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176 results on '"Zeippen, C. J."'

1. A Quantitative Comparison of Opacities Calculated Using the Distorted- Wave and $\boldsymbol{R}$-Matrix Methods

Author

Delahaye, F., Badnell, N. R., Ballance, C. P., Palmeri, P., Preval, S., Quinet, P., Ramsbottom, C., Smyth, R. T., Turkington, M., and Zeippen, C. J.

Subjects
Astrophysics - Solar and Stellar Astrophysics, Physics - Atomic Physics
Abstract

The present debate on the reliability of astrophysical opacities has reached a new climax with the recent measurements of Fe opacities on the Z-machine at the Sandia National Laboratory \citep{Bailey2015}. To understand the differences between theoretical results, on the one hand, and experiments on the other, as well as the differences among the various theoretical results, detailed comparisons are needed. Many ingredients are involved in the calculation of opacities; deconstructing the whole process and comparing the differences at each step are necessary to quantify their importance and impact on the final results. We present here such a comparison using the two main approaches to calculate the required atomic data, the $R$-Matrix and distorted-wave methods, as well as sets of configurations and coupling schemes to quantify the effects on the opacities for the $Fe\ XVII$ and $Ni\ XIV$ ions., Comment: 10 pages, 2 figures

Published
2018

2. Collision strengths and transition probabilities for Co II infrared forbidden lines

Author

Storey, P. J., Zeippen, C. J., and Sochi, Taha

Subjects
Physics - Atomic Physics, Astrophysics - Solar and Stellar Astrophysics, Physics - Computational Physics
Abstract

We calculate collision strengths and their thermally-averaged Maxwellian values for electron excitation and de-excitation between the fifteen lowest levels of singly-ionised cobalt, Co+, which give rise to emission lines in the near- and mid-infrared. Transition probabilities are also calculated and relative line intensities predicted for conditions typical of supernova ejecta. The diagnostic potential of the 10.52, 15.46 and 14.74 micro-metre transition lines is briefly discussed., Comment: 9 pages, 4 figures, 7 tables

Published
2015
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3. Ipopv2: Photoionization of Ni XIV -- a test case

Author

Delahaye, F., Palmeri, P., Quinet, P., and Zeippen, C. J.

Subjects
Astrophysics - Solar and Stellar Astrophysics, Physics - Atomic Physics
Abstract

Several years ago, M. Asplund and coauthors (2004) proposed a revision of the Solar composition. The use of this new prescription for Solar abundances in standard stellar models generated a strong disagreement between the predictions and the observations of Solar observables. Many claimed that the Standard Solar Model (SSM) was faulty, and more specifically the opacities used in such models. As a result, activities around the stellar opacities were boosted. New experiments (J. Bailey at Sandia on Z-Pinch, The OPAC consortium at LULI200) to measure directly absorbtion coefficients have been realized or are underway. Several theoretical groups (CEA-OPAS, Los Alamos Nat. Lab., CEA-SCORCG, The Opacity Project - The Iron Project (IPOPv2)) have started new sets of calculations using different approaches and codes. While the new results seem to confirm the good quality of the opacities used in SSM, it remains important to improve and complement the data currently available. We present recent results in the case of the photoionization cross sections for Ni XIV (Ni13+ ) from IPOPv2 and possible implications on stellar modelling., Comment: 10 pages, 3 figures, Conf. on New Advances in Stellar Physics: From Microscopic to Macroscopic Processes

Published
2014
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4. Comparison of Fe and Ni opacity calculations for a better understanding of pulsating stellar envelopes

Author

Gilles, D., Turck-Chièze, S., Loisel, G., Piau, L., Ducret, J. -E., Poirier, M., Blenski, T., Thais, F., Blancard, C., Cossé, P., Faussurier, G., Gilleron, F., Pain, J. -C., Porcherot, Q., Guzik, J. A., Kilcrease, D. P., Magee, N. H., Harris, J., Busquet, M., Delahaye, F., Zeippen, C. J., and Bastiani-Ceccotti, S.

Subjects
Astrophysics - Solar and Stellar Astrophysics, Physics - Atomic Physics, Physics - Plasma Physics
Abstract

Opacity is an important ingredient of the evolution of stars. The calculation of opacity coefficients is complicated by the fact that the plasma contains partially ionized heavy ions that contribute to opacity dominated by H and He. Up to now, the astrophysical community has greatly benefited from the work of the contributions of Los Alamos [1], Livermore [2] and the Opacity Project (OP) [3]. However unexplained differences of up to 50% in the radiative forces and Rosseland mean values for Fe have been noticed for conditions corresponding to stellar envelopes. Such uncertainty has a real impact on the understanding of pulsating stellar envelopes, on the excitation of modes, and on the identification of the mode frequencies. Temperature and density conditions equivalent to those found in stars can now be produced in laboratory experiments for various atomic species. Recently the photo-absorption spectra of nickel and iron plasmas have been measured during the LULI 2010 campaign, for temperatures between 15 and 40 eV and densities of ~3 mg/cm3. A large theoretical collaboration, the "OPAC", has been formed to prepare these experiments. We present here the set of opacity calculations performed by eight different groups for conditions relevant to the LULI 2010 experiment and to astrophysical stellar envelope conditions., Comment: 15 pages, 10 figures

