithospheric plate. The mechanismand driving force of this process remain obscure. In contrast,the investigated spinel peridotite complexes of the South Alpinelithospheric plate seem to have been derived from shallow, uppermostmantle sections characterized by oceanic geothermal gradients.For this reason it is conjectured that these massifs were derivedfrom the northern margin of the southern plate where continentalcrust evidently was moderately thin or absent. Their upliftand overthrusting involved P-T paths which in most cases alloweddecompression partial recrystallization and incipient fusion,the latter indicated by the presence of transecting mafic dikesand segregations associated with the peridotites. The Finerobody appears to have reached its present position at the baseof the South Alpine continental crust in pre-Mesozoic time,whereas the Lanzo complex was tectonically involved in the EarlyAlpine orogeny.     

The OSIRIS‐REx target asteroid (101955) Bennu: Constraints on its physical,geological, and dynamical nature from astronomical observations

We review the results of an extensive campaign to determine the physical, geological, and dynamical properties of asteroid (101955) Bennu. This investigation provides information on the orbit, shape, mass, rotation state, radar response, photometric, spectroscopic, thermal, regolith, and environmental properties of Bennu. We combine these data with cosmochemical and dynamical models to develop a hypothetical timeline for Bennu's formation and evolution. We infer that Bennu is an ancient object that has witnessed over 4.5 Gyr of solar system history. Its chemistry and mineralogy were established within the first 10 Myr of the solar system. It likely originated as a discrete asteroid in the inner Main Belt approximately 0.7–2 Gyr ago as a fragment from the catastrophic disruption of a large (approximately 100‐km), carbonaceous asteroid. It was delivered to near‐Earth space via a combination of Yarkovsky‐induced drift and interaction with giant‐planet resonances. During its journey, YORP processes and planetary close encounters modified Bennu's spin state, potentially reshaping and resurfacing the asteroid. We also review work on Bennu's future dynamical evolution and constrain its ultimate fate. It is one of the most Potentially Hazardous Asteroids with an approximately 1‐in‐2700 chance of impacting the Earth in the late 22nd century. It will most likely end its dynamical life by falling into the Sun. The highest probability for a planetary impact is with Venus, followed by the Earth. There is a chance that Bennu will be ejected from the inner solar system after a close encounter with Jupiter. OSIRIS‐REx will return samples from the surface of this intriguing asteroid in September 2023.