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832 results on '"Orio M"'

103. From non-innocent to guilty : on the role of redox-active ligands in the electro-assisted reduction of CO2 mediated by a cobalt(ii)-polypyridyl complex

Author

Queyriaux, Nicolas, Abel, K., Fize, J., Pecaut, J., Orio, M., Hammarström, Leif, Queyriaux, Nicolas, Abel, K., Fize, J., Pecaut, J., Orio, M., and Hammarström, Leif

Abstract

The electrochemical behavior of [Co(bapbpy)Cl](+)[1-Cl](+), a pentacoordinated polypyridyl cobalt(ii) complex containing a redox-active tetradentate ligand (bapbpy: 6,6 '-bis-(2-aminopyridyl)-2,2 '-bipyridine) has been investigated in DMF. Cyclic voltammograms (CV), recorded in the presence of increasing amounts of chloride anions, highlighted the existence of an equilibrium with the neutral hexacoordinated complex. Under a CO(2)atmosphere, CVs of [Co(bapbpy)Cl](+)exhibit significant current enhancement assigned to CO(2)catalytic reduction. Controlled-potential electrolysis experiments confirmed formation of CO and HCOOH as the only identifiable products. The addition of water or chloride ions was shown to affect the distribution of the products obtained, as well as the faradaic efficiency associated with their electrocatalytic generation. A combination of electrochemical techniques, chemical reductions, spectroscopic measurements (UV-vis and IR) and quantum chemical calculations suggests that the ability of thebapbpyligand to be reduced at moderately negative potentials drastically limits the catalytic performances of [1-Cl](+), by stabilizing the formation of a catalytically-competent CO2-adduct that only slowly reacts with oxide acceptors to evolve towards the desired reduction products.

Published
2020
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104. Early Spectral Evolution of Classical Novae:Consistent Evidence for Multiple Distinct Outflows

Author

Aydi, E., Chomiuk, L., Izzo, L., Harvey, E. J., Leahy-McGregor, J., Strader, J., Buckley, D. A. H., Sokolovsky, K. V., Kawash, A., Kochanek, C. S., Linford, J. D., Metzger, B. D., Mukai, K., Orio, M., Shappee, B. J., Shishkovsky, L., Steinberg, E., Swihart, S. J., Sokoloski, J. L., Walter, F. M., Woudt, P. A., Aydi, E., Chomiuk, L., Izzo, L., Harvey, E. J., Leahy-McGregor, J., Strader, J., Buckley, D. A. H., Sokolovsky, K. V., Kawash, A., Kochanek, C. S., Linford, J. D., Metzger, B. D., Mukai, K., Orio, M., Shappee, B. J., Shishkovsky, L., Steinberg, E., Swihart, S. J., Sokoloski, J. L., Walter, F. M., and Woudt, P. A.

Abstract

The physical mechanism driving mass ejection during a nova eruption is still poorly understood. Possibilities include ejection in a single ballistic event, a common-envelope interaction, a continuous wind, or some combination of these processes. Here, we present a study of 12 Galactic novae, for which we have premaximum high-resolution spectroscopy. All 12 novae show the same spectral evolution. Before optical peak, they show a slow P Cygni component. After peak, a fast component quickly arises, while the slow absorption remains superimposed on top of it, implying the presence of at least two physically distinct flows. For novae with high-cadence monitoring, a third, intermediate-velocity component is also observed. These observations are consistent with a scenario where the slow component is associated with the initial ejection of the accreted material and the fast component with a radiation-driven wind from the white dwarf. When these flows interact, the slow flow is swept up by the fast flow, producing the intermediate component. These colliding flows may produce the gamma-ray emission observed in some novae. Our spectra also show that the transient heavy-element absorption lines seen in some novae have the same velocity structure and evolution as the other lines in the spectrum, implying an association with the nova ejecta rather than a preexisting circumbinary reservoir of gas or material ablated from the secondary. While this basic scenario appears to qualitatively reproduce multiwavelength observations of classical novae, substantial theoretical and observational work is still needed to untangle the rich diversity of nova properties.

Published
2020

105. Early Spectral Evolution of Classical Novae: Consistent Evidence for Multiple Distinct Outflows

Author

Aydi, E., primary, Chomiuk, L., additional, Izzo, L., additional, Harvey, E. J., additional, Leahy-McGregor, J., additional, Strader, J., additional, Buckley, D. A. H., additional, Sokolovsky, K. V., additional, Kawash, A., additional, Kochanek, C. S., additional, Linford, J. D., additional, Metzger, B. D., additional, Mukai, K., additional, Orio, M., additional, Shappee, B. J., additional, Shishkovsky, L., additional, Steinberg, E., additional, Swihart, S. J., additional, Sokoloski, J. L., additional, Walter, F. M., additional, and Woudt, P. A., additional

Published
2020
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106. On the Nature of CP Pup

Author

Mason, E, Orio, M, Mukai, K, Bianchini, A, deMartino, D, diMille, F, and Williams, R. E

Subjects
Astrophysics
Abstract

We present new X-ray and optical spectra of the old nova CP Pup (nova Pup 1942) obtained with Chandra and the CTIO 4m telescope. The X-ray spectrum reveals a multi-temperature optically thin plasma reaching a maximum temperature of 36+19 keV 16 absorbed by local complex neutral material. The time resolved optical spectroscopy confirms the presence of the 1.47 hr period, with cycle-to-cycle amplitude changes, as well as of an additional long term modulation which is suggestive either of a longer pe- riod or of non-Keplerian velocities in the emission line regions. These new observational facts add further support to CP Pup as a magnetic cataclysmic variable (mCV). We compare the mCV and the non-mCV scenarios and while we cannot conclude whether CP Pup is a long period system, all observational evidences point at an intermediate polar (IP) type CV.

Published
2013
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107. Stellar and galactic environment survey (SAGE)

Author

Barstow, M. A., primary, Burleigh, M. R., additional, Bannister, N. J., additional, Lapington, J. S., additional, Kowalski, M. P., additional, Cruddace, R. G., additional, Wood, K. S., additional, Auchere, F., additional, Bode, M. F., additional, Bromage, G. E., additional, Gibson, B., additional, Cameron, A. C., additional, Cassatella, A., additional, Delmotte, F., additional, Ravet, M.-F., additional, Doyle, J. G., additional, Jeffery, C. S., additional, Gaensicke, B., additional, Jordan, C., additional, Kappelmann, N., additional, Werner, K., additional, Lallement, R., additional, de Martino, D., additional, Matthews, S. A., additional, Phillips, K. J. H., additional, Del Zanna, G., additional, Orio, M., additional, Pace, E., additional, Pagano, I., additional, Schmitt, J. H. M. M., additional, and Welsh, B. Y., additional

Published
2008
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110. Chandra High Energy Transmission Gratings Spectra of V3890 Sgr

Author

Orio, M., primary, Drake, J. J., additional, Ness, J.-U., additional, Behar, E., additional, Luna, G. J. M., additional, Darnley, M. J., additional, Gallagher, J., additional, Gehrz, R. D., additional, Kuin, N. P. M., additional, Mikolajewska, J., additional, Ospina, N., additional, Page, K. L., additional, Poggiani, R., additional, Starrfield, S., additional, Williams, R., additional, and Woodward, C. E., additional

Published
2020
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112. Resurfacing Capitate Pyrocarbon Implant for the treatment of advanced wrist arthritis in the elderly: a retrospective study.

Author

ROCCHI, L., DE VITIS, R., PIETRAMALA, S., FULCHIGNONI, C., D'ORIO, M., MAZZONE, V., and MARCUZZI, A.