Published
2012
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5. Iron and Nickel spectral opacity calculations in conditions relevant for pulsating stellar envelopes and experiments

Author

Gilles, D., Turck-Chièze, S., Busquet, M., Thais, F., Loisel, G., Piau, L., Ducret, J. E., Blenski, T., Blancard, C., Cossé, P., Faussurier, G., Gilleron, F., Pain, J. C., Porcherot, Q., Guzik, J. A., Kilcrease, D. P., Magee, N. H., Harris, J., Bastiani-Ceccotti, S., Delahaye, F., and Zeippen, C. J.

Subjects
Astrophysics - Solar and Stellar Astrophysics, Physics - Atomic Physics, Physics - Plasma Physics
Abstract

Seismology of stars is strongly developing. To address this question we have formed an international collaboration OPAC to perform specific experimental measurements, compare opacity calculations and improve the opacity calculations in the stellar codes [1]. We consider the following opacity codes: SCO, CASSANDRA, STA, OPAS, LEDCOP, OP, SCO-RCG. Their comparison has shown large differences for Fe and Ni in equivalent conditions of envelopes of type II supernova precursors, temperatures between 15 and 40 eV and densities of a few mg/cm3 [2, 3, 4]. LEDCOP, OPAS, SCO-RCG structure codes and STA give similar results and differ from OP ones for the lower temperatures and for spectral interval values [3]. In this work we discuss the role of Configuration Interaction (CI) and the influence of the number of used configurations. We present and include in the opacity code comparisons new HULLAC-v9 calculations [5, 6] that include full CI. To illustrate the importance of this effect we compare different CI approximations (modes) available in HULLAC-v9 [7]. These results are compared to previous predictions and to experimental data. Differences with OP results are discussed., Comment: 4 pages, 3 figures, conference Inertial Fusion Sciences and Applications, Bordeaux, 12th to 16th September 2011; EPJ web of Conferences 2012

Published
2012
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6. Radiative properties of stellar plasmas and open challenges

Author

Turck-Chièze, S., Loisel, G., Gilles, D., Piau, L., Blancard, C., Blenski, T., Busquet, M., Caillaud, T., Cossé, P., Delahaye, F., Faussurier, G., Fariaut, J., Gilleron, F., Guzik, J. A., Harris, J., Kilcrease, D. P., Magee, N. H., Pain, J. C., Porcherot, Q., Poirier, M., Soullier, G., Zeippen, C. J., Bastiani-Ceccotti, S., Reverdin, C., Silvert, V., Thais, F., and Villette, B.

Subjects
Astrophysics - Solar and Stellar Astrophysics, Physics - Plasma Physics
Abstract

The lifetime of solar-like stars, the envelope structure of more massive stars, and stellar acoustic frequencies largely depend on the radiative properties of the stellar plasma. Up to now, these complex quantities have been estimated only theoretically. The development of the powerful tools of helio- and astero- seismology has made it possible to gain insights on the interiors of stars. Consequently, increased emphasis is now placed on knowledge of the monochromatic opacity coefficients. Here we review how these radiative properties play a role, and where they are most important. We then concentrate specifically on the envelopes of $\beta$ Cephei variable stars. We discuss the dispersion of eight different theoretical estimates of the monochromatic opacity spectrum and the challenges we need to face to check these calculations experimentally., Comment: 6 pages, 5 figures, in press (conference HEDLA 2010)

Published
2011
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7. Helioseismic Constraints on the Solar Ne/O Ratio and Heavy Element Abundances

Author

Delahaye, F., Pinsonneault, M. H., Pinsonneault, L., and Zeippen, C. J.

Subjects
Astrophysics - Solar and Stellar Astrophysics
Abstract

We examine the constraints imposed by helioseismic data on the solar heavy element abundances. In prior work we argued that the measured depth of the surface convection zone R_CZ and the surface helium abundance Y_surf were good metallicity indicators which placed separable constraints on light metals (CNONe) and the heavier species with good relative meteoritic abundances. The resulting interiors-based abundance scale was higher than some published studies based on 3D model atmospheres at a highly significant level. In this paper we explore the usage of the solar sound speed in the radiative interior as an additional diagnostic, and find that it is sensitive to changes in the Ne/O ratio even for models constructed to have the same R_CZ and Y_surf. Three distinct helioseismic tests (opacity in the radiative core, ionization in the convection zone, and the core mean molecular weight) yield consistent results. Our preferred O, Ne and Fe abundances are 8.86 +/-0.04, 8.15 +/-0.17 and 7.50 +/-0.05 respectively. They are consistent with the midrange of recently published 3D atmospheric abundances measurements. The values for O, Ne and Fe which combine interiors and atmospheric inferences are 8.83 +/-0.04, 8.08 +/-0.09 and 7.49 +/-0.04 respectively., Comment: 18 pages, 3 figures, submitted to ApJ Letter

Published
2010

8. OPserver: interactive online-computations of opacities and radiative accelerations

Author

Mendoza, C., Seaton, M. J., Buerger, P., Bellorin, A., Melendez, M., Gonzalez, J., Rodriguez, L. S., Delahaye, F., Palacios, E., Pradhan, A. K., and Zeippen, C. J.

