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7 results on '"DOUBLE WHITE-DWARFS"'

1. POSYDON:A General-purpose Population Synthesis Code with Detailed Binary-evolution Simulations

Author

Fragos, Tassos, Andrews, Jeff J., Bavera, Simone S., Berry, Christopher P. L., Coughlin, Scott, Dotter, Aaron, Giri, Prabin, Kalogera, Vicky, Katsaggelos, Aggelos, Kovlakas, Konstantinos, Lalvani, Shamal, Misra, Devina, Srivastava, Philipp M., Qin, Ying, Rocha, Kyle A., Roman-Garza, Jaime, Serra, Juan Gabriel, Stahle, Petter, Sun, Meng, Teng, Xu, Trajcevski, Goce, Tran, Nam Hai, Xing, Zepei, Zapartas, Emmanouil, Zevin, Michael, Fragos, Tassos, Andrews, Jeff J., Bavera, Simone S., Berry, Christopher P. L., Coughlin, Scott, Dotter, Aaron, Giri, Prabin, Kalogera, Vicky, Katsaggelos, Aggelos, Kovlakas, Konstantinos, Lalvani, Shamal, Misra, Devina, Srivastava, Philipp M., Qin, Ying, Rocha, Kyle A., Roman-Garza, Jaime, Serra, Juan Gabriel, Stahle, Petter, Sun, Meng, Teng, Xu, Trajcevski, Goce, Tran, Nam Hai, Xing, Zepei, Zapartas, Emmanouil, and Zevin, Michael

Abstract

Most massive stars are members of a binary or a higher-order stellar system, where the presence of a binary companion can decisively alter their evolution via binary interactions. Interacting binaries are also important astrophysical laboratories for the study of compact objects. Binary population synthesis studies have been used extensively over the last two decades to interpret observations of compact-object binaries and to decipher the physical processes that lead to their formation. Here, we present POSYDON, a novel, publicly available, binary population synthesis code that incorporates full stellar structure and binary-evolution modeling, using the MESA code, throughout the whole evolution of the binaries. The use of POSYDON enables the self-consistent treatment of physical processes in stellar and binary evolution, including: realistic mass-transfer calculations and assessment of stability, internal angular-momentum transport and tides, stellar core sizes, mass-transfer rates, and orbital periods. This paper describes the detailed methodology and implementation of POSYDON, including the assumed physics of stellar and binary evolution, the extensive grids of detailed single- and binary-star models, the postprocessing, classification, and interpolation methods we developed for use with the grids, and the treatment of evolutionary phases that are not based on precalculated grids. The first version of POSYDON targets binaries with massive primary stars (potential progenitors of neutron stars or black holes) at solar metallicity.

Published
2023

2. POSYDON: A General-Purpose Population Synthesis Code with Detailed Binary-Evolution Simulations

Author

Tassos Fragos, Jeff J. Andrews, Simone S. Bavera, Christopher P. L. Berry, Scott Coughlin, Aaron Dotter, Prabin Giri, Vicky Kalogera, Aggelos Katsaggelos, Konstantinos Kovlakas, Shamal Lalvani, Devina Misra, Philipp M. Srivastava, Ying Qin, Kyle A. Rocha, Jaime Román-Garza, Juan Gabriel Serra, Petter Stahle, Meng Sun, Xu Teng, Goce Trajcevski, Nam Hai Tran, Zepei Xing, Emmanouil Zapartas, and Michael Zevin

Subjects
PULSATIONAL PAIR INSTABILITY, FOS: Physical sciences, Astronomy and Astrophysics, BLACK-HOLE BINARIES, EQUATION-OF-STATE, ROTATING MASSIVE STARS, ELECTRON-CAPTURE SUPERNOVAE, SECULAR ORBITAL EVOLUTION, Astrophysics - Solar and Stellar Astrophysics, Space and Planetary Science, Astrophysics::Solar and Stellar Astrophysics, GRAVITATIONAL-WAVE SOURCES, Astrophysics::Earth and Planetary Astrophysics, DOUBLE WHITE-DWARFS, X-RAY BINARIES, COMMON-ENVELOPE EVOLUTION, Astrophysics::Galaxy Astrophysics, Solar and Stellar Astrophysics (astro-ph.SR)
Abstract