Abstract

OBJECTIVE: Advanced forms of wrist osteoarthritis in the elderly are quite common and often under-treated, preferring a conservative management of the condition due to the age of the patient. However, in elderly people who are still active, sporty and physically demanding, surgical management of wrist osteoarthritis should be considered. Proximal Row Carpectomy associated with a Resurfacing Capitate Pyrocarbon Implant (RCPI), allows the management of a wide range of wrist arthrosis, involving both the radio-carpal and the mid-carpal joints. This treatment has been already reported as a solution in younger people affected by degenerative pathologies of the wrist, giving overall good results. Authors aimed at verifying how this technique could be useful in elderly patients, resolving the severe pain often related to this pathology and letting them recover strength and motion. PATIENTS AND METHODS: This is a retrospective analysis involving 7 cases of elderly men (mean age = 68 y.o.), suffering from severe wrist arthritis and treated with RCPI between 2016 and 2021. RESULTS: All patients reported a return to manual activities between 6 and 12 months after surgery, significantly improving pain. Two patients complained moderate pain under strain at follow-up, with residual difficulty in performing manual tasks. In all cases, an increase of strength and improvement in terms of stiffness was registered. No cases of infections or implant mobilization were reported. CONCLUSIONS: RCPI combined with proximal row carpectomy shows satisfying results in all published studies and it has been confirmed in our series as well. Indications for this procedure should be widened to elderly people, as useful alternatives to more aggressive salvage procedures, such as total prosthesis or arthrodesis. [ABSTRACT FROM AUTHOR]

Published
2022

114. Novae as a Class of Transient X-ray Sources

Author

Mukai, K, Orio, M, and Valle, M. Della

Subjects
Astrophysics
Abstract

Motivated by the recently discovered class of faint (10(exp 34)-10(exp 35) ergs/s) X-ray transients in the Galactic Center region, we investigate the 2-10 keV properties of classical and recurrent novae. Existing data are consistent with the idea that all classical novae are transient X-ray sources with durations of months to years and peak luminosities in the 10(exp 34)-10(exp 35)ergs/s range. This makes classical novae a viable candidate class for the faint Galactic Center transients. We estimate the rate of classical novae within a 15 arcmin radius region centered on the Galactic Center (roughly the field of view of XMM-Newton observations centered on Sgr A*) to be approx.0.1 per year. Therefore, it is plausible that some of the Galactic Center transients that have been announced to date are unrecognized classical novae. The continuing monitoring of the Galactic Center region carried out by Chandra and XMM-Newton may therefore provide a new method to detect classical novae in this crowded and obscured region, an

Published
2007

117. X-ray Observations of the Bright Old Nova V603 Aquilae

Author

Mukai, K and Orio, M

Subjects
Astronomy
Abstract

We report on our Chandra and RXTE observations of the bright old nova, V603 Aql, performed in 2001 April, supplemented by our analysis of archival X-ray data on this object. We find that the RXTE data are contaminated by the Galactic Ridge X-ray emission. After accounting for this effect, we find a high level of aperiodic variability in the RXTE data, at a level consistent with the uncontaminated Chandra data. The Chandra HETG spectrum clearly originates in a multi-temperature plasma. We constrain the possible emission measure distribution of the plasma through a combination of global and local fits. The X-ray luminosity and the spectral shape of V603 Aql resemble those of SS Cyg in transition between quiescence and outburst. The fact that the X-ray flux variability is only weakly energy dependent can be interpreted by supposing that the variability is due to changes in the maximum temperature of the plasma. The plasma density is likely to be high, and the emission region is likely to be compact. Finally, the apparent overabundance of Ne is consistent with V603 Aql being a young system.

Published
2004

123. Multiwavelength observations of nova SMCN 2016-10a -- one of the brightest novae ever observed

Author

Aydi, E., Page, K. L., Kuin, N. P. M., Darnley, M. J., Walter, F. M., Mróz, P., Buckley, D., Mohamed, S., Whitelock, P., Woudt, P., Williams, S. C., Orio, M., Williams, R. E., Beardmore, A. P., Osborne, J. P., Kniazev, A., Ribeiro, V. A. R. M., Udalski, A., Strader, J., Chomiuk, L., Aydi, E., Page, K. L., Kuin, N. P. M., Darnley, M. J., Walter, F. M., Mróz, P., Buckley, D., Mohamed, S., Whitelock, P., Woudt, P., Williams, S. C., Orio, M., Williams, R. E., Beardmore, A. P., Osborne, J. P., Kniazev, A., Ribeiro, V. A. R. M., Udalski, A., Strader, J., and Chomiuk, L.

Abstract

We report on multiwavelength observations of nova SMCN 2016-10a. The present observational set is one of the most comprehensive for any nova in the Small Magellanic Cloud, including: low, medium, and high resolution optical spectroscopy and spectropolarimetry from SALT, FLOYDS, and SOAR; long-term OGLE $V$- and $I$- bands photometry dating back to six years before eruption; SMARTS optical and near-IR photometry from $\sim$ 11 days until over 280 days post-eruption; $Swift$ satellite X-ray and ultraviolet observations from $\sim$ 6 days until 319 days post-eruption. The progenitor system contains a bright disk and a main sequence or a sub-giant secondary. The nova is very fast with $t_2 \simeq$ 4.0 $\pm$ 1.0 d and $t_3 \simeq$ 7.8 $\pm$ 2.0 d in the $V$-band. If the nova is in the SMC, at a distance of $\sim$ 61 $\pm$ 10 kpc, we derive $M_{V,\mathrm{max}} \simeq - 10.5$ $\pm$ 0.5, making it the brightest nova ever discovered in the SMC and one of the brightest on record. At day 5 post-eruption the spectral lines show a He/N spectroscopic class and a FWHM of $\sim$ 3500 kms$^{-1}$ indicating moderately high ejection velocities. The nova entered the nebular phase $\sim$ 20 days post-eruption, predicting the imminent super-soft source turn-on in the X-rays, which started $\sim$ 28 days post-eruption. The super-soft source properties indicate a white dwarf mass between 1.2 M$_{\odot}$ and 1.3 M$_{\odot}$ in good agreement with the optical conclusions.