Subjects
Astrophysics
Abstract

Codes to compute mean opacities and radiative accelerations for arbitrary chemical mixtures using the Opacity Project recently revised data have been restructured in a client--server architecture and transcribed as a subroutine library. This implementation increases efficiency in stellar modelling where element stratification due to diffusion processes is depth dependent, and thus requires repeated fast opacity reestimates. Three user modes are provided to fit different computing environments, namely a web browser, a local workstation and a distributed grid., Comment: 5 pages, 1 figure

Published
2007
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9. Up-dated opacities from the Opacity Project

Author

Badnell, N. R., Bautista, M. A., Butler, K., Delahaye, F., Mendoza, C., Palmeri, P., Zeippen, C. J., and Seaton, M. J.

Subjects
Astrophysics
Abstract

Using the code AUTOSTRUCTURE, extensive calculations of inner-shell atomic data have been made for the chemical elements He, C, N, O, Ne, Na, Mg, Al, Si, S, Ar, Ca, Cr, Mn, Fe and Ni. The results are used to obtain up-dated opacities from the Opacity Project, OP. A number of other improvements on earlier work have also been included. Rosseland-mean opacities from OP are compared with those from OPAL. Differences of 5 to 10% occur. OP gives the `Z-bump', at log(T)=5.2, to be shifted to slightly higher temperatures. The opacities from OP, as functions of temperature and density, are smoother than those from OPAL. Extensive tests show that the numerical accuracy of the OP opacities following integration over frequency mesh and interpolation on temperature-density mesh is better than 1%. Prior to a number of recent investigations which have indicated a need for a downward revision in the solar abundances of oxygen and other elements, there was good agreement between properties of the sun deduced from helioseismology and from stellar evolution models calculated using OPAL opacities. The revisions in abundances destroy that agreement. In a recent paper Bahcall et al argue that the agreement would be restored if opacities for the regions of the sun between 0.7 and 0.4 solar radii were larger than those given by OPAL by about 10%. In the region concerned, the present results from OP do not differ from those of OPAL by more than 2.5%., Comment: 12 pages, 8 figures, MNRAS At Press. Revised accepted MS. Results unchanged. Revisions: New info on Data Archives, esp. OPserver. Typos corrected etc

Published
2004
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10. Atomic data from the Iron Project.XLIII. Transition probabilities for Fe V

Author

Nahar, Sultana N., Delahaye, Franck, Pradhan, Anil K., and Zeippen, C. J.

Subjects
Astrophysics, Physics - Atomic Physics
Abstract

An extensive set of dipole-allowed, intercombination, and forbidden transition probabilities for Fe V is presented. The Breit-Pauli R-matrix (BPRM) method is used to calculate 1.46 x 10^6 oscillator strengths for the allowed and intercombination E1 transitions among 3,865 fine-structure levels dominated by configuration complexes with n <= 10 and l <= 9. These data are complemented by an atomic structure configuration interaction (CI) calculation using the SUPERSTRUCTURE program for 362 relativistic quadrupole (E2) and magnetic dipole (M1) transitions among 65 low-lying levels dominated by the 3d^4 and 3d^ 4s configurations. Procedures have been developed for the identification of the large number of fine-structure levels and transitions obtained through the BPRM calculations. The target ion Fe VI is represented by an eigenfunction expansion of 19 fine-structure levels of 3d^3 and a set of correlation configurations. Fe V bound levels are obtained with angular and spin symmetries SL\pi and J\pi of the (e + Fe VI) system such that 2S+1 = 5,3,1, L <= 10, J <= 8 of even and odd parities. The completeness of the calculated dataset is verified in terms of all possible bound levels belonging to relevant LS terms and transitions in correspondence with the LS terms. The fine-structure averaged relativistic values are compared with previous Opacity Project LS coupling data and other works. The 362 forbidden transition probabilities considerably extend the available data for the E2 and M1 transtions, and are in good agreement with those computed by Garstang for the 3d^4 transitions., Comment: 19 pages, 1 figure. This paper marks the beginning of a large-scale effort of ab initio atomic calculations that should eventually lead to re-calculation of accurate iron opacities. Astron. Astrophys. Suppl. Ser. (in press)

