Application of ab initio molecular orbital calculations to the structural moieties of carbohydrates. 3

Ab initio RHF/4-31G level molecular orbital calculations have been carried out on dimethoxymethane as a model compound for the acetal moiety in methyl pyranosides. The calculations are consistent with the predictions of the anomeric effect and the exo-anomeric effect. They reproduce very successfully the differences in molecular geometry observed by x-ray and neutron diffraction of single crystals of the methyl cy-D- and methyl 0-D-pyranosides. Calculations carried out at the 6-3 1G* level for methanediol confirm the earlier calculations at the 4-31G level, with smaller energy differences between the four staggered conformations.

Application of molecular orbital theory to the interpretation of x-ray absorption spectra of platinum complexes

X-ray LIII-absorption edges of platinum in nine octahedral complexes have been recorded using a bent crystal spectrograph. The edge features of the discontinuities have been interpreted with the help of qualitative molecular orbital diagrams. A correlation between the energy separation of the first two absorption maxima and the spectrochemical series of the ligands has been arrived at.

Third post-Newtonian angular momentum flux and the secular evolution of orbital elements for inspiralling compact binaries in quasi-elliptical orbits

The angular-momentum flux from an inspiralling binary system of compact objects moving in quasi-elliptical orbits is computed at the third post-Newtonian (3PN) order using the multipolar post-Minkowskian wave generation formalism. The 3PN angular-momentum flux involves the instantaneous, tail, and tail-of-tails contributions as for the 3PN energy flux, and in addition a contribution due to nonlinear memory. We average the angular-momentum flux over the binary's orbit using the 3PN quasi-Keplerian representation of elliptical orbits. The averaged angular-momentum flux provides the final input needed for gravitational-wave phasing of binaries moving in quasi-elliptical orbits. We obtain the evolution of orbital elements under 3PN gravitational radiation reaction in the quasi-elliptic case. For small eccentricities, we give simpler limiting expressions relevant for phasing up to order e(2). This work is important for the construction of templates for quasi-eccentric binaries, and for the comparison of post-Newtonian results with the numerical relativity simulations of the plunge and merger of eccentric binaries.

Asteroid identification using statistical orbital inversion methods

An efficient and statistically robust solution for the identification of asteroids among numerous sets of astrometry is presented. In particular, numerical methods have been developed for the short-term identification of asteroids at discovery, and for the long-term identification of scarcely observed asteroids over apparitions, a task which has been lacking a robust method until now. The methods are based on the solid foundation of statistical orbital inversion properly taking into account the observational uncertainties, which allows for the detection of practically all correct identifications. Through the use of dimensionality-reduction techniques and efficient data structures, the exact methods have a loglinear, that is, O(nlog(n)), computational complexity, where n is the number of included observation sets. The methods developed are thus suitable for future large-scale surveys which anticipate a substantial increase in the astrometric data rate. Due to the discontinuous nature of asteroid astrometry, separate sets of astrometry must be linked to a common asteroid from the very first discovery detections onwards. The reason for the discontinuity in the observed positions is the rotation of the observer with the Earth as well as the motion of the asteroid and the observer about the Sun. Therefore, the aim of identification is to find a set of orbital elements that reproduce the observed positions with residuals similar to the inevitable observational uncertainty. Unless the astrometric observation sets are linked, the corresponding asteroid is eventually lost as the uncertainty of the predicted positions grows too large to allow successful follow-up. Whereas the presented identification theory and the numerical comparison algorithm are generally applicable, that is, also in fields other than astronomy (e.g., in the identification of space debris), the numerical methods developed for asteroid identification can immediately be applied to all objects on heliocentric orbits with negligible effects due to non-gravitational forces in the time frame of the analysis. The methods developed have been successfully applied to various identification problems. Simulations have shown that the methods developed are able to find virtually all correct linkages despite challenges such as numerous scarce observation sets, astrometric uncertainty, numerous objects confined to a limited region on the celestial sphere, long linking intervals, and substantial parallaxes. Tens of previously unknown main-belt asteroids have been identified with the short-term method in a preliminary study to locate asteroids among numerous unidentified sets of single-night astrometry of moving objects, and scarce astrometry obtained nearly simultaneously with Earth-based and space-based telescopes has been successfully linked despite a substantial parallax. Using the long-term method, thousands of realistic 3-linkages typically spanning several apparitions have so far been found among designated observation sets each spanning less than 48 hours.