Published
2018

124. Science with e-ASTROGAM: A space mission for MeV–GeV gamma-ray astrophysics

Author

Angelis, A. De, Tatischeff, V., Grenier, I.A., McEnery, J., Mallamaci, M., Tavani, M., Oberlack, U., Hanlon, L., Walter, R., Argan, A., Ballmoos, P. Von, Bulgarelli, A., Bykov, A., Hernanz, M., Kanbach, G., Kuvvetli, I., Pearce, M., Zdziarski, A., Conrad, J., Ghisellini, G., Harding, A., Isern, J., Leising, M., Longo, F., Madejski, G., Martinez, M., Mazziotta, M.N., Paredes, J.M., Pohl, M., Rando, R., Razzano, M., Aboudan, A., Ackermann, M., Addazi, A., Ajello, M., Albertus, C., Alvarez, J.M., Ambrosi, G., Anton, S., Antonelli, L.A., Babic, A., Baibussinov, B., Balbo, M., Baldini, L., Balman, S., Bambi, C., Almeida, U. Barres de, Barrio, J.A., Bartels, R., Bastieri, D., Bednarek, W., Bernard, D., Bernardini, E., Bernasconi, T., Bertucci, B., Biland, A., Bissaldi, E., Boettcher, M., Bonvicini, V., Bosch-Ramon, V., Bottacini, E., Bozhilov, V., Bretz, T., Branchesi, M., Brdar, V., Bringmann, T., Brogna, A., Budtz-Jørgensen, C., Busetto, G., Buson, S., Busso, M., Caccianiga, A., Camera, S., Campana, R., Caraveo, P., Cardillo, M., Carlson, P., Celestin, S., Cermeno, M., Chen, A., Cheung, C., Churazov, E., Ciprini, S., Coc, A., Colafrancesco, S., Coleiro, A., Collmar, W., Coppi, P., Silva, R. Curado da, Cutini, S., D'Ammando, F., Lotto, B. De, Martino, D. de, Rosa, A. De, Santo, M. Del, Delgado, L., Diehl, R., Dietrich, S., Dolgov, A.D., Dominguez, A., Prester, D. Dominis, Donnarumma, I., Dorner, D., Doro, M., Dutra, M., Elsaesser, D., Fabrizio, M., Fernandez-Barral, A., Fioretti, V., Foffano, L., Formato, V., Fornengo, N., Foschini, L., Franceschini, A., Franckowiak, A., Funk, S., Fuschino, F., Gaggero, D., Galanti, G., Gargano, F., Gasparrini, D., Gehrz, R., Giammaria, P., Giglietto, N., Giommi, P., Giordano, F., Giroletti, M., Ghirlanda, G., Godinovic, N., Gouiffes, C., Grove, J.E., Hamadache, C., Hartmann, D.H., Hayashida, M., Hryczuk, A., Jean, P., Johnson, T., Josae, J., Kaufmann, S., Khelifi, B., Kiener, J., Knodlseder, J., Kole, M., Kopp, J., Kozhuharov, V., Labanti, C., Lalkovski, S., Laurent, P., Limousin, O., Linares, M., Lindfors, E., Lindner, M., Liu, J., Lombardi, S., Loparco, F., Lopez-Coto, R., Moya, M. Lopez, Lott, B., Lubrano, P., Malyshev, D., Mankuzhiyil, N., Mannheim, K., Marcha, M.J., Marciano, A., Marcote, B., Mariotti, M., Marisaldi, M., McBreen, S., Mereghetti, S., Merle, A., Mignani, R., Minervini, G., Moiseev, A., Morselli, A., Moura, F., Nakazawa, K., Nava, L., Nieto, D., Orienti, M., Orio, M., Orlando, E., Orleanski, P., Paiano, S., Paoletti, R., Papitto, A., Pasquato, M., Patricelli, B., Perez-Garcla, M.A., Persic, M., Piano, G., Pichel, A., Pimenta, M., Pittori, C., Porter, T., Poutanen, J., Prandini, E., Prantzos, N., Produit, N., Profumo, S., Queiroz, F.S., Raino, S., Raklev, A., Regis, M., Reichardt, I., Rephaeli, Y., Rico, J., Rodejohann, W., Fernandez, G. Rodriguez, Roncadelli, M., Roso, L., Rovero, A., Ruffini, R., Sala, G., Sanchez-Conde, M.A., Santangelo, A., Parkinson, P. Saz, Sbarrato, T., Shearer, A., Shellard, R., Short, K., Siegert, T., Siqueira, C., Spinelli, P., Stamerra, A., Starrfield, S., Strong, A., Striimke, I., Tavecchio, F., Taverna, R., Terzic, T., Thompson, D.J., Tibolla, O., Torres, D.F., Turolla, R., Ulyanov, A., Ursi, A., Vacchi, A., Abeele, J. Van den, Vankova-Kirilovai, G., Venter, C., Verrecchia, F., Vincent, P., Wang, X., Weniger, C., Wu, X., Zaharijas, G., Zampieri, L., Zane, S., Zimmer, S., Zoglauer, A., Angelis, A. De, Tatischeff, V., Grenier, I.A., McEnery, J., Mallamaci, M., Tavani, M., Oberlack, U., Hanlon, L., Walter, R., Argan, A., Ballmoos, P. Von, Bulgarelli, A., Bykov, A., Hernanz, M., Kanbach, G., Kuvvetli, I., Pearce, M., Zdziarski, A., Conrad, J., Ghisellini, G., Harding, A., Isern, J., Leising, M., Longo, F., Madejski, G., Martinez, M., Mazziotta, M.N., Paredes, J.M., Pohl, M., Rando, R., Razzano, M., Aboudan, A., Ackermann, M., Addazi, A., Ajello, M., Albertus, C., Alvarez, J.M., Ambrosi, G., Anton, S., Antonelli, L.A., Babic, A., Baibussinov, B., Balbo, M., Baldini, L., Balman, S., Bambi, C., Almeida, U. Barres de, Barrio, J.A., Bartels, R., Bastieri, D., Bednarek, W., Bernard, D., Bernardini, E., Bernasconi, T., Bertucci, B., Biland, A., Bissaldi, E., Boettcher, M., Bonvicini, V., Bosch-Ramon, V., Bottacini, E., Bozhilov, V., Bretz, T., Branchesi, M., Brdar, V., Bringmann, T., Brogna, A., Budtz-Jørgensen, C., Busetto, G., Buson, S., Busso, M., Caccianiga, A., Camera, S., Campana, R., Caraveo, P., Cardillo, M., Carlson, P., Celestin, S., Cermeno, M., Chen, A., Cheung, C., Churazov, E., Ciprini, S., Coc, A., Colafrancesco, S., Coleiro, A., Collmar, W., Coppi, P., Silva, R. Curado da, Cutini, S., D'Ammando, F., Lotto, B. De, Martino, D. de, Rosa, A. De, Santo, M. Del, Delgado, L., Diehl, R., Dietrich, S., Dolgov, A.D., Dominguez, A., Prester, D. Dominis, Donnarumma, I., Dorner, D., Doro, M., Dutra, M., Elsaesser, D., Fabrizio, M., Fernandez-Barral, A., Fioretti, V., Foffano, L., Formato, V., Fornengo, N., Foschini, L., Franceschini, A., Franckowiak, A., Funk, S., Fuschino, F., Gaggero, D., Galanti, G., Gargano, F., Gasparrini, D., Gehrz, R., Giammaria, P., Giglietto, N., Giommi, P., Giordano, F., Giroletti, M., Ghirlanda, G., Godinovic, N., Gouiffes, C., Grove, J.E., Hamadache, C., Hartmann, D.H., Hayashida, M., Hryczuk, A., Jean, P., Johnson, T., Josae, J., Kaufmann, S., Khelifi, B., Kiener, J., Knodlseder, J., Kole, M., Kopp, J., Kozhuharov, V., Labanti, C., Lalkovski, S., Laurent, P., Limousin, O., Linares, M., Lindfors, E., Lindner, M., Liu, J., Lombardi, S., Loparco, F., Lopez-Coto, R., Moya, M. Lopez, Lott, B., Lubrano, P., Malyshev, D., Mankuzhiyil, N., Mannheim, K., Marcha, M.J., Marciano, A., Marcote, B., Mariotti, M., Marisaldi, M., McBreen, S., Mereghetti, S., Merle, A., Mignani, R., Minervini, G., Moiseev, A., Morselli, A., Moura, F., Nakazawa, K., Nava, L., Nieto, D., Orienti, M., Orio, M., Orlando, E., Orleanski, P., Paiano, S., Paoletti, R., Papitto, A., Pasquato, M., Patricelli, B., Perez-Garcla, M.A., Persic, M., Piano, G., Pichel, A., Pimenta, M., Pittori, C., Porter, T., Poutanen, J., Prandini, E., Prantzos, N., Produit, N., Profumo, S., Queiroz, F.S., Raino, S., Raklev, A., Regis, M., Reichardt, I., Rephaeli, Y., Rico, J., Rodejohann, W., Fernandez, G. Rodriguez, Roncadelli, M., Roso, L., Rovero, A., Ruffini, R., Sala, G., Sanchez-Conde, M.A., Santangelo, A., Parkinson, P. Saz, Sbarrato, T., Shearer, A., Shellard, R., Short, K., Siegert, T., Siqueira, C., Spinelli, P., Stamerra, A., Starrfield, S., Strong, A., Striimke, I., Tavecchio, F., Taverna, R., Terzic, T., Thompson, D.J., Tibolla, O., Torres, D.F., Turolla, R., Ulyanov, A., Ursi, A., Vacchi, A., Abeele, J. Van den, Vankova-Kirilovai, G., Venter, C., Verrecchia, F., Vincent, P., Wang, X., Weniger, C., Wu, X., Zaharijas, G., Zampieri, L., Zane, S., Zimmer, S., and Zoglauer, A.