Published
2000
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13. A quantitative comparison of opacities calculated using the distorted-wave and R-Matrix methods

Author

Delahaye, F., Badnell, N. R., Ballance, C. P., Palmeri, P., Preval, S., Quinet, P., Ramsbottom, C., Smyth, R. T., Turkington, M., Zeippen, C. J., Mendoza, Claudio, Turck-Chieze, Sylvaine, and Colgan, James

Subjects
astro-ph.SR, physics.atom-ph
Abstract

The present debate on the reliability of astrophysical opacities has reached a new climax with the recent measurements of Fe opacities on the Z-machine at the Sandia National Laboratory (Bailey et al 2015). To understand the differences between theoretical results, on the one hand, and experiments on the other, as well as the differences among the various theoretical results, detailed comparisons are needed. Many ingredients are involved in the calculation of opacities; deconstructing the whole process and comparing the differences at each step are necessary to quantify their importance and impact on the final results. We present here such a comparison using the two main approaches to calculate the required atomic data, the R-Matrix and distorted-wave methods, as well as sets of configurations and coupling schemes to quantify the effects on the opacities for the Fe XVII and Ni XIV ions.

Published
2018

15. The virtual atomic and molecular data centre (VAMDC) consortium

Author

Dubernet, M. L., Antony, B. K., Ba, Y. A., Babikov, Yu L., Bartschat, K., Boudon, V., Braams, B. J., Chung, H-K, Daniel, F., Delahaye, F., Del Zanna, G., de Urquijo, J., Dimitrijevic, M. S., Domaracka, A., Doronin, M., Drouin, B. J., Endres, C. P., Fazliev, A. Z., Gagarin, S. V., Gordon, I. E., Gratier, P., Heiter, Ulrike, Hill, C., Jevremovic, D., Joblin, C., Kasprzak, A., Krishnakumar, E., Leto, G., Loboda, P. A., Louge, T., Maclot, S., Marinkovic, B. P., Markwick, A., Marquart, Thomas, Mason, H. E., Mason, N. J., Mendoza, C., Mihajlov, A. A., Millar, T. J., Moreau, N., Mulas, G., Pakhomov, Yu, Palmeri, P., Pancheshnyi, S., Perevalov, V. I., Piskunov, Nikolai, Postler, J., Quinet, P., Quintas-Sanchez, E., Ralchenko, Yu, Rhee, Y-J, Rixon, G., Rothman, L. S., Roueff, E., Ryabchikova, T., Sahal-Brechot, S., Scheier, P., Schlemmer, S., Schmitt, B., Stempels, Eric H. C., Tashkun, S., Tennyson, J., Tyuterev, Vl G., Vujcic, V., Wakelam, V., Walton, N. A., Zatsarinny, O., Zeippen, C. J., Zwoelf, C. M., Dubernet, M. L., Antony, B. K., Ba, Y. A., Babikov, Yu L., Bartschat, K., Boudon, V., Braams, B. J., Chung, H-K, Daniel, F., Delahaye, F., Del Zanna, G., de Urquijo, J., Dimitrijevic, M. S., Domaracka, A., Doronin, M., Drouin, B. J., Endres, C. P., Fazliev, A. Z., Gagarin, S. V., Gordon, I. E., Gratier, P., Heiter, Ulrike, Hill, C., Jevremovic, D., Joblin, C., Kasprzak, A., Krishnakumar, E., Leto, G., Loboda, P. A., Louge, T., Maclot, S., Marinkovic, B. P., Markwick, A., Marquart, Thomas, Mason, H. E., Mason, N. J., Mendoza, C., Mihajlov, A. A., Millar, T. J., Moreau, N., Mulas, G., Pakhomov, Yu, Palmeri, P., Pancheshnyi, S., Perevalov, V. I., Piskunov, Nikolai, Postler, J., Quinet, P., Quintas-Sanchez, E., Ralchenko, Yu, Rhee, Y-J, Rixon, G., Rothman, L. S., Roueff, E., Ryabchikova, T., Sahal-Brechot, S., Scheier, P., Schlemmer, S., Schmitt, B., Stempels, Eric H. C., Tashkun, S., Tennyson, J., Tyuterev, Vl G., Vujcic, V., Wakelam, V., Walton, N. A., Zatsarinny, O., Zeippen, C. J., and Zwoelf, C. M.

Abstract

The Virtual Atomic and Molecular Data Centre (VAMDC) Consortium is a worldwide consortium which federates atomic and molecular databases through an e-science infrastructure and an organisation to support this activity. About 90% of the inter-connected databases handle data that are used for the interpretation of astronomical spectra and for modelling in many fields of astrophysics. Recently the VAMDC Consortium has connected databases from the radiation damage and the plasma communities, as well as promoting the publication of data from Indian institutes. This paper describes how the VAMDC Consortium is organised for the optimal distribution of atomic and molecular data for scientific research. It is noted that the VAMDC Consortium strongly advocates that authors of research papers using data cite the original experimental and theoretical papers as well as the relevant databases.

