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948 results on '"Thielemann, F.-K."'

173. The LOFT perspective on neutron star thermonuclear bursts: White paper in support of the mission concept of the large observatory for X-ray timing

Author

in't Zand, J. J.M., primary, Malone, Christopher M., additional, Altamirano, D., additional, Ballantyne, D. R., additional, Bhattacharyya, S., additional, Brown, E. F., additional, Cavecchi, Y., additional, Chakrabarty, D., additional, Chenevez, J., additional, Cumming, A., additional, Degenaar, N., additional, Falanga, M., additional, Galloway, D. K., additional, Heger, A., additional, Jose, J., additional, Keek, L., additional, Linares, M., additional, Mahmoodifar, S., additional, Mendez, M., additional, Miller, M. C., additional, Paerels, F. B. S., additional, Poutanen, J., additional, Rozanska, A., additional, Schatz, H., additional, Serino, M., additional, Strohmayer, T. E., additional, Suleimanov, V. F., additional, Thielemann, F. -K., additional, Watts, A. L., additional, Weinberg, N. N., additional, Woosley, S. E., additional, Yu, W., additional, Zhang, S., additional, and Zingale, M., additional

Published
2015
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174. SUPERNOVAE AND GALACTIC EVOLUTION INDICATORS OF THEIR NUCLEOSYNTHESIS

Author

THIELEMANN, F.-K., primary, ARGAST, D., additional, BRACHWITZ, F., additional, GERHARD, O.E., additional, MARTINEZ-PINEDO, G., additional, SAMLAND, M., additional, HIX, W.R., additional, LIEBENDÖRFER, M., additional, MEZZACAPPA, A., additional, NOMOTO, K., additional, NAKAMURA, T., additional, UMEDA, H., additional, and IWAMOTO, K., additional

Published
2001
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177. Yields from Type Ia Supernovae

Author

Thielemann, F.-K., primary, Brachwitz, F., additional, Nomoto, K., additional, Umeda, H., additional, Iwamoto, K., additional, Langanke, K., additional, Martinez-Pinedo, G., additional, Dean, D. J., additional, Hix, W. R., additional, and Strayer, M. S., additional

Published
2000
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179. Observatory science with eXTP