Abstract

e-ASTROGAM (‘enhanced ASTROGAM’) is a breakthrough Observatory space mission, with a detector composed by a Silicon tracker, a calorimeter, and an anticoincidence system, dedicated to the study of the non-thermal Universe in the photon energy range from 0.3 MeV to 3 GeV – the lower energy limit can be pushed to energies as low as 150 keV for the tracker, and to 30 keV for calorimetric detection. The mission is based on an advanced space-proven detector technology, with unprecedented sensitivity, angular and energy resolution, combined with polarimetric capability. Thanks to its performance in the MeV-GeV domain, substantially improving its predecessors, e-ASTROGAM will open a new window on the non-thermal Universe, making pioneering observations of the most powerful Galactic and extragalactic sources, elucidating the nature of their relativistic outflows and their effects on the surroundings. With a line sensitivity in the MeV energy range one to two orders of magnitude better than previous generation instruments, e-ASTROGAM will determine the origin of key isotopes fundamental for the understanding of supernova explosion and the chemical evolution of our Galaxy. The mission will provide unique data of significant interest to a broad astronomical community, complementary to powerful observatories such as LIGO-Virgo-GEO600-KAGRA, SKA, ALMA, E-ELT, TMT, LSST, JWST, Athena, CTA, IceCube, KM3NeT, and LISA.

Published
2018

125. AstroSat soft X-ray observations of the symbiotic recurrent nova V3890 Sgr during its 2019 outburst.

Author

Singh, K P, Girish, V, Pavana, M, Ness, Jan-Uwe, Anupama, G C, and Orio, M

Subjects
SOFT X rays, NOVAE (Astronomy), X-ray telescopes, X-ray spectra, THERMAL equilibrium
Abstract

Two long AstroSat Soft X-ray Telescope observations were taken of the third recorded outburst of the symbiotic recurrent nova V3890 Sgr. The first observing run, 8.1–9.9 d after the outburst, initially showed a stable intensity level with a hard X-ray spectrum that we attribute to shocks between the nova ejecta and the pre-existing stellar companion. On day 8.57, the first, weak, signs appeared of supersoft source (SSS) emission powered by residual burning on the surface of the white dwarf. The SSS emission was observed to be highly variable on time-scales of hours. After day 8.9, the SSS component was more stable and brighter. In the second observing run, on days 15.9–19.6 after the outburst, the SSS component was even brighter but still highly variable. The SSS emission was observed to fade significantly during days 16.8–17.8 followed by re-brightening. Meanwhile, the shock component was stable, leading to increase in hardness ratio during the period of fading. AstroSat and XMM–Newton observations have been used to study the spectral properties of V3890 Sgr to draw quantitative conclusions even if their drawback is model dependent. We used the xspec to fit spectral models of plasma emission, and the best fits are consistent with the elemental abundances being lower during the second observing run compared to the first for spectra ≥1 keV. The SSS emission is well fitted by non-local thermal equilibrium model atmosphere used for white dwarfs. The resulting spectral parameters, however, are subject to systematic uncertainties such as completeness of atomic data. [ABSTRACT FROM AUTHOR]

Published
2021
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126. The soft X-ray turnoff of Nova Muscae 1983

Author

Shanley, L, Ogelman, H, Gallagher, J. S, Orio, M, and Krautter, J

Subjects
Astrophysics
Abstract

Nova GQ Muscae 1983 was detected by ROSAT as a luminous 'supersoft' X-ray source in 1992, nearly a decade after outburst. Further, this is the only classical postnova known to have maintained constant luminosity on a timescale predicted by theoretical models. Follow-up observations were made with the ROSAT position-sensitive proportional counter in 1993 January and September, and complemented with B-band photometry taken in 1993 January. By 1993 January, the X-ray count rate had declined by a factor of 17, while there was neither an appreciable decrease in the optical magnitude nor a change in the amplitude of modulation. In 1993 September the soft X-ray flux was below the ROSAT threshold limit, implying a decrease of a factor greater than or equal to 30 in the count rate. This decline can be interpreted by the turnoff of nuclear processes due to the complete consumption of the residual hydrogen-rich envelope. However, the optical luminosity of the system is not simply coupled to the X-ray luminosity (e.g., through reprocessing).

Published
1995
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127. Optical identification of the supersoft X-ray source 1E 0035.4 in the Small Magellanic Cloud

Author

Orio, M, Della Valle, M, Massone, G, and Ogelman, H

Subjects
Astronomy
Abstract

We report the identification of the optical counterpart of the Small Magellanic Cloud (SMC) super-soft X-ray source 1E0035.4- 7230 with a variable star of the magnitude B = 19.9-20.2 within the 40 arcsecs Einstein error box. The star shows strong UV excess, a hot, blue continuum and weak lines of high ionization. The lines are red-shifted by 3-4 A, indicating SMC membership. This object appears similar to CAL 83 and CAL 87 and is probably a binary system hosting an accreting, hydrogen burning white dwarf.

Published
1994

130. Optical observations of ‘hot’ novae returning to quiescence

Author

Zemko, P, primary, Ciroi, S, additional, Orio, M, additional, Odendaal, A, additional, Shugarov, S, additional, Barsukova, E, additional, Bianchini, A, additional, Cracco, V, additional, Gabdeev, M, additional, Goranskij, V, additional, Tofflemire, B, additional, Valeev, A F, additional, and Katysheva, N, additional

Published
2018
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131. What We Learn from the X-Ray Grating Spectra of Nova SMC 2016

Author

Orio, M., primary, Ness, J.-U., additional, Dobrotka, A., additional, Gatuzz, E., additional, Ospina, N., additional, Aydi, E., additional, Behar, E., additional, Buckley, D. A. H., additional, Ciroi, S., additional, Della Valle, M., additional, Hernanz, M., additional, Henze, M., additional, Osborne, J. P., additional, Page, K. L., additional, Rauch, T., additional, Sala, G., additional, Starrfield, S., additional, Williams, R. E., additional, Woodward, C. E., additional, and Zemko, P., additional

Published
2018
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132. Multiwavelength observations of V407 Lupi (ASASSN-16kt) – a very fast nova erupting in an intermediate polar

Author

Aydi, E, primary, Orio, M, additional, Beardmore, A P, additional, Ness, J-U, additional, Page, K L, additional, Kuin, N P M, additional, Walter, F M, additional, Buckley, D A H, additional, Mohamed, S, additional, Whitelock, P, additional, Osborne, J P, additional, Strader, J, additional, Chomiuk, L, additional, Darnley, M J, additional, Dobrotka, A, additional, Kniazev, A, additional, Miszalski, B, additional, Myers, G, additional, Ospina, N, additional, Henze, M, additional, Starrfield, S, additional, and Woodward, C E, additional

Published
2018
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135. Multiwavelength observations of nova SMCN 2016-10a – one of the brightest novae ever observed

Author

Aydi, E, primary, Page, K L, primary, Kuin, N P M, primary, Darnley, M J, primary, Walter, F M, primary, Mróz, P, primary, Buckley, D A H, primary, Mohamed, S, primary, Whitelock, P, primary, Woudt, P, primary, Williams, S C, primary, Orio, M, primary, Williams, R E, primary, Beardmore, A P, primary, Osborne, J P, primary, Kniazev, A, primary, Ribeiro, V A R M, primary, Udalski, A, primary, Strader, J, primary, and Chomiuk, L, primary

Published
2017
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137. Getting unprecedented fast photochromic organic nanoparticles: a challenge solved using bridged hexaarylbiimidazole