Most massive stars are members of a binary or a higher-order stellar systems, where the presence of a binary companion can decisively alter their evolution via binary interactions. Interacting binaries are also important astrophysical laboratories for the study of compact objects. Binary population synthesis studies have been used extensively over the last two decades to interpret observations of compact-object binaries and to decipher the physical processes that lead to their formation. Here, we present POSYDON, a novel, binary population synthesis code that incorporates full stellar-structure and binary-evolution modeling, using the MESA code, throughout the whole evolution of the binaries. The use of POSYDON enables the self-consistent treatment of physical processes in stellar and binary evolution, including: realistic mass-transfer calculations and assessment of stability, internal angular-momentum transport and tides, stellar core sizes, mass-transfer rates and orbital periods. This paper describes the detailed methodology and implementation of POSYDON, including the assumed physics of stellar- and binary-evolution, the extensive grids of detailed single- and binary-star models, the post-processing, classification and interpolation methods we developed for use with the grids, and the treatment of evolutionary phases that are not based on pre-calculated grids. The first version of POSYDON targets binaries with massive primary stars (potential progenitors of neutron stars or black holes) at solar metallicity., Comment: 60 pages, 33 figures, 8 tables, referee's comments addressed. The code and the accompanying documentations and data products are available at https:\\posydon.org

Published
2022
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3. Binary Black Hole Formation with Detailed Modeling: Stable Mass Transfer Leads to Lower Merger Rates

Author

Pablo Marchant, Vicky Kalogera, Christopher P. L. Berry, and Monica Gallegos-Garcia

Subjects
Astrophysics::High Energy Astrophysical Phenomena, Metallicity, Population, FOS: Physical sciences, Binary number, POPULATION SYNTHESIS, Astrophysics, Astronomy & Astrophysics, Orders of magnitude (bit rate), Common envelope, Binary black hole, NEUTRON-STAR, Stellar structure, GRAVITATIONAL-WAVE SOURCES, PRESUPERNOVA EVOLUTION, education, Solar and Stellar Astrophysics (astro-ph.SR), High Energy Astrophysical Phenomena (astro-ph.HE), Physics, education.field_of_study, COSMIC cancer database, Science & Technology, CHEMICALLY HOMOGENEOUS EVOLUTION, Astronomy and Astrophysics, EQUATION-OF-STATE, Astrophysics - Solar and Stellar Astrophysics, Space and Planetary Science, STELLAR EVOLUTION, ASYMPTOTIC GIANT BRANCH, Physical Sciences, Astrophysics - High Energy Astrophysical Phenomena, DOUBLE WHITE-DWARFS, COMMON-ENVELOPE EVOLUTION
Abstract

Rapid binary population synthesis codes are often used to investigate the evolution of compact-object binaries. They typically rely on analytical fits of single-star evolutionary tracks and parameterized models for interactive phases of evolution (e.g., mass-transfer on thermal timescale, determination of dynamical instability, and common envelope) that are crucial to predict the fate of binaries. These processes can be more carefully implemented in stellar structure and evolution codes such as MESA. To assess the impact of such improvements, we compare binary black hole mergers as predicted in models with the rapid binary population synthesis code COSMIC to models ran with MESA simulations through mass transfer and common-envelope treatment. We find that results significantly differ in terms of formation paths, the orbital periods and mass ratios of merging binary black holes, and consequently merger rates. While common-envelope evolution is the dominant formation channel in COSMIC, stable mass transfer dominates in our MESA models. Depending upon the black hole donor mass, and mass-transfer and common-envelope physics, at sub-solar metallicity COSMIC overproduces the number of binary black hole mergers by factors of 2--35 with a significant fraction of them having merger times orders of magnitude shorter than the binary black holes formed when using detailed MESA models. Therefore we find that some binary black hole merger rate predictions from rapid population syntheses of isolated binaries may be overestimated by factors of ~5--500. We conclude that the interpretation of gravitational-wave observations requires the use of detailed treatment of these interactive binary phases., 17 pages (13 main text), 5 figures, ApJ, in press

Published
2021

4. Be X-ray binaries in the SMC as indicators of mass-transfer efficiency

Author

Vinciguerra, Serena, Neijssel, Coenraad J., Vigna-Gomez, Alejandro, Mandel, Ilya, Podsiadlowski, Philipp, Maccarone, Thomas J., Nicholl, Matt, Kingdon, Samuel, Perry, Alice, Salemi, Francesco, Vinciguerra, Serena, Neijssel, Coenraad J., Vigna-Gomez, Alejandro, Mandel, Ilya, Podsiadlowski, Philipp, Maccarone, Thomas J., Nicholl, Matt, Kingdon, Samuel, Perry, Alice, and Salemi, Francesco