Published
2016
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16. The virtual atomic and molecular data centre (VAMDC) consortium

Author

Dubernet, M L, primary, Antony, B K, additional, Ba, Y A, additional, Babikov, Yu L, additional, Bartschat, K, additional, Boudon, V, additional, Braams, B J, additional, Chung, H-K, additional, Daniel, F, additional, Delahaye, F, additional, Zanna, G Del, additional, Urquijo, J de, additional, Dimitrijević, M S, additional, Domaracka, A, additional, Doronin, M, additional, Drouin, B J, additional, Endres, C P, additional, Fazliev, A Z, additional, Gagarin, S V, additional, Gordon, I E, additional, Gratier, P, additional, Heiter, U, additional, Hill, C, additional, Jevremović, D, additional, Joblin, C, additional, Kasprzak, A, additional, Krishnakumar, E, additional, Leto, G, additional, Loboda, P A, additional, Louge, T, additional, Maclot, S, additional, Marinković, B P, additional, Markwick, A, additional, Marquart, T, additional, Mason, H E, additional, Mason, N J, additional, Mendoza, C, additional, Mihajlov, A A, additional, Millar, T J, additional, Moreau, N, additional, Mulas, G, additional, Pakhomov, Yu, additional, Palmeri, P, additional, Pancheshnyi, S, additional, Perevalov, V I, additional, Piskunov, N, additional, Postler, J, additional, Quinet, P, additional, Quintas-Sánchez, E, additional, Ralchenko, Yu, additional, Rhee, Y-J, additional, Rixon, G, additional, Rothman, L S, additional, Roueff, E, additional, Ryabchikova, T, additional, Sahal-Bréchot, S, additional, Scheier, P, additional, Schlemmer, S, additional, Schmitt, B, additional, Stempels, E, additional, Tashkun, S, additional, Tennyson, J, additional, Tyuterev, Vl G, additional, Vujčić, V, additional, Wakelam, V, additional, Walton, N A, additional, Zatsarinny, O, additional, Zeippen, C J, additional, and Zwölf, C M, additional

Published
2016
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18. Oxygen in the Universe

Author

Stasińska, G., Prantzos, N., Meynet, G., Simón-Díaz, S., Chiappini, C., Dessauges-Zavadsky, M., Charbonnel, Corinne, Ludwig, H.-G., Mendoza, C., Grevesse, N., Arnould, M., Barbuy, B., Lebreton, Y., Decourchelle, A., Hill, V., Ferrando, P., Hébrard, G., Durret, F., Katsuma, M., Zeippen, C. J., Observatoire Astronomique de l'Université de Genève (ObsGE), Université de Genève (UNIGE), Zentrum für Astronomie der Universität Heidelberg (ZAH), Universität Heidelberg [Heidelberg], Universidad de Los Andes [Venezuela] (ULA), Instituto Venezolano Investigaciones Cientificas, Ctr Fis, Caracas, Instituto Venezolano Investigaciones Cientificas, Université libre de Bruxelles (ULB), Institut de Recherches sur les lois Fondamentales de l'Univers (IRFU), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris-Saclay, APC - Astrophysique des Hautes Energies (APC - AHE), AstroParticule et Cosmologie (APC (UMR_7164)), Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Dipartimento di Astronomia, Universita degli Studi di Bologna, Alma Mater Studiorum Università di Bologna [Bologna] (UNIBO)-Alma Mater Studiorum Università di Bologna [Bologna] (UNIBO), Parizot, Etienne, Université Libre de Bruxelles [Bruxelles] (ULB), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Dipartimento di Astronomia, Universita degli Studi di Bologna, Università di Bologna [Bologna] (UNIBO)-Università di Bologna [Bologna] (UNIBO), Université de Genève = University of Geneva (UNIGE), Universität Heidelberg [Heidelberg] = Heidelberg University, Universidad de Los Andes [Mérida, Venezuela] (ULA), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Observatoire de Paris, and Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS)-Alma Mater Studiorum Università di Bologna [Bologna] (UNIBO)

Subjects
[PHYS.ASTR.HE]Physics [physics]/Astrophysics [astro-ph]/High Energy Astrophysical Phenomena [astro-ph.HE], [PHYS.ASTR.GA]Physics [physics]/Astrophysics [astro-ph]/Galactic Astrophysics [astro-ph.GA], [SDU.ASTR.HE] Sciences of the Universe [physics]/Astrophysics [astro-ph]/High Energy Astrophysical Phenomena [astro-ph.HE], [SDU.ASTR.HE]Sciences of the Universe [physics]/Astrophysics [astro-ph]/High Energy Astrophysical Phenomena [astro-ph.HE], [PHYS.ASTR.GA] Physics [physics]/Astrophysics [astro-ph]/Galactic Astrophysics [astro-ph.GA], [SDU.ASTR.GA]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Galactic Astrophysics [astro-ph.GA], [SDU.ASTR.GA] Sciences of the Universe [physics]/Astrophysics [astro-ph]/Galactic Astrophysics [astro-ph.GA], [PHYS.ASTR.HE] Physics [physics]/Astrophysics [astro-ph]/High Energy Astrophysical Phenomena [astro-ph.HE]
Abstract