Author

Sliwa, M., Debus, B., Ruckebusch, C., Orio, M., Miyasaka, H., Abe, J., Laboratoire Avancé de Spectroscopie pour les Intéractions la Réactivité et l'Environnement - UMR 8516 (LASIRE), Institut de Chimie du CNRS (INC)-Université de Lille-Centre National de la Recherche Scientifique (CNRS)-Centrale Lille Institut (CLIL), Institute of Chemistry, St Petersburg State University (SPbU), Division of Frontier Materials Science, Graduate School of Engineering Science, Osaka University [Osaka], and Institut de Chimie du CNRS (INC)-Université de Lille-Centre National de la Recherche Scientifique (CNRS)

Subjects
[CHIM.THEO]Chemical Sciences/Theoretical and/or physical chemistry
Published
2015

138. Multiset multivariate curve resolution of transient absorption spectroscopy data to model ultrafast photodynamics

Author

Debus, B., Devos, O., Orio, M., Réhault, J., Burdzinski, G., Ruckebusch, C., Sliwa, M., Institute of Chemistry, St Petersburg State University (SPbU), Laboratoire Avancé de Spectroscopie pour les Intéractions la Réactivité et l'Environnement - UMR 8516 (LASIRE), Institut de Chimie du CNRS (INC)-Université de Lille-Centre National de la Recherche Scientifique (CNRS)-Centrale Lille Institut (CLIL), Physikalisch-Chemisches Institut [Zürich], Universität Zürich [Zürich] = University of Zurich (UZH), Faculty of Physics, Adam Mickiewicz University in Poznań (UAM), and Institut de Chimie du CNRS (INC)-Université de Lille-Centre National de la Recherche Scientifique (CNRS)

Subjects
[CHIM.THEO]Chemical Sciences/Theoretical and/or physical chemistry
Published
2015

141. Charge-ordering induces magnetic axes rotation in organic materials (TMTTF)₂X (with X = SbF₆, AsF₆, and PF₆)

Author

Dutoit, C.-E., Bertaina, S., Orio, M., Dressel, M., and Stepanov, A.

Subjects
Кpаткие сообщения, Condensed Matter::Strongly Correlated Electrons
Abstract

We have performed a comprehensive EPR investigation of the quasi-one-dimensional organic systems (TMTTF)₂X with centrosymmetrical anions X (X = SbF₆, AsF₆, and PF₆). We observe a strong rotation of g-factor principal axes when the temperature decreases below charge-ordering temperature TCO. The possible origin of this rotation is analyzed on the basis of quantum chemical calculations performed using density functional theory method. A good agreement between theory and experiment is found.

Published
2015

142. Pan-Chromatic observations of the Recurrent Nova LMC 2009a (LMC 1971b)

Author

Bode, M. F., Darnley, M. J., Beardmore, A. P., Osborne, J. P., Page, K. L., Walter, F. M., Krautter, J., Melandri, A., Ness, J. -U., O'Brien, T. J., Orio, M., Schwarz, G. J., Shara, M. M., Starrfield, S., Bode, M. F., Darnley, M. J., Beardmore, A. P., Osborne, J. P., Page, K. L., Walter, F. M., Krautter, J., Melandri, A., Ness, J. -U., O'Brien, T. J., Orio, M., Schwarz, G. J., Shara, M. M., and Starrfield, S.

Abstract

Nova LMC 2009a is confirmed as a Recurrent Nova (RN) from positional coincidence with nova LMC 1971b. The observational data set is one of the most comprehensive for any Galactic or extragalactic RN: optical and near-IR photometry from outburst until over 6 years later; optical spectra for the first 6 months, and Swift satellite Ultraviolet and X-ray observations from 9 days to almost 1 year post-outburst. We find $M_V = -8.4\pm0.8_{\mathrm{r}}\pm0.7_{\mathrm{s}}$ and expansion velocities between 1000 and 4000 km s$^{-1}$. Coronal line emission before day 9 indicates shocks in the ejecta. Strengthening of He II $\lambda$4686 preceded the emergence of the Super-Soft Source (SSS) in X-rays at $\sim63-70$ days, which was initially very variable. Periodic modulations, $P=1.2$ days, most probably orbital in nature, were evident in the UV and optical from day 43. Subsequently, the SSS shows an oscillation with the same period but with a delay of 0.28P. The progenitor system has been identified; the secondary is most likely a sub-giant feeding a luminous accretion disk. Properties of the SSS infer a white dwarf (WD) mass $1.1 \mathrm{M}_\odot \lesssim M_{\rm WD} \lesssim 1.3 \mathrm{M}_\odot$. If the accretion occurs at constant rate, $\dot{\it{M}}_{\rm acc} \simeq 3.6^{+4.7}_{-2.5} \times 10^{-7} \mathrm{M}_\odot$ yr$^{-1}$ is needed, consistent with nova models for an inter-eruption interval of 38 years, low outburst amplitude, progenitor position in the color-magnitude diagram, and spectral energy distribution at quiescence. We note striking similarities between LMC 2009a and the Galactic nova KT Eri, suggesting that KT Eri is a candidate RN., Comment: 20 pages, 23 figures, accepted for publication in the Astrophysical Journal

Published
2016
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143. Chemical and physical parameters from X-ray high resolution spectra of the Galactic nova V959 Mon

Author

Peretz, U., Orio, M., Behar, E., Bianchini, A., Gallagher, J., Rauch, T., Tofflemire, B., Zemko, P., Peretz, U., Orio, M., Behar, E., Bianchini, A., Gallagher, J., Rauch, T., Tofflemire, B., and Zemko, P.

Abstract

Two observations of V959 Mon, done using the Chandra X-ray gratings during the late outburst phases (2012 September and December), offer extraordinary insight into the physics and chemistry of this Galactic ONe nova. the X-ray flux was 1.7 x 10(-11) erg/cm(2)/s and 8.6 x 10(-12) erg/cm(2)/s, respectively at the two epochs. The first result, coupled with electron density diagnostics and compared with published optical and ultraviolet observations, indicates that most likely in 2012 September the X-rays originate from a very small fraction of the ejecta, concentrated in very dense clumps. We obtained a fairly good fit to the September spectrum with a model of plasma in collisional ionization equilibrium (CIE) with two components; one at a temperature of 0.78 keV, blueshifted by 710-930 km/s, the other at a temperature of 4.5 keV, mostly contributing to the high-energy continuum. However, we cannot rule out a range of plasma temperatures between these two extremes. In December, the central white dwarf (WD) became visible in X-rays. We estimate an effective temperature of about 680,000 K, consistent with a WD mass ~1.1 M(sol). The WD flux is modulated with the orbital period, indicating high inclination, and two quasi-periodic modulations with hour timescales were also observed. No hot plasma component with temperature above 0.5 keV was observed in December, and the blue-shifted component cooled to kT~0.45 keV. Additionally, new emission lines due to a much cooler plasma appeared, which were not observed two months earlier. We estimate abundances and yields of elements in the nova wind that cannot be measured in the optical spectra and confirm the high Ne abundance previously derived for this nova. We also find high abundance of Al, 230 times the solar value, consistently with the prediction that ONe novae contribute to at least 1/3rd of the Galactic yield of Al(26)., Comment: In press, Astrophysical Journal 2016

Published
2016
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144. V4743 Sgr, a magnetic nova?

Author

Zemko, P., Orio, M., Mukai, K., Bianchini, A., Ciroi, S., Cracco, V., Zemko, P., Orio, M., Mukai, K., Bianchini, A., Ciroi, S., and Cracco, V.