Abstract

Be X-ray binaries (BeXRBs) consist of rapidly rotating Be stars with neutron star (NS) companions accreting from the circumstellar emission disc. We compare the observed population of BeXRBs in the Small Magellanic Cloud (SMC) with simulated populations of BeXRB-like systems produced with the COMPAS population synthesis code. We focus on the apparently higher minimal mass of Be stars in BeXRBs than in the Be population at large. Assuming that BeXRBs experienced only dynamically stablemass transfer, theirmass distribution suggests that at least similar to 30 per cent of themass donated by the progenitor of the NS is typically accreted by the B-star companion. We expect these results to affect predictions for the population of double compact object mergers. A convolution of the simulated BeXRB population with the star formation history of the SMC shows that the excess of BeXRBs is most likely explained by this galaxy's burst of star formation similar to 20-40 Myr ago.

Published
2020

5. Be X-ray binaries in the SMC as indicators of mass transfer efficiency

Author

Thomas J. Maccarone, Francesco Salemi, Matt Nicholl, Samuel Kingdon, Philipp Podsiadlowski, Ilya Mandel, Alejandro Vigna-Gómez, Alice Perry, Coenraad J. Neijssel, and Serena Vinciguerra

Subjects
NEUTRINO-DRIVEN EXPLOSIONS, Astrophysics::High Energy Astrophysical Phenomena, Population, FOS: Physical sciences, POPULATION SYNTHESIS, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Compact star, 01 natural sciences, neutron [stars], 0103 physical sciences, data analysis [methods], Astrophysics::Solar and Stellar Astrophysics, STAR-FORMATION CONDITIONS, PRESUPERNOVA EVOLUTION, SMALL-MAGELLANIC-CLOUD, education, 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics, Solar and Stellar Astrophysics (astro-ph.SR), Physics, High Energy Astrophysical Phenomena (astro-ph.HE), FORMATION HISTORY, education.field_of_study, Mass distribution, 010308 nuclear & particles physics, Star formation, SUPERNOVA SIMULATIONS, Be, Astronomy and Astrophysics, emission-line [stars], CLOSE BINARIES, Galaxy, Stars, Neutron star, gravitational waves, Astrophysics - Solar and Stellar Astrophysics, STELLAR EVOLUTION, Space and Planetary Science, evolution [stars], binaries [X-rays], Small Magellanic Cloud, Astrophysics::Earth and Planetary Astrophysics, DOUBLE WHITE-DWARFS, Astrophysics - High Energy Astrophysical Phenomena
Abstract

Be X-ray binaries (BeXRBs) consist of rapidly rotating Be stars with neutron star (NS) companions accreting from the circumstellar emission disc. We compare the observed population of BeXRBs in the Small Magellanic Cloud (SMC) with simulated populations of BeXRB-like systems produced with the compas population synthesis code. We focus on the apparently higher minimal mass of Be stars in BeXRBs than in the Be population at large. Assuming that BeXRBs experienced only dynamically stable mass transfer, their mass distribution suggests that at least $\sim 30{{\ \rm per\ cent}}$ of the mass donated by the progenitor of the NS is typically accreted by the B-star companion. We expect these results to affect predictions for the population of double compact object mergers. A convolution of the simulated BeXRB population with the star formation history of the SMC shows that the excess of BeXRBs is most likely explained by this galaxy’s burst of star formation ∼20–40 Myr ago.

Published
2020
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6. Spectroscopy of the helium-rich binary ES Ceti reveals accretion via a disc and evidence of eclipses