ISBN:978-2-7598-0710-9; This book, written by a group of specialists in the different areas involved, summarises what we understand of the production and distribution of oxygen, the most abundant metal in the Universe. After presenting the methods of oxygen abundance determination in various media, it traces a panorama of oxygen in the Universe, describes the mechanisms and sites of oxygen production and finally discusses the chemical evolution of oxygen in different galactic and extragalactic contexts. An appendix thoroughly discusses the oxygen atomic data. This book is intended for the graduate student as well as for the professional astrophysicist. Its aim is to provide the reader with tools for a deeper understanding of the covered topics rather than just to summarise the latest results. Following the thread of oxygen, the reader can gain a diagonal perspective of the realm of stellar, galactic and extragalactic astronomy.

Published
2012

19. Virtual Atomic and Molecular Data Center

Author

Dubernet, M. L., Vincent Boudon, Culhane, J. L., Dimitrijevic, M. S., Fazliev, A. Z., Joblin, C., Kupka, F., Leto, G., Pierre Le Sidaner, Loboda, P. A., Mason, H. E., Mason, N. J., Mendoza, C., Mulas, G., Millar, T. J., Nuñez, L. A., Perevalov, V. I., Piskunov, N., Ralchenko, Y., Rixon, G., Rothman, L. S., Roueff, E., Ryabchikova, T. A., Ryabtsev, A., Sahal-Brechot, S., Bernard Schmitt, Schlemmer, S., Tennyson, J., Tyuterev, Vladimir G., Walton, N. A., Valentine Wakelam, Zeippen, C. J., Laboratoire de Physique Moleculaire pour l'Atmosphere et l'Astrophysique ( LPMAA ), Université Pierre et Marie Curie - Paris 6 ( UPMC ) -Centre National de la Recherche Scientifique ( CNRS ), Laboratoire Univers et Théories ( LUTH ), Institut national des sciences de l'Univers ( INSU - CNRS ) -Observatoire de Paris-Université Paris Diderot - Paris 7 ( UPD7 ) -Centre National de la Recherche Scientifique ( CNRS ), Laboratoire Interdisciplinaire Carnot de Bourgogne ( LICB ), Université de Bourgogne ( UB ) -Centre National de la Recherche Scientifique ( CNRS ), Mullard Space Science Laboratory ( MSSL ), University College of London [London] ( UCL ), Astronomical Observatory Belgrade, V.E. Zuev Institute of Atmospheric Optics ( IAO ), Siberian Branch of the Russian Academy of Sciences ( SB RAS ), Univ Toulouse UPS, Ctr Etud Spatiale Rayonnements, F-31062 Toulouse 9, France, Centre Etud Spatiale Rayonnements Toulouse, University Vienna, Fac Math, Osserv Astrofis Catania, Ist Nazl Astrofis, Observatoire de Paris - Site de Meudon ( OBSPM ), Observatoire de Paris-Centre National de la Recherche Scientifique ( CNRS ), All-Russian Scientific Research Institute of Technical Physics RFNTC VNIITF, Centre for Mathematical Science, Dept Appl Math & Theoret Phys Cambridge, Centre for Mathematical Science, Open university Faculty of Sciences, Universidad de Los Andes Venezuela, CeCalCULA, Corp Parque Tecnol Merida, Ctr Calculo Cient, Universidad de Los Andes Venezuela, Instituto Venezolano Investigaciones Cientificas, Ctr Fis, Caracas, Instituto Venezolano Investigaciones Cientificas, Osservatorio Astronomico di Cagliari, Ist Nazl Astrofis, Osservatorio Astronomico di Cagliari, Queen's UniversityBelfast, Sch Math & Phys, Universidad Industrial de Santander [Bucaramanga] ( UIS ), AMOR 2010, Laboratoire d'astrodynamique, d'astrophysique et d'aéronomie de bordeaux ( L3AB ), Université Sciences et Technologies - Bordeaux 1-Institut national des sciences de l'Univers ( INSU - CNRS ) -Centre National de la Recherche Scientifique ( CNRS ) -Université Sciences et Technologies - Bordeaux 1-Institut national des sciences de l'Univers ( INSU - CNRS ) -Centre National de la Recherche Scientifique ( CNRS ) -Observatoire aquitain des sciences de l'univers ( OASU ), Université Sciences et Technologies - Bordeaux 1-Institut national des sciences de l'Univers ( INSU - CNRS ) -Centre National de la Recherche Scientifique ( CNRS ) -Centre National de la Recherche Scientifique ( CNRS ) -Laboratoire d'Astrophysique de Bordeaux [Pessac] ( LAB ), Université de Bordeaux ( UB ) -Institut national des sciences de l'Univers ( INSU - CNRS ) -Centre National de la Recherche Scientifique ( CNRS ) -Université de Bordeaux ( UB ), Laboratoire de Physique Moleculaire pour l'Atmosphere et l'Astrophysique (LPMAA), Université Pierre et Marie Curie - Paris 6 (UPMC)-Centre National de la Recherche Scientifique (CNRS), Laboratoire Univers et Théories (LUTH (UMR_8102)), Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), Laboratoire Interdisciplinaire Carnot de Bourgogne (ICB), Université de Bourgogne (UB)-Centre National de la Recherche Scientifique (CNRS), Mullard Space Science Laboratory (MSSL), University College of London [London] (UCL), Astronomical Observatory Belgrade (AOB), V.E. Zuev Institute of Atmospheric Optics (IAO), Siberian Branch of the Russian Academy of Sciences (SB RAS), Centre d'étude spatiale des rayonnements (CESR), Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire Midi-Pyrénées (OMP), Institut de Recherche pour le Développement (IRD)-Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Institut de Recherche pour le Développement (IRD)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Centre National de la Recherche Scientifique (CNRS), Observatoire de Paris - Site de Meudon (OBSPM), Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS), Universidad de Los Andes [Mérida, Venezuela] (ULA), INAF - Osservatorio Astronomico di Cagliari (OAC), Istituto Nazionale di Astrofisica (INAF), Queen's University [Belfast] (QUB), Universidad Industrial de Santander [Bucaramanga] (UIS), Laboratoire d'astrodynamique, d'astrophysique et d'aéronomie de bordeaux (L3AB), Université Sciences et Technologies - Bordeaux 1 (UB)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Université Sciences et Technologies - Bordeaux 1 (UB)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Observatoire aquitain des sciences de l'univers (OASU), Université Sciences et Technologies - Bordeaux 1 (UB)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Centre National de la Recherche Scientifique (CNRS)-Laboratoire d'Astrophysique de Bordeaux [Pessac] (LAB), Université de Bordeaux (UB)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Université de Bordeaux (UB), Francois, Francoise, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-Université Paris Diderot - Paris 7 (UPD7), Laboratoire Interdisciplinaire Carnot de Bourgogne (LICB), Universidad de Los Andes [Venezuela] (ULA), Université Sciences et Technologies - Bordeaux 1-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Université Sciences et Technologies - Bordeaux 1-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Observatoire aquitain des sciences de l'univers (OASU), Université Sciences et Technologies - Bordeaux 1-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Centre National de la Recherche Scientifique (CNRS)-Laboratoire d'Astrophysique de Bordeaux [Pessac] (LAB), PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), and PSL Research University (PSL)-PSL Research University (PSL)-Centre National de la Recherche Scientifique (CNRS)