Stereoselectivity in the addition of hydrogen chloride to cyclohex-1-enecarbonitrile: Possible role of chlorine lone pair-nitrile π-orbital pseudoallylic A1, 3 interaction

The (overall trans) addition of hydrogen chloride to cyclohex-1- enecarbonitrile in anhydrous alcoholic media proceeds to give cis-2-chlorocyclohexanecarboxylate (together with some cis-2- chlorocyclohexanecarboxamide): no corresponding products with the trans-configuration are detectable. In anhydrous ether the addition proceeds to give a single isomer, presumably cis-, of 2-chlorocyclohexanecarbonitrile, indicating that the configuration of the products may not be equilibrium-controlled in alcoholic media. An examination of the steric factors indicates that the transition state for protonation of the presumed intermediate, 2-chlorocyclohexylidenemethylideneimine, leading to cis-product is favoured if interaction between the lateral π-orbital of the C-N double bond and the lone-pairs on the chlorine atom at the 2-position is large. Consideration of interactions in the transition states meets Zimmerman's criticism that invoking A1, 3 interaction existing in ground states to explain product configuration takes insufficient account of the Curtin-Hammett principle.

Resistance responses blocking systemic movement of Potato virus A in potato

Peruna kestää A-virusta estämällä sen leviämistä Peruna on maissin ohella maailman kolmanneksi tärkein ravintokasvi vehnän ja riisin jälkeen. Perunaa lisätään kasvullisesti mukuloita istuttamalla, jolloin virukset siirtyvät sairaiden siemenmukuloiden välityksellä kasvukaudesta toiseen. Virustauteja voi torjua ainoastaan terveen siemenperunan ja kestävien lajikkeiden avulla. Kestävyys perustuu usein siihen, että kasvi estää viruksen leviämisen tartuntakohdasta välttyäkseen virustaudilta. Tässä työssä tutkittiin kolmea perunan A-viruksen (PVA) liikkumista estävää kestävyysmekanismia perunassa. Lisäksi työn kokeelliseen osaan oleellisesti kuuluvaa virustartutusta varten kehitettiin uusi paranneltu versio geenipyssystä. Tämä itse rakennettu laite optimoitiin PVA:n tartuttamiseen mahdollisimman helposti ja pienin käyttökustannuksin. Tutkimuksen kohteena olleessa perunan risteytysjälkeläistössä oli PVA:ta kestäviä kasveja (ryhmä nnr), jotka estivät viruksen liikkumisen aiheuttamatta oireita tartutuskohdassa, sekä kasveja, joissa PVA aiheutti kuolioläikkinä näkyvän yliherkkyysvasteen (ryhmä HR). Molemmissa kestävyystyypeissä virus pystyi monistumaan ja leviämään solusta soluun paikallisesti, mutta liikkuminen muihin kasvinosiin nilan kautta estyi. Ryhmän nnr kasveissa PVA-tartunta ei aiheuttanut tilastollisesti merkitsevää muutosta useimpien geenien ilmenemiseen tartuntakohdassa. Ainoastaan geeniperhe, joka ilmentää tiettyä proteinaasi-inhibiittoria (PI), reagoi PVA:han 24 tuntia tartutuksesta. Kun tämän PVA:han reagoivan geeniperheen jäsenet hiljennettiin nnr- perunalinjoissa, ne muuttuivat alttiiksi PVA:lle ja virus levisi tartuntakohdasta muihin kasvinosiin. Tulos osoittaa, että PI on viruskestävyystekijä. Lisäksi muut tutkimuksessa saadut tulokset tukevat mahdollisuutta, että PI estää PVA:n P1-proteinaasin toimintaa. HR-linjoissa todettiin erilaisiin puolustusvasteisiin liittyvien PR-geenien aktivoitumista PVA-tartunnan seurauksena, mutta myös ilman sitä kasvien kasvettua mullassa noin neljä viikkoa. Sen sijaan solukkoviljelyssä tai vasta kaksi viikkoa mullassa kasvaneissa kasveissa vastaavaa ei vielä todettu. Tulos viittaa siihen, että HR-perunat reagoivat herkemmin ympäristöön ja/tai kasvin kehitysasteeseen laukaisten puolustusvasteita, jotka saattavat parantaa kestävyyttä taudinaiheuttajia vastaan. Kolmas tutkittu kestävyystyyppi havaittiin Pito-perunalajikkeessa. Se muistutti nnr-kestävyyttä siten, että myös siinä viruksen liikkuminen nilassa muihin kasvinosiin estyi. PVA:n todettiin pysähtyvän vasta lehtiruodin tyvelle muodostuvaan irtoamisvyöhykkeeseen, mitä havainnollistettiin käyttämällä muunnettua PVA-rotua, joka tuotti UV-valossa fluoresoivaa vihreää valoa. Tulos viittaa siihen, että virus ei pääse kulkemaan vyöhykkeeseen kuuluvan suojaavan kerroksen läpi, jollei sillä ole pääsyä nilaan. Tällainen kestävyys on tarpeen, jotta virus ei voi korvata nilakuljetusta solusta soluun leviämisellä. Tulokset tuovat uusia näkökulmia kasvien viruskestävyyteen ja auttavat selittämään viruksen nilakuljetuksen estymistä sekä solusta soluun leviämisen pysähtymistä kestävissä kasveissa.