Author

Paul J. Groot, K. Bąkowska, D. Steeghs, Gijs Nelemans, and T. R. Marsh

Subjects
PHASE-RESOLVED SPECTROSCOPY, close [binaries], NOVA, Astronomy, Astrophysics::High Energy Astrophysical Phenomena, FOS: Physical sciences, Binary number, chemistry.chemical_element, POPULATION SYNTHESIS, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, Astronomy & Astrophysics, Computer Science::Digital Libraries, 01 natural sciences, SYSTEMS, 0103 physical sciences, Astrophysics::Solar and Stellar Astrophysics, Spectroscopy, 010303 astronomy & astrophysics, Solar and Stellar Astrophysics (astro-ph.SR), Astrophysics::Galaxy Astrophysics, Helium, white dwarfs, novae, ORBITAL PERIODS, Physics, cataclysmic variables, Science & Technology, 010308 nuclear & particles physics, Astrophysics::Instrumentation and Methods for Astrophysics, White dwarf, Astronomy and Astrophysics, Physics::History of Physics, Accretion (astrophysics), AM, Astrophysics - Solar and Stellar Astrophysics, chemistry, individual: ES Ceti [stars], Space and Planetary Science, Physical Sciences, Astrophysics::Earth and Planetary Astrophysics, DOUBLE WHITE-DWARFS, EMISSION, STARS
Abstract

Amongst the hydrogen-deficient accreting binaries known as the "AM~CVn stars" are three systems with the shortest known orbital periods: HM Cnc (321 s), V407 Vul (569 s) and ES Cet (620 s). These compact binaries are predicted to be strong sources of persistent gravitational wave radiation. HM Cnc and V407 Vul are undergoing direct impact accretion in which matter transferred from their donor hits the accreting white dwarfs directly. ES Cet, is the longest period of the three and is amongst the most luminous AM CVn stars, but it is not known whether it accretes via a disk or direct impact. ES Cet displays strong HeII 4686 line emission, which is sometimes a sign of magnetically-controlled accretion. Peculiarly, although around one third of hydrogen accreting white dwarfs show evidence for magnetism, none have been found amongst helium accretors. We present the results of Magellan and VLT spectroscopic and spectropolarimetric observing campaigns dedicated to ES Cet with the aim of understanding its accretion structure. We find strong variability in our spectra on the 620 s period. The lines show evidence for double-peaked emission, characteristic for an accretion disc, with an additional component associated with the outermost disc, rather than a direct impact, that is broadly consistent with "S"-wave emission from the gas stream/disc impact region. This confirms beyond any doubt that 620\,s is the orbital period of ES Cet. We find no significant circular polarisation (below 0.1 %). The trailed spectra show that ES Cet's outer disc is eclipsed by the mass donor, revealing at the same time that the photometric minimum coincides with the hitherto unrecognised eclipse. ES Cet shows spectroscopic behaviour consistent with accretion via a disc, and is the shortest orbital period eclipsing AM CVn star known., 8 pages, 8 figures, 2 tables, accepted for publication in Astronomy and Astrophysics