Author

in ’t Zand, Jean J. M., Bozzo, Enrico, Qu, JinLu, Li, Xiang-Dong, Amati, Lorenzo, Chen, Yang, Donnarumma, Immacolata, Doroshenko, Victor, Drake, Stephen A., Hernanz, Margarita, Jenke, Peter A., Maccarone, Thomas J., Mahmoodifar, Simin, de Martino, Domitilla, De Rosa, Alessandra, Rossi, Elena M., Rowlinson, Antonia, Sala, Gloria, Stratta, Giulia, Tauris, Thomas M., Wilms, Joern, Wu, XueFeng, Zhou, Ping, Agudo, Iván, Altamirano, Diego, Atteia, Jean-Luc, Andersson, Nils A., Baglio, M. Cristina, Ballantyne, David R., Baykal, Altan, Behar, Ehud, Belloni, Tomaso, Bhattacharyya, Sudip, Bianchi, Stefano, Bilous, Anna, Blay, Pere, Braga, João, Brandt, Søren, Brown, Edward F., Bucciantini, Niccolò, Burderi, Luciano, Cackett, Edward M., Campana, Riccardo, Campana, Sergio, Casella, Piergiorgio, Cavecchi, Yuri, Chambers, Frank, Chen, Liang, Chen, Yu-Peng, Chenevez, Jérôme, Chernyakova, Maria, Jin, ChiChuan, Ciolfi, Riccardo, Costantini, Elisa, Cumming, Andrew, D’Aì, Antonino, Dai, Zi-Gao, D’Ammando, Filippo, De Pasquale, Massimiliano, Degenaar, Nathalie, Del Santo, Melania, D’Elia, Valerio, Di Salvo, Tiziana, Doyle, Gerry, Falanga, Maurizio, Fan, XiLong, Ferdman, Robert D., Feroci, Marco, Fraschetti, Federico, Galloway, Duncan K., Gambino, Angelo F., Gandhi, Poshak, Ge, MingYu, Gendre, Bruce, Gill, Ramandeep, Götz, Diego, Gouiffès, Christian, Grandi, Paola, Granot, Jonathan, Güdel, Manuel, Heger, Alexander, Heinke, Craig O., Homan, Jeroen, Iaria, Rosario, Iwasawa, Kazushi, Izzo, Luca, Ji, Long, Jonker, Peter G., José, Jordi, Kaastra, Jelle S., Kalemci, Emrah, Kargaltsev, Oleg, Kawai, Nobuyuki, Keek, Laurens, Komossa, Stefanie, Kreykenbohm, Ingo, Kuiper, Lucien, Kunneriath, Devaky, Li, Gang, Liang, En-Wei, Linares, Manuel, Longo, Francesco, Lu, FangJun, Lutovinov, Alexander A., Malyshev, Denys, Malzac, Julien, Manousakis, Antonios, McHardy, Ian, Mehdipour, Missagh, Men, YunPeng, Méndez, Mariano, Mignani, Roberto P., Mikusincova, Romana, Miller, M. Coleman, Miniutti, Giovanni, Motch, Christian, Nättilä, Joonas, Nardini, Emanuele, Neubert, Torsten, O’Brien, Paul T., Orlandini, Mauro, Osborne, Julian P., Pacciani, Luigi, Paltani, Stéphane, Paolillo, Maurizio, Papadakis, Iossif E., Paul, Biswajit, Pellizzoni, Alberto, Peretz, Uria, Pérez Torres, Miguel A., Perinati, Emanuele, Prescod-Weinstein, Chanda, Reig, Pablo, Riggio, Alessandro, Rodriguez, Jerome, Rodríguez-Gil, Pablo, Romano, Patrizia, Różańska, Agata, Sakamoto, Takanori, Salmi, Tuomo, Salvaterra, Ruben, Sanna, Andrea, Santangelo, Andrea, Savolainen, Tuomas, Schanne, Stéphane, Schatz, Hendrik, Shao, LiJing, Shearer, Andy, Shore, Steven N., Stappers, Ben W., Strohmayer, Tod E., Suleimanov, Valery F., Svoboda, Jir̆í, Thielemann, F.-K., Tombesi, Francesco, Torres, Diego F., Torresi, Eleonora, Turriziani, Sara, Vacchi, Andrea, Vercellone, Stefano, Vink, Jacco, Wang, Jian-Min, Wang, JunFeng, Watts, Anna L., Weng, ShanShan, Weinberg, Nevin N., Wheatley, Peter J., Wijnands, Rudy, Woods, Tyrone E., Woosley, Stan E., Xiong, ShaoLin, Xu, YuPeng, Yan, Zhen, Younes, George, Yu, WenFei, Yuan, Feng, Zampieri, Luca, Zane, Silvia, Zdziarski, Andrzej A., Zhang, Shuang-Nan, Zhang, Shu, Zhang, Shuo, Zhang, Xiao, Zingale, Michael, in ’t Zand, Jean J. M., Bozzo, Enrico, Qu, JinLu, Li, Xiang-Dong, Amati, Lorenzo, Chen, Yang, Donnarumma, Immacolata, Doroshenko, Victor, Drake, Stephen A., Hernanz, Margarita, Jenke, Peter A., Maccarone, Thomas J., Mahmoodifar, Simin, de Martino, Domitilla, De Rosa, Alessandra, Rossi, Elena M., Rowlinson, Antonia, Sala, Gloria, Stratta, Giulia, Tauris, Thomas M., Wilms, Joern, Wu, XueFeng, Zhou, Ping, Agudo, Iván, Altamirano, Diego, Atteia, Jean-Luc, Andersson, Nils A., Baglio, M. Cristina, Ballantyne, David R., Baykal, Altan, Behar, Ehud, Belloni, Tomaso, Bhattacharyya, Sudip, Bianchi, Stefano, Bilous, Anna, Blay, Pere, Braga, João, Brandt, Søren, Brown, Edward F., Bucciantini, Niccolò, Burderi, Luciano, Cackett, Edward M., Campana, Riccardo, Campana, Sergio, Casella, Piergiorgio, Cavecchi, Yuri, Chambers, Frank, Chen, Liang, Chen, Yu-Peng, Chenevez, Jérôme, Chernyakova, Maria, Jin, ChiChuan, Ciolfi, Riccardo, Costantini, Elisa, Cumming, Andrew, D’Aì, Antonino, Dai, Zi-Gao, D’Ammando, Filippo, De Pasquale, Massimiliano, Degenaar, Nathalie, Del Santo, Melania, D’Elia, Valerio, Di Salvo, Tiziana, Doyle, Gerry, Falanga, Maurizio, Fan, XiLong, Ferdman, Robert D., Feroci, Marco, Fraschetti, Federico, Galloway, Duncan K., Gambino, Angelo F., Gandhi, Poshak, Ge, MingYu, Gendre, Bruce, Gill, Ramandeep, Götz, Diego, Gouiffès, Christian, Grandi, Paola, Granot, Jonathan, Güdel, Manuel, Heger, Alexander, Heinke, Craig O., Homan, Jeroen, Iaria, Rosario, Iwasawa, Kazushi, Izzo, Luca, Ji, Long, Jonker, Peter G., José, Jordi, Kaastra, Jelle S., Kalemci, Emrah, Kargaltsev, Oleg, Kawai, Nobuyuki, Keek, Laurens, Komossa, Stefanie, Kreykenbohm, Ingo, Kuiper, Lucien, Kunneriath, Devaky, Li, Gang, Liang, En-Wei, Linares, Manuel, Longo, Francesco, Lu, FangJun, Lutovinov, Alexander A., Malyshev, Denys, Malzac, Julien, Manousakis, Antonios, McHardy, Ian, Mehdipour, Missagh, Men, YunPeng, Méndez, Mariano, Mignani, Roberto P., Mikusincova, Romana, Miller, M. Coleman, Miniutti, Giovanni, Motch, Christian, Nättilä, Joonas, Nardini, Emanuele, Neubert, Torsten, O’Brien, Paul T., Orlandini, Mauro, Osborne, Julian P., Pacciani, Luigi, Paltani, Stéphane, Paolillo, Maurizio, Papadakis, Iossif E., Paul, Biswajit, Pellizzoni, Alberto, Peretz, Uria, Pérez Torres, Miguel A., Perinati, Emanuele, Prescod-Weinstein, Chanda, Reig, Pablo, Riggio, Alessandro, Rodriguez, Jerome, Rodríguez-Gil, Pablo, Romano, Patrizia, Różańska, Agata, Sakamoto, Takanori, Salmi, Tuomo, Salvaterra, Ruben, Sanna, Andrea, Santangelo, Andrea, Savolainen, Tuomas, Schanne, Stéphane, Schatz, Hendrik, Shao, LiJing, Shearer, Andy, Shore, Steven N., Stappers, Ben W., Strohmayer, Tod E., Suleimanov, Valery F., Svoboda, Jir̆í, Thielemann, F.-K., Tombesi, Francesco, Torres, Diego F., Torresi, Eleonora, Turriziani, Sara, Vacchi, Andrea, Vercellone, Stefano, Vink, Jacco, Wang, Jian-Min, Wang, JunFeng, Watts, Anna L., Weng, ShanShan, Weinberg, Nevin N., Wheatley, Peter J., Wijnands, Rudy, Woods, Tyrone E., Woosley, Stan E., Xiong, ShaoLin, Xu, YuPeng, Yan, Zhen, Younes, George, Yu, WenFei, Yuan, Feng, Zampieri, Luca, Zane, Silvia, Zdziarski, Andrzej A., Zhang, Shuang-Nan, Zhang, Shu, Zhang, Shuo, Zhang, Xiao, and Zingale, Michael