Subjects
[PHYS.ASTR.EP] Physics [physics]/Astrophysics [astro-ph]/Earth and Planetary Astrophysics [astro-ph.EP], [ PHYS.ASTR.EP ] Physics [physics]/Astrophysics [astro-ph]/Earth and Planetary Astrophysics [astro-ph.EP], [PHYS.ASTR.EP]Physics [physics]/Astrophysics [astro-ph]/Earth and Planetary Astrophysics [astro-ph.EP], [SDU.ASTR.EP]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Earth and Planetary Astrophysics [astro-ph.EP], [SDU.ASTR.EP] Sciences of the Universe [physics]/Astrophysics [astro-ph]/Earth and Planetary Astrophysics [astro-ph.EP], [ SDU.ASTR.EP ] Sciences of the Universe [physics]/Astrophysics [astro-ph]/Earth and Planetary Astrophysics [astro-ph.EP]
Abstract

(special issue HighRus2009). VAMDC; International audience

Published
2010

20. Collision strengths and transition probabilities for Co II infrared forbidden lines.

Author

Storey, P. J., Zeippen, C. J., and Sochi, Taha

Subjects
*COLLISIONS (Nuclear physics), *ATOMIC transition probabilities, *THERMAL analysis, *ELECTRONIC excitation, *COBALT compounds, *SUPERNOVAE
Abstract

We calculate collision strengths and their thermally-averaged Maxwellian values for electron excitation and de-excitation between the fifteen lowest levels of singly-ionized cobalt, Co+, which give rise to emission lines in the near- and mid-infrared. Transition probabilities are also calculated and relative line intensities predicted for conditions typical of supernova ejecta. The diagnostic potential of the 10.52, 15.46 and 14.74 μm transition lines is briefly discussed. [ABSTRACT FROM AUTHOR]

Published
2016
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21. Radiative properties of stellar plasmas and open challenges