Abstract

Two XMM Newton observations of Nova V4743 Sgr (Nova Sgr 2002) were performed shortly after it returned to quiescence, 2 and 3.5 years after the explosion. The X-ray light curves revealed a modulation with a frequency of ~0.75 mHz, indicating that V4743 Sgr is most probably an intermediate polar (IP). The X-ray spectra have characteristics in common with known IPs, with a hard thermal plasma component that can be fitted only assuming a partially covering absorber. In 2004 the X-ray spectrum had also a supersoft blackbody-like component, whose temperature was close to that of the white dwarf (WD) in the supersoft X-ray phase following the outburst, but with flux by at least two orders of magnitude lower. In quiescent IPs, a soft X-ray flux component originates at times in the polar regions irradiated by an accretion column, but the supersoft component of V4743 Sgr disappeared in 2006, indicating a possible origin different from accretion. We suggest that it may have been due to an atmospheric temperature gradient on the WD surface, or to continuing localized thermonuclear burning at the bottom of the envelope, before complete turn-off. An optical spectrum obtained with SALT 11.5 years after the outburst showed a prominent He II 4686A line and the Bowen blend, which reveal a very hot region, but with peak temperature shifted to the ultraviolet (UV) range. V4743 Sgr is the third post-outburst nova and IP candidate showing a low-luminosity supersoft component in the X-ray flux a few years after the outburst., Comment: 9 pages, 5 figures, accepted to MNRAS

Published
2016
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145. The LOFT mission concept: a status update