Published
2021

7. Low-frequency gravitational-wave science with eLISA/NGO

Author

Edward K. Porter, Alberto Sesana, T. J. Sumner, Pierre Binétruy, Alberto Lobo, Jonathan R. Gair, Monica Colpi, Tyson Littenberg, Ryan N. Lang, Chiara Caprini, Emanuele Berti, Sean T. McWilliams, H. Ward, Bernard F. Schutz, Gijs Nelemans, Robin Stebbins, Marta Volonteri, Pau Amaro-Seoane, Karsten Danzmann, Antoine Petiteau, Antoine Klein, Stefano Vitale, Jean-François Dufaux, Sofiane Aoudia, Michele Vallisneri, Alejandro Bohé, Neil J. Cornish, Philippe Jetzer, Stanislav Babak, Oliver Jennrich, Max Planck Institute for Gravitational Physics (Albert Einstein Institute) (AEI), Max-Planck-Gesellschaft, Institut de Ciencies de l'Espai [Barcelona] (ICE-CSIC), Consejo Superior de Investigaciones Científicas [Madrid] (CSIC), APC - THEORIE, AstroParticule et Cosmologie (APC (UMR_7164)), 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, 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)-Institut für theoretische Physik, Universität Hamburg (UHH)-Universität Hamburg (UHH), Department of Physics and Astronomy [U Mississippi], The University of Mississippi [Oxford], California Institute of Technology (CALTECH), Institut d'Astrophysique de Paris (IAP), Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Institut de Physique Théorique - UMR CNRS 3681 (IPHT), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris-Saclay-Centre National de la Recherche Scientifique (CNRS), Università degli Studi di Milano-Bicocca = University of Milano-Bicocca (UNIMIB), Department of Physics, Montana State University (MSU), Max-Planck-Institut für Gravitationsphysik ( Albert-Einstein-Institut ) (AEI), Laboratoire de Physique Théorique d'Orsay [Orsay] (LPT), Université Paris-Sud - Paris 11 (UP11)-Centre National de la Recherche Scientifique (CNRS), Institute of Astronomy [Cambridge], University of Cambridge [UK] (CAM), Agence Spatiale Européenne = European Space Agency (ESA), Institute of Theoretical Physics, Universität Zürich [Zürich] = University of Zurich (UZH), Washington University in Saint Louis (WUSTL), Maryland Center for Fundamental Physics, Department of Physics [College Park] (UMD), University of Maryland [College Park], University of Maryland System-University of Maryland System-University of Maryland [College Park], University of Maryland System-University of Maryland System, Gravitational Astrophysics Laboratory, NASA Goddard Space Flight Center (GSFC), Princeton University, Department of Astrophysics [Nijmegen], Institute for Mathematics, Astrophysics and Particle Physics (IMAPP), Radboud University [Nijmegen]-Radboud University [Nijmegen], Institute of Astronomy [Leuven], Catholic University of Leuven - Katholieke Universiteit Leuven (KU Leuven), National Institute for Subatomic Physics [Amsterdam] (NIKHEF), APC - Gravitation (APC-Gravitation), 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)-Max-Planck-Institut für Gravitationsphysik ( Albert-Einstein-Institut ) (AEI), Max-Planck-Gesellschaft-Max-Planck-Gesellschaft, Quantum Optics and Laser Science, Blackett Laboratory, Blackett Laboratory, Imperial College London-Imperial College London, Jet Propulsion Laboratory (JPL), NASA-California Institute of Technology (CALTECH), Department of Physics and INFN, University of Trento [Trento], Department of Astronomy [Ann Arbor], University of Michigan [Ann Arbor], University of Michigan System-University of Michigan System, SUPA School of Physics and Astronomy [Glasgow], University of Glasgow, eLISA/NGO, Max Planck Institute for Gravitational Physics, Albert Einstein Institute, Institut de Ciencies de l'Espai [Barcelona] ( ICE-CSIC ), Consejo Superior de Investigaciones Científicas [Spain] ( CSIC ), AstroParticule et Cosmologie ( APC - UMR 7164 ), 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 Diderot - Paris 7 ( UPD7 ) -Commissariat à l'énergie atomique et aux énergies alternatives ( CEA ) -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 Diderot - Paris 7 ( UPD7 ) -Commissariat à l'énergie atomique et aux énergies alternatives ( CEA ) -Institut für theoretische Physik, Universität Hamburg ( UHH ) -Universität Hamburg ( UHH ), California Institute of Technology ( CALTECH ), Institut d'Astrophysique de Paris ( IAP ), Université Pierre et Marie Curie - Paris 6 ( UPMC ) -Institut national des sciences de l'Univers ( INSU - CNRS ) -Centre National de la Recherche Scientifique ( CNRS ), Institut de Physique Théorique - UMR CNRS 3681 ( IPHT ), Commissariat à l'énergie atomique et aux énergies alternatives ( CEA ) -Université Paris-Saclay-Centre National de la Recherche Scientifique ( CNRS ), University of Milano Bicocca, Montana State University ( MSU ), Max-Planck-Institut für Gravitationsphysik ( Albert-Einstein-Institut ), Laboratoire de Physique Théorique d'Orsay [Orsay] ( LPT ), Université Paris-Sud - Paris 11 ( UP11 ) -Centre National de la Recherche Scientifique ( CNRS ), Institute of Astronomy, University of Cambridge [UK] ( CAM ), Agence Spatiale Européenne ( ESA ), European Space Agency ( ESA ), University of Zürich [Zürich] ( UZH ), Washington University in St Louis, NASA Goddard Space Flight Center ( GSFC ), Institute for Mathematics, Astrophysics and Particle Physics ( IMAPP ), Radboud university [Nijmegen]-Radboud university [Nijmegen], Katholieke Universiteit Leuven ( KU Leuven ), Nikhef, APC - Gravitation ( APC-Gravitation ), 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 Diderot - Paris 7 ( UPD7 ) -Commissariat à l'énergie atomique et aux énergies alternatives ( CEA ) -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 Diderot - Paris 7 ( UPD7 ) -Commissariat à l'énergie atomique et aux énergies alternatives ( CEA ) -Max-Planck-Institut für Gravitationsphysik (Albert-Einstein-Institut), Max-Planck-Institut-Max-Planck-Institut, Jet Propulsion Laboratory ( JPL ), NASA-California Institute of Technology ( CALTECH ), Department of Astronomy, Department of Physics and Astronomy [Glasgow], 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)-Institut für theoretische Physik, PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7), PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Max-Planck-Institut für Gravitationsphysik ( Albert-Einstein-Institut ) (AEI), Consejo Superior de Investigaciones Científicas [Spain] (CSIC), Agence Spatiale Européenne (ESA), European Space Agency (ESA), University of Zürich [Zürich] (UZH), National Institute for Subatomic Physics Nikhef [Amsterdam] (NIKHEF), 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), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Pierre et Marie Curie - Paris 6 (UPMC), Amaro Seoane, P, Aoudia, S, Babak, S, Binétruy, P, Berti, E, Bohé, A, Caprini, C, Colpi, M, Cornish, N, Danzmann, K, Dufaux, J, Gair, J, Jennrich, O, Jetzer, P, Klein, A, Lang, R, Lobo, A, Littenberg, T, Mcwilliams, S, Nelemans, G, Petiteau, A, Porter, E, Schutz, B, Sesana, A, Stebbins, R, Sumner, T, Vallisneri, M, Vitale, S, Volonteri, M, Ward, H, University of Zurich, Amaro-Seoane, Pau, Science and Technology Facilities Council (STFC), 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)-Institut für theoretische Physik, Centre National de la Recherche Scientifique (CNRS)-Université Paris-Saclay-Commissariat à l'énergie atomique et aux énergies alternatives (CEA), Università degli Studi di Milano-Bicocca [Milano] (UNIMIB), Centre National de la Recherche Scientifique (CNRS)-Université Paris-Sud - Paris 11 (UP11), and 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)-Max-Planck-Institut für Gravitationsphysik ( Albert-Einstein-Institut ) (AEI)