Abstract

In this White Paper we present the potential of the enhanced X-ray Timing and Polarimetry (eXTP) mission for studies related to Observatory Science targets. These include flaring stars, supernova remnants, accreting white dwarfs, low and high mass X-ray binaries, radio quiet and radio loud active galactic nuclei, tidal disruption events, and gamma-ray bursts. eXTP will be excellently suited to study one common aspect of these objects: their often transient nature. Developed by an international Consortium led by the Institute of High Energy Physics of the Chinese Academy of Science, the eXTP mission is expected to be launched in the mid 2020s.

Published
2019

181. NUCLEOSYNTHESIS AND STELLAR EVOLUTION

Author

Thielemann, F.-K., Argast, D., Brachwitz, F., Martinez-Pinedo, G., Rauscher, T., Liebendörfer, M., Mezzacappa, A., Höflich, P., and Nomoto, K.

Published
2002

192. Simplifying silicon burning: Application of quasi-equilibrium to (alpha) network nucleosynthesis

Author

Hix, W. R, Thielemann, F.-K, Khokhlov, A. M, and Wheeler, J. C

Subjects
Astrophysics
Abstract

While the need for accurate calculation of nucleosynthesis and the resulting rate of thermonuclear energy release within hydrodynamic models of stars and supernovae is clear, the computational expense of these nucleosynthesis calculations often force a compromise in accuracy to reduce the computational cost. To redress this trade-off of accuracy for speed, the authors present an improved nuclear network which takes advantage of quasi- equilibrium in order to reduce the number of independent nuclei, and hence the computational cost of nucleosynthesis, without significant reduction in accuracy. In this paper they will discuss the first application of this method, the further reduction in size of the minimal alpha network. The resultant QSE- reduced alpha network is twice as fast as the conventional alpha network it replaces and requires the tracking of half as many abundance variables, while accurately estimating the rate of energy generation. Such reduction in cost is particularly necessary for future generation of multi-dimensional models for supernovae.

Published
1997

197. Mn abundances in the stars of the Galactic disc with metallicities −1.0 < [Fe/H] < 0.3

Author

Mishenina, T., Gorbaneva, T., Pignatari, M., Thielemann, F.-K, and Korotin, S. A.

Abstract

In this work, we present and discuss the observations of the Mn abundances for 247 FGK dwarfs, located in the Galactic disc with metallicity −1 < [Fe/H] < +0.3. The observed stars belong to the substructures of the Galaxy thick and thin disks, and to the Hercules stream. The observations were conducted using the 1.93m telescope at Observatoire de Haute-Provence (OHP, France) equipped with the echelle-type spectrographs ELODIE and SOPHIE. The abundances were derived under the LTE approximation, with an average error for the [Mn/Fe] ratio of 0.10 dex. For most of the stars in the sample, Mn abundances are not available in the literature. We obtain an evolution of [Mn/Fe] ratio with the metallicity [Fe/H] consistent with previous data compilations. In particular, within the metallicity range covered by our stellar sample, the [Mn/Fe] ratio is increasing with the increase of metallicity. This due to the contribution to the Galactic chemical evolution of Mn and Fe from thermonuclear supernovae. We confirm the baseline scenario where most of the Mn in the Galactic disc and in the Sun is made by thermonuclear supernovae. In particular, the effective contribution from core-collapse supernovae to the Mn in the Solar system is about 10-20 per cent. However, present uncertainties affecting the production of Mn and Fe in thermonuclear supernovae are limiting the constraining power of the observed [Mn/Fe] trend in the Galactic discs on, e.g. the frequency of different thermonuclear supernovae populations. The different production of these two elements in different types of thermonuclear supernovae needs to be disentangled by the dependence of their relative production on the metallicity of the supernova progenitor