Author

den Herder, Jan-Willem A., Takahashi, Tadayuki, Bautz, Marshall, Feroci, M., Bozzo, E., Brandt, Søren, Hernanz, M., van der Klis, M., Liu, L.-P., Orleanski, P., Pohl, M., Santangelo, A., Schanne, S., Stella, L., Takahashi, T., Tamura, H., Watts, A., Wilms, J., Zane, S., Bhattacharyya, S., Agudo, I., Ahangarianabhari, M., Albertus, C., Alford, M., Alpar, A., Altamirano, D., Alvarez, L., Amati, L., Amoros, C., Andersson, Niclas, Antonelli, A., Argan, A., Artigue, R., Artigues, B., Atteia, J.-L., Azzarello, P., Bakala, P., Ballantyne, D., Baldazzi, G., Baldo, M., Balman, S., Barbera, M., van Baren, C., Barret, D., Baykal, A., Begelman, M., Behar, O., Belloni, T., Bernardini, F., Bertuccio, G., Bianchi, S., Bianchini, A., Binko, P., Blay, P., Bocchino, F., Bode, M., Bodin, Peter, Bombaci, I., Bonnet Bidaud, J.-M., Boutloukos, S., Bouyjou, F., Bradley, L., Braga, J., Briggs, M. S., Brown, Elliot John, Buballa, M., Bucciantini, N., Burderi, L., Burgay, M., Bursa, M., Budtz-Jørgensen, Carl, Cackett, E., Cadoux, F., Cais, P., Caliandro, G. A., Campana, S., Cao, Xianyi, Capitanio, F., Casares, J., Casella, P., Castro-Tirado, A. J., Cavazzuti, E., Cavechi, Y., Celestin, S., Cerda-Duran, P., Chakrabarty, D., Chamel, N., Château, F., Chen, Y., Chenevez, Jérôme, Chernyakova, M., Coker, J., Cole, R., Collura, A., Coriat, M., Cornelisse, R., Costamante, L., Cros, A., Cui, W., Cumming, A., Cusumano, G., Czerny, B., D'Aì, A., D'Ammando, F., D'Elia, V., Dai, Zhuojun, Del Monte, E., De Luca, A., De Martino, D., Dercksen, J. P. C., De Pasquale, M., De Rosa, A., Del Santo, M., Di Cosimo, S., Degenaar, N., den Herder, J. W., Diebold, S., Di Salvo, T., Dong, Y., Donnarumma, I., Doroshenko, V., Doyle, G., Drake, S. A., Durant, M., Emmanoulopoulos, D., Enoto, T., Erkut, M. H., Esposito, P., Evangelista, Y., Fabian, A., Falanga, M., Favre, Y., Feldman, C., Fender, R., Feng, Huan, Ferrari, V., Ferrigno, C., Finger, M. H., Fraser, G. W., Frericks, M., Fullekrug, M., Fuschino, F., Gabler, M., Galloway, D. K., Gálvez Sanchez, J. L., Gandhi, P., Gao, Z., Garcia-Berro, E., Gendre, B., Gevin, O., Gezari, S., Giles, A. B., Gilfanov, M., Giommi, P., Giovannini, G., Giroletti, M., Gogus, E., Goldwurm, A., Goluchová, K., Götz, D., Gou, L., Gouiffes, C., Grandi, P., Grassi, M., Greiner, J., Grinberg, V., Groot, P., Gschwender, M., Gualtieri, L., Guedel, M., Guidorzi, C., Guy, L., Haas, D., Haensel, P., Hailey, M., Hamuguchi, K., Hansen, Flemming, Hartmann, D. H., Haswell, C. A., Hebeler, K., Heger, A., Hempel, M., Hermsen, W., Homan, J., Hornstrup, Allan, Hudec, R., Huovelin, J., Huppenkothen, D., Inam, S. C., Ingram, A., In't Zand, J. J. M., Israel, G., Iwasawa, K., Izzo, L., Jacobs, H. M., Jetter, F., Johannsen, T., Jenke, P. A., Jonker, P., Josè, J., Kaaret, P., Kalamkar, K., Kalemci, E., Kanbach, G., Karas, V., Karelin, D., Kataria, D., Keek, L., Kennedy, T., Klochkov, D., Kluzniak, W., Koerding, E., Kokkotas, K., Komossa, S., Korpela, S., Kouveliotou, C., Kowalski, A. F., Kreykenbohm, I., Kuiper, L. M., Kunneriath, D., Kurkela, A., Kuvvetli, Irfan, La Franca, F., Labanti, C., Lai, D., Lamb, F. K., Lachaud, C., Laubert, P. P., Lebrun, F., Li, X., Liang, E., Limousin, O., Lin, D., Linares, M., Linder, D., Lodato, G., Longo, F., Lu, F., Lund, Niels, Maccarone, T. J., Macera, D., Maestre, S., Mahmoodifar, S., Maier, D., Malcovati, P., Malzac, J., Malone, C., Mandel, I., Mangano, V., Manousakis, A., Marelli, M., Margueron, J., Marisaldi, M., Markoff, S. B., Markowitz, A., Marinucci, A., Martindale, A., Martínez, G., McHardy, I. M., Medina-Tanco, G., Mehdipour, M., Melatos, A., Mendez, M., Mereghetti, S., Migliari, S., Mignani, R., Michalska, M., Mihara, T., Miller, J. M., Mineo, T., Miniutti, G., Morsink, S., Motch, C., Motta, S., Mouchet, M., Mouret, G., Mulacova, Jana Hanis, Muleri, F., Muñoz-Darias, T., Negueruela, I., Neilsen, J., Neubert, Torsten, Norton, A. J., Nowak, M., Nucita, A., O'Brien, P., Oertel, M., Olsen, Poul Erik Holmdahl, Orienti, M., Orio, M., Orlandini, M., Osborne, J. P., Osten, R., Ozel, F., Pacciani, L., Paerels, F., Paltani, S., Paolillo, M., Papadakis, I., Papitto, A., Paragi, Z., Paredes, J. M., Patruno, A., Paul, B., Pederiva, F., Perinati, E., Pellizzoni, A., Penacchioni, A. V., Peretz, U., Perez, M. A., Perez-Torres, M., Peterson, B. M., Petracek, V., Pittori, C., Pons, J., Portell, J., Possenti, A., Postnov, K., Poutanen, J., Prakash, M., Prandoni, I., Le Provost, H., Psaltis, D., Pye, J., Qu, Jing, Rambaud, D., Ramon, P., Ramsay, G., Rapisarda, M., Rashevski, A., Rashevskaya, I., Ray, P. S., Rea, N., Reddy, S., Reig, P., Reina Aranda, M., Remillard, R., Reynolds, C., Rezzolla, L., Ribo, M., de la Rie, R., Riggio, A., Rios, A., Rischke, D. H., Rodríguez-Gil, P., Rodriguez, J., Rohlfs, R., Romano, P., Rossi, E. M. R., Rozanska, A., Rousseau, A., Rudak, B., Russell, D. M., Ryde, F., Sabau-Graziati, L., Sakamoto, T., Sala, G., Salvaterra, R., Salvetti, D., Sanna, A., Sandberg, J., Savolainen, T., Scaringi, S., Schaffner-Bielich, J., Schatz, H., Schee, J., Schmid, C., Serino, M., Shakura, N., Shore, S., Schnittman, J. D., Schneider, Raphael, Schwenk, A., Schwope, A. D., Sedrakian, A., Seyler, J.-Y., Shearer, A., Slowikowska, A., Sims, M., Smith, P. J., Sobolewska, M., Sochora, V., Soffitta, P., Soleri, P., Song, L., Spencer, A., Stamerra, A., Stappers, B., Staubert, R., Steiner, A. W., Stergioulas, N., Stevens, A. L., Stratta, G., Strohmayer, T. E., Stuchlik, Z., Suchy, S., Suleimanov, V., Tamburini, F., Tauris, T., Tavecchio, F., Tenzer, C., Thielemann, F. K., Tiengo, A., Tolos, L., Tombesi, F., Tomsick, J., Torok, G., Torrejon, J. M., Torres, D. F., Torresi, Elena, Tramacere, A., Traulsen, I., Trois, A., Turolla, R., Turriziani, S., Typel, S., Uter, P., Uttley, P., Vacchi, A., Varniere, P., Vaughan, S., Vercellone, S., Vietri, M., Vincent, F. H., Vrba, V., Walton, D., Wang, Z., Watanabe, Shigeki, Wawrzaszek, R., Webb, N., Weinberg, N., Wende, H., Wheatley, P., Wijers, R., Wijnands, R., Wille, Mads, Wilson-Hodge, C. A., Winter, B., Walk, S. J., Wood, K., Woosley, S. E., Wu, X., Xu, Ruichao, Yu, Wenye, Yuan, Y., Zampa, N., Zampieri, L., Zdunik, L., Zdziarski, A., Zech, A., Zhang, S., Zingale, M., Zwart, F., den Herder, Jan-Willem A., Takahashi, Tadayuki, Bautz, Marshall, Feroci, M., Bozzo, E., Brandt, Søren, Hernanz, M., van der Klis, M., Liu, L.-P., Orleanski, P., Pohl, M., Santangelo, A., Schanne, S., Stella, L., Takahashi, T., Tamura, H., Watts, A., Wilms, J., Zane, S., Bhattacharyya, S., Agudo, I., Ahangarianabhari, M., Albertus, C., Alford, M., Alpar, A., Altamirano, D., Alvarez, L., Amati, L., Amoros, C., Andersson, Niclas, Antonelli, A., Argan, A., Artigue, R., Artigues, B., Atteia, J.-L., Azzarello, P., Bakala, P., Ballantyne, D., Baldazzi, G., Baldo, M., Balman, S., Barbera, M., van Baren, C., Barret, D., Baykal, A., Begelman, M., Behar, O., Belloni, T., Bernardini, F., Bertuccio, G., Bianchi, S., Bianchini, A., Binko, P., Blay, P., Bocchino, F., Bode, M., Bodin, Peter, Bombaci, I., Bonnet Bidaud, J.-M., Boutloukos, S., Bouyjou, F., Bradley, L., Braga, J., Briggs, M. S., Brown, Elliot John, Buballa, M., Bucciantini, N., Burderi, L., Burgay, M., Bursa, M., Budtz-Jørgensen, Carl, Cackett, E., Cadoux, F., Cais, P., Caliandro, G. A., Campana, S., Cao, Xianyi, Capitanio, F., Casares, J., Casella, P., Castro-Tirado, A. J., Cavazzuti, E., Cavechi, Y., Celestin, S., Cerda-Duran, P., Chakrabarty, D., Chamel, N., Château, F., Chen, Y., Chenevez, Jérôme, Chernyakova, M., Coker, J., Cole, R., Collura, A., Coriat, M., Cornelisse, R., Costamante, L., Cros, A., Cui, W., Cumming, A., Cusumano, G., Czerny, B., D'Aì, A., D'Ammando, F., D'Elia, V., Dai, Zhuojun, Del Monte, E., De Luca, A., De Martino, D., Dercksen, J. P. C., De Pasquale, M., De Rosa, A., Del Santo, M., Di Cosimo, S., Degenaar, N., den Herder, J. W., Diebold, S., Di Salvo, T., Dong, Y., Donnarumma, I., Doroshenko, V., Doyle, G., Drake, S. A., Durant, M., Emmanoulopoulos, D., Enoto, T., Erkut, M. H., Esposito, P., Evangelista, Y., Fabian, A., Falanga, M., Favre, Y., Feldman, C., Fender, R., Feng, Huan, Ferrari, V., Ferrigno, C., Finger, M. H., Fraser, G. W., Frericks, M., Fullekrug, M., Fuschino, F., Gabler, M., Galloway, D. K., Gálvez Sanchez, J. L., Gandhi, P., Gao, Z., Garcia-Berro, E., Gendre, B., Gevin, O., Gezari, S., Giles, A. B., Gilfanov, M., Giommi, P., Giovannini, G., Giroletti, M., Gogus, E., Goldwurm, A., Goluchová, K., Götz, D., Gou, L., Gouiffes, C., Grandi, P., Grassi, M., Greiner, J., Grinberg, V., Groot, P., Gschwender, M., Gualtieri, L., Guedel, M., Guidorzi, C., Guy, L., Haas, D., Haensel, P., Hailey, M., Hamuguchi, K., Hansen, Flemming, Hartmann, D. H., Haswell, C. A., Hebeler, K., Heger, A., Hempel, M., Hermsen, W., Homan, J., Hornstrup, Allan, Hudec, R., Huovelin, J., Huppenkothen, D., Inam, S. C., Ingram, A., In't Zand, J. J. M., Israel, G., Iwasawa, K., Izzo, L., Jacobs, H. M., Jetter, F., Johannsen, T., Jenke, P. A., Jonker, P., Josè, J., Kaaret, P., Kalamkar, K., Kalemci, E., Kanbach, G., Karas, V., Karelin, D., Kataria, D., Keek, L., Kennedy, T., Klochkov, D., Kluzniak, W., Koerding, E., Kokkotas, K., Komossa, S., Korpela, S., Kouveliotou, C., Kowalski, A. F., Kreykenbohm, I., Kuiper, L. M., Kunneriath, D., Kurkela, A., Kuvvetli, Irfan, La Franca, F., Labanti, C., Lai, D., Lamb, F. K., Lachaud, C., Laubert, P. P., Lebrun, F., Li, X., Liang, E., Limousin, O., Lin, D., Linares, M., Linder, D., Lodato, G., Longo, F., Lu, F., Lund, Niels, Maccarone, T. J., Macera, D., Maestre, S., Mahmoodifar, S., Maier, D., Malcovati, P., Malzac, J., Malone, C., Mandel, I., Mangano, V., Manousakis, A., Marelli, M., Margueron, J., Marisaldi, M., Markoff, S. B., Markowitz, A., Marinucci, A., Martindale, A., Martínez, G., McHardy, I. M., Medina-Tanco, G., Mehdipour, M., Melatos, A., Mendez, M., Mereghetti, S., Migliari, S., Mignani, R., Michalska, M., Mihara, T., Miller, J. M., Mineo, T., Miniutti, G., Morsink, S., Motch, C., Motta, S., Mouchet, M., Mouret, G., Mulacova, Jana Hanis, Muleri, F., Muñoz-Darias, T., Negueruela, I., Neilsen, J., Neubert, Torsten, Norton, A. J., Nowak, M., Nucita, A., O'Brien, P., Oertel, M., Olsen, Poul Erik Holmdahl, Orienti, M., Orio, M., Orlandini, M., Osborne, J. P., Osten, R., Ozel, F., Pacciani, L., Paerels, F., Paltani, S., Paolillo, M., Papadakis, I., Papitto, A., Paragi, Z., Paredes, J. M., Patruno, A., Paul, B., Pederiva, F., Perinati, E., Pellizzoni, A., Penacchioni, A. V., Peretz, U., Perez, M. A., Perez-Torres, M., Peterson, B. M., Petracek, V., Pittori, C., Pons, J., Portell, J., Possenti, A., Postnov, K., Poutanen, J., Prakash, M., Prandoni, I., Le Provost, H., Psaltis, D., Pye, J., Qu, Jing, Rambaud, D., Ramon, P., Ramsay, G., Rapisarda, M., Rashevski, A., Rashevskaya, I., Ray, P. S., Rea, N., Reddy, S., Reig, P., Reina Aranda, M., Remillard, R., Reynolds, C., Rezzolla, L., Ribo, M., de la Rie, R., Riggio, A., Rios, A., Rischke, D. H., Rodríguez-Gil, P., Rodriguez, J., Rohlfs, R., Romano, P., Rossi, E. M. R., Rozanska, A., Rousseau, A., Rudak, B., Russell, D. M., Ryde, F., Sabau-Graziati, L., Sakamoto, T., Sala, G., Salvaterra, R., Salvetti, D., Sanna, A., Sandberg, J., Savolainen, T., Scaringi, S., Schaffner-Bielich, J., Schatz, H., Schee, J., Schmid, C., Serino, M., Shakura, N., Shore, S., Schnittman, J. D., Schneider, Raphael, Schwenk, A., Schwope, A. D., Sedrakian, A., Seyler, J.-Y., Shearer, A., Slowikowska, A., Sims, M., Smith, P. J., Sobolewska, M., Sochora, V., Soffitta, P., Soleri, P., Song, L., Spencer, A., Stamerra, A., Stappers, B., Staubert, R., Steiner, A. W., Stergioulas, N., Stevens, A. L., Stratta, G., Strohmayer, T. E., Stuchlik, Z., Suchy, S., Suleimanov, V., Tamburini, F., Tauris, T., Tavecchio, F., Tenzer, C., Thielemann, F. K., Tiengo, A., Tolos, L., Tombesi, F., Tomsick, J., Torok, G., Torrejon, J. M., Torres, D. F., Torresi, Elena, Tramacere, A., Traulsen, I., Trois, A., Turolla, R., Turriziani, S., Typel, S., Uter, P., Uttley, P., Vacchi, A., Varniere, P., Vaughan, S., Vercellone, S., Vietri, M., Vincent, F. H., Vrba, V., Walton, D., Wang, Z., Watanabe, Shigeki, Wawrzaszek, R., Webb, N., Weinberg, N., Wende, H., Wheatley, P., Wijers, R., Wijnands, R., Wille, Mads, Wilson-Hodge, C. A., Winter, B., Walk, S. J., Wood, K., Woosley, S. E., Wu, X., Xu, Ruichao, Yu, Wenye, Yuan, Y., Zampa, N., Zampieri, L., Zdunik, L., Zdziarski, A., Zech, A., Zhang, S., Zingale, M., and Zwart, F.