Author

Turck-Chièze, S., primary, Loisel, G., additional, Gilles, D., additional, Piau, L., additional, Blancard, C., additional, Blenski, T., additional, Busquet, M., additional, Caillaud, T., additional, Cossé, P., additional, Delahaye, F., additional, Faussurier, G., additional, Fariaut, J., additional, Gilleron, F., additional, Guzik, J. A., additional, Harris, J., additional, Kilcrease, D. P., additional, Magee, N. H., additional, Pain, J. C., additional, Porcherot, Q., additional, Poirier, M., additional, Soullier, G., additional, Zeippen, C. J., additional, Bastiani-Ceccotti, S., additional, Reverdin, C., additional, Silvert, V., additional, Thais, F., additional, and Villette, B., additional

Published
2011
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22. VAMDC—The Virtual Atomic and Molecular Data Centre—A New Way to Disseminate Atomic and Molecular Data—VAMDC Level 1 Release

Author

Rixon, G., primary, Dubernet, M. L., additional, Piskunov, N., additional, Walton, N., additional, Mason, N., additional, Le Sidaner, P., additional, Schlemmer, S., additional, Tennyson, J., additional, Akram, A., additional, Benson, K., additional, Bureau, J., additional, Doronin, M., additional, Endres, C., additional, Heiter, U., additional, Hill, C., additional, Kupka, F., additional, Nenadovic, L., additional, Marquart, T., additional, Mulas, G., additional, Ralchenko, Y., additional, Shih, A., additional, Smith, K., additional, Schmitt, B., additional, Witherick, D., additional, Boudon, V., additional, Culhane, J. L., additional, Dimitrijevic, M. S., additional, Fazliev, A. Z., additional, Joblin, C., additional, Leto, G., additional, Loboda, P. A., additional, Mason, H. E., additional, Mendoza, C., additional, Millar, T. J., additional, Nunez, L. A., additional, Perevalov, V. I., additional, Rothman, L. S., additional, Roueff, E., additional, Ryabchikova, T. A., additional, Ryabtsev, A., additional, Sahal-Bréchot, S., additional, Tyuterev, V. G., additional, Wakelam, V., additional, and Zeippen, C. J., additional

Published
2011
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24. Some O I oscillator strengths and the interstellar abundance of oxygen

Author

Zeippen, C. J, Seaton, M. J, and Morton, D. C

Subjects
Astrophysics
Abstract

Calculated and experimental oscillator strengths for the O I intersystem line at 1356 A and for other O I lines of interest in interstellar absorption-line studies are discussed. Attention is given to experimental f-values for the lines at 1302, 1305, and 1306 A, previous work on the f-values for the lines at 1356 and 1359 A, wave-function expansion, and calculations for permitted as well as intercombination lines. Copernicus observations of several interstellar absorption lines due to O I, C II, P II, and Ni II toward Zeta Oph are reported, equivalent widths are determined, and a curve-of-growth analysis is performed for the O I absorption lines. Oscillator strengths are recommended for the far-UV resonance lines of O I, and it is concluded that the oxygen in the interstellar H I regions toward Zeta Oph is depleted by 45% to 69%.

Published
1977

27. The reversible H + H(-) yields H2(v, j) + e(-) reaction - A consistent description of the associative detachment and dissociative attachment processes using the resonant scattering theory

Author

Launay, Jean-Michel, Le Dourneuf, M., Zeippen, C. J., Viel, Alexandra, Observatoire de Paris - Site de Meudon (OBSPM), Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS), Laboratoire d'Etude du Rayonnement et de la Matière en Astrophysique (LERMA), École normale supérieure - Paris (ENS Paris), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université de Cergy Pontoise (UCP), Université Paris-Seine-Université Paris-Seine-Centre National de la Recherche Scientifique (CNRS), and École normale supérieure - Paris (ENS-PSL)

Subjects
[PHYS]Physics [physics], Collisions, Quantum dynamics, Molecular physics, ComputingMilieux_MISCELLANEOUS, [PHYS] Physics [physics]
Abstract

International audience

Published
1991

28. Updated opacities from the Opacity Project

Author

Badnell, N. R., primary, Bautista, M. A., additional, Butler, K., additional, Delahaye, F., additional, Mendoza, C., additional, Palmeri, P., additional, Zeippen, C. J., additional, and Seaton, M. J., additional

Published
2005
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36. Oscillator strengths and radiative transition probabilities from the IRON Project.

Author

Zeippen, C. J.

Subjects
*RADIATIVE transitions, *ATOMIC transition probabilities
Abstract

A short summary is given of the methods used by the IRON Project team in order to supply users of atomic data with reliable oscillator strengths and radiative transition probabilities. Available results and corresponding references are listed. A few cases are discussed briefly with a view to illustrate the progress made and the difficulties encountered. [ABSTRACT FROM AUTHOR]

Published
2000

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