Published
2017

198. Numerical aspects of low Mach number flows in astrophysics: preconditioning techniques

Author

Hujeirat, A. A. and Thielemann, F.-K

Subjects
Physics::Fluid Dynamics
Abstract

Internal flows inside gravitationally stable astrophysical objects, such as the Sun, normal and compact stars, are rotating, highly compressed and extremely subsonic. Such low Mach number flows are usually encountered when studying, for example, the dynamo action in stars and planets or the nuclear burst on neutron stars and white dwarfs. Handling of such flows numerically on time-scales longer than the dynamical one is complicated and challenging. The aim of this paper is to address the numerical problems associated with the modelling of internal quasi-stationary, rotating low Mach number flows in stars and to discuss possible solution scenarios. It is shown that the quasi-symmetric approximate factorization method (AFM) as a pre-conditioner within a non-linear Newton-type defect-correction solution procedure is best suited for modelling quasi-stationary weakly compressible flows with moderate low Mach numbers. This method is robust as it can be applied to model time-dependent compressible flows without further modifications. The AFM-pre-conditioning techniques are shown to be extendable into three dimensions with an arbitrary equation of state. Classical dimensional splitting techniques, however, such as the alternating direction implicit or line-Gauss-Seidel methods are not suited for modelling compressible low Mach number flows. It is also argued that hot and low Mach number astrophysical flows cannot be considered as an asymptotic limit of incompressible flows, but rather as highly compressed flows with extremely stiff pressure terms. We show that, unlike the pseudo-pressure in incompressible fluids, a Poisson-like treatment for the pressure would smooth unnecessarily physically induced acoustic perturbations, thereby violating the conservation of the total energy. Results of several hydrodynamical calculations are presented, which demonstrate the capability of the solver to search for solutions, that correspond to stationary, viscous and rotating flows with a Mach number as small as as well as to fluid flows that are subject to ultra-strong Newtonian and general relativistic gravitational fields

Published
2017

199. Boron depletion in 9 to 15 M stars with rotation

Author

Frischknecht, U., Hirschi, R., Meynet, G., Ekström, S., Georgy, C., Rauscher, T., Winteler, C., and Thielemann, F.-K

Subjects
Astrophysics::Solar and Stellar Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics::Galaxy Astrophysics
Abstract

The treatment of mixing is still one of the major uncertainties in stellar evolution models. One open question is how well the prescriptions for rotational mixing describe the real effects. We tested the mixing prescriptions included in the Geneva stellar evolution code (GENEC) by following the evolution of surface abundances of light isotopes in massive stars, such as boron and nitrogen. We followed 9, 12 and 15 M models with rotation from the zero age main sequence up to the end of He burning. The calculations show the expected behaviour with faster depletion of boron for faster rotating stars and more massive stars. The mixing at the surface is more efficient than predicted by prescriptions used in other codes and reproduces the majority of observations very well. However two observed stars with strong boron depletion but no nitrogen enrichment still can not be explained and let the question open whether additional mixing processes are acting in these massive stars

Published
2017

200. Shock waves and nucleosynthesis in type II supernovae

Author

Aufderheide, M. B, Baron, E, and Thielemann, F.-K

Subjects
Astrophysics
Abstract

In the study of nucleosynthesis in type II SN, shock waves are initiated artificially, since collapse calculations do not, as yet, give self-consistent shock waves strong enough to produce the SN explosion. The two initiation methods currently used by light-curve modelers are studied, with a focus on the peak temperatures and the nucleosynthetic yields in each method. The various parameters involved in artificially initiating a shock wave and the effects of varying these parameters are discussed.

Published
1991
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