Electronic structures of electron donor-acceptor complexes: results from ultraviolet photoelectron spectroscopy and molecular orbital calculations

HeI photoelectron spectra of 1:1 electron donor-acceptor complexes are discussed in the light of molecular orbital calculations. The complexes discussed include those formed by BH3, BF3 and SO2. Some systematics have been found in the ionization energy shifts of the complexes compared to the free components and these are related to the strength of the donor-acceptor bond. Hel spectra of hydrogen bonded complexes are discussed in comparison with results from MO calculations. Limitations of such studies as well as scope for further investigations are indicated.

Orbital evolution studies of two HMXB pulsars

High mass X-ray binary (HMXB) pulsars are of two types, persistent and transient. 4U1538-52 is a persistent HMXB whose orbit was previously measured to be circular but the RXTE observations revealed an eccentric orbit. We observed this system with RXTE-PCA in August 2003 and our timing analysis supports the eccentric orbit of the system. However, we do not find any evidence for orbital evolution. Rotational and tidal interactions between the stars of a closed binary system result in apsidal motion which can be measured in systems with eccentric orbit. 4U0115+63 is a Be-transient HMXB whose eccentric orbit was well-determined during its 1978 outburst. We report preliminary results from analysis of data obtained during the 1999 outburst of this source with the RXTE-PCA.

Orbital evolution and orbital phase resolved spectroscopy of the HMXB pulsar 4U 1538-52 with RXTE-PCA and BeppoSAX

We report here results from detailed timing and spectral studies of the high mass X-ray binary pulsar 4U 1538-52 over several binary periods using observations made with the Rossi X-ray Timing Explorer (RXTE) and BeppoSAX satellites. Pulse timing analysis with the 2003 RXTE data over two binary orbits confirms an eccentric orbit of the system. Combining the orbitial parameters determined from this observation with the earlier measurements we did not find any evidence of orbital decay in this X-ray binary. We have carried out orbital phase resolved spectroscopy to measure changes in the spectral parameters with orbital phase, particularly the absorption column density and the iron line flux. The RXTE-PCA spectra in the 3-20 keV energy range were fitted with a power law and a high energy cut-off along with a Gaussian line at similar to 6.4 keV, whereas the BeppoSAX spectra needed only a power law and Gaussian emission line at similar to 6.4keV in the restricted energy range of 0.3-10.0 keV. An absorption along the line of sight was included for both the RXTE and BeppoSAX data. The variation of the free spectral parameters over the binary orbit was investigated and we found that the variation of the column density of absorbing material in the line of sight with orbital phase is in reasonable agreement with a simple model of a spherically symmetric stellar wind from the companion star.

Orbital evolution studies of two HMXB pulsars

High mass X-ray binary (H M X B) pulsars are of two types, persistent and transient. 4U 1538-52 is a persistent HMXB whose orbit was previously measured to be circular but the RXTE observations revealed an eccentric orbit. We observed this system with RXTE-PCA in August 2003 and our timing analysis supports the eccentric orbit of the system. However, we do not find any evidence for orbital evolution. Rotational and tidal interactions between the stars of a closed binary system result in apsidal motion which can be measured in systems with eccentric orbit. 4U0115+63 is a Be-transient HMXB whose eccentric orbit was well-determined during its 1978 outburst. We report preliminary results from analysis of data obtained during the 1999 outburst of this source with the RXTE-PCA.

KO2: Realization of Orbital Ordering in a p-Orbital System

KO2 is a molecular solid consisting of oxygen dimers. K present in the lattice donates an electron which goes on to occupy the O p levels.As the basic electronic structure is similar to that of an oxygen molecule, except for broadening due to solid state effects, KO2 represents the realization of the doping of oxygen molecules arranged in a lattice. These considerations alone result in magnetism with high ordering temperatures as our calculations reveal. However, we find that the high temperature structure is unstable to an orbital ordering (OO) transition. The microscopic considerations driving the OO transition, however, are electrostatic interactions instead of the often encountered superexchange driven ordering within the Kugel-Khomskii model often used to describe the OO. This OO transition is also found to preclude any possibility of high magnetic ordering temperatures, which otherwise seemed possible.

Ab-initio molecular orbital studies on C---H…X hydrogen bonded systemsstar

C---H…X hydrogen bonded systems are studied by the STO-3G method. The proton donor ability of carbon is analysed in terms of its hybridization states and the substituents.

Apsidal motion in 4U 0115+63 and orbital parameters of 2S 1417-624 and V0332+53

Be/X-ray binary pulsars have wide eccentric orbits and hence the angle of periastron of the orbit is very well defined in these sources. The presence of an X-ray pulsar allows for accurate measurements of orbital elements. A Be star usually is a rapidly rotating star and hence will deviate from spherical geometry. The tidal interaction between the neutron star and the Be star will add to the distortion of the Be star and alter its mass distribution. Thus a measurable rate of apsidal motion is expected from these systems. In this paper, we present the first conclusive detection of apsidal motion of the binary 4U 0115+63. We also present new and accurate orbital parameters of the Be/X-ray binaries V0332+53 and 2S 1417-624.