Published
2016

147. RELAP5 simulation of two-phase flow experiments in vertical helical tubes

Author

Casamirra, M, CASTIGLIA, Francesco, GIARDINA, Mariarosa, MORANA, Giuseppe, De Salve, M, Orio, M, Panella, B., Casamirra, M, Castiglia, F, Giardina, M, Morana, G, De Salve, M, Orio, M, and Panella, B

Subjects
relap,helical tubes, two-phase flow, Settore ING-IND/19 - Impianti Nucleari
Abstract

In the framework of the studies concerning the thermalfluid dynamic phenomena in helicoidal pipes of the innovative nuclear reactor IRIS steam generators, the Department of Nuclear Engineering of the University of Palermo in collaboration with the Politecnico di Torino Department of Energetics has been engaged in a work aimed to adapt, by implementing new suitable models, RELAP5/mod3.2.2β code to simulate the thermalfluid-dynamics and geometries such as the ones involved in helicoidal pipes. In fact this code is based on one-dimensional thermal-hydraulic relationships and presents limitations to model complicated geometry such as helicoidal pipes. Therefore the code was improved with additional correlations that are valid for two-phase flow and allow to overcome the drawbacks. The validation work of the models that were added is based on the experimental data carried out at the Politecnico di Torino Department of Energetics. In this paper it will be shown that the so modified RELAP5 code allows to represent adequately the experimental data.

Published
2010

148. Theoretical insight onto ligand radical localization in biomimetic models of galactose oxydase

Author

Orio, M., Laboratoire Avancé de Spectroscopie pour les Intéractions la Réactivité et l'Environnement - UMR 8516 (LASIRE), Institut de Chimie du CNRS (INC)-Université de Lille-Centre National de la Recherche Scientifique (CNRS), and Institut de Chimie du CNRS (INC)-Université de Lille-Centre National de la Recherche Scientifique (CNRS)-Centrale Lille Institut (CLIL)

Subjects
[CHIM.THEO]Chemical Sciences/Theoretical and/or physical chemistry
Published
2014

149. Innovative molecular electrocatalyst for carbon dioxide reduction: experimental and theoretical characterization of a key-intermediate

Author

Duboc, C., Bourrez, M., Sylvie Chardon, Deronzier, A., Vezin, H., Orio, M., Département de Chimie Moléculaire - Chimie Inorganique Redox Biomimétique (DCM - CIRE), Département de Chimie Moléculaire (DCM), Université Joseph Fourier - Grenoble 1 (UJF)-Institut de Chimie du CNRS (INC)-Centre National de la Recherche Scientifique (CNRS)-Université Joseph Fourier - Grenoble 1 (UJF)-Institut de Chimie du CNRS (INC)-Centre National de la Recherche Scientifique (CNRS), Laboratoire Avancé de Spectroscopie pour les Intéractions la Réactivité et l'Environnement - UMR 8516 (LASIRE), Institut de Chimie du CNRS (INC)-Université de Lille-Centre National de la Recherche Scientifique (CNRS)-Centrale Lille Institut (CLIL), Département de Chimie Moléculaire - Chimie Inorganique Redox (DCM - CIRE), and Institut de Chimie du CNRS (INC)-Université de Lille-Centre National de la Recherche Scientifique (CNRS)

Subjects
[CHIM.THEO]Chemical Sciences/Theoretical and/or physical chemistry
Published
2014

150. Radical dissociation/recombination in hexaarylbiimidazoles: NMR and quantum chemical investigation

Author

Delbaere, S., Orio, M., Berthet, J., Hatano, S., Abe, J., Laboratoire Avancé de Spectroscopie pour les Intéractions la Réactivité et l'Environnement - UMR 8516 (LASIRE), Institut de Chimie du CNRS (INC)-Université de Lille-Centre National de la Recherche Scientifique (CNRS)-Centrale Lille Institut (CLIL), Department of Chemistry, School of Science and Engineering, Aoyama Gakuin University (AGU), and Institut de Chimie du CNRS (INC)-Université de Lille-Centre National de la Recherche Scientifique (CNRS)

Subjects
[CHIM.THEO]Chemical Sciences/Theoretical and/or physical chemistry
Published
2014

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