Subjects
Double white-dwarfs, Massive black-hole, Minute orbital period, Physics and Astronomy (miscellaneous), [SDU.ASTR.CO]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO], Astronomy, Astrophysics, AM CVN Stars, 01 natural sciences, 7. Clean energy, Mathematical Sciences, General Relativity and Quantum Cosmology, Physics, Particles & Fields, Observatory, LISA data stream, 010303 astronomy & astrophysics, media_common, Physics, [PHYS]Physics [physics], Galaxy formation, Dynamical friction, Nuclear & Particles Physics, gravitational waves, [ SDU.ASTR.CO ] Sciences of the Universe [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO], Physical Sciences, [PHYS.GRQC]Physics [physics]/General Relativity and Quantum Cosmology [gr-qc], ComputingMethodologies_DOCUMENTANDTEXTPROCESSING, Astrophysics - Cosmology and Nongalactic Astrophysics, double white dwraf, Common envelope evolution, Cosmology and Nongalactic Astrophysics (astro-ph.CO), General relativity, 530 Physics, media_common.quotation_subject, Astrophysics::High Energy Astrophysical Phenomena, Physics, Multidisciplinary, FOS: Physical sciences, General Relativity and Quantum Cosmology (gr-qc), Astrophysics::Cosmology and Extragalactic Astrophysics, Astronomy & Astrophysics, Galaxy merger, [ PHYS.ASTR.CO ] Physics [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO], [PHYS.ASTR.CO]Physics [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO], FIS/05 - ASTRONOMIA E ASTROFISICA, 0103 physical sciences, 3101 Physics and Astronomy (miscellaneous), Astrophysics::Galaxy Astrophysics, Active galactic nuclei, Science & Technology, 010308 nuclear & particles physics, Gravitational wave, Cosmology and Extragalactic Astrophysics, Spin evolution, Astrophysics - Astrophysics of Galaxies, Galaxy, Universe, massive black hole binarie, Stars, 13. Climate action, Sky, Astrophysics of Galaxies (astro-ph.GA), 10231 Institute for Computational Science, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Galaxy Astrophysics
Abstract

We review the expected science performance of the New Gravitational-Wave Observatory (NGO, a.k.a. eLISA), a mission under study by the European Space Agency for launch in the early 2020s. eLISA will survey the low-frequency gravitational-wave sky (from 0.1 mHz to 1 Hz), detecting and characterizing a broad variety of systems and events throughout the Universe, including the coalescences of massive black holes brought together by galaxy mergers; the inspirals of stellar-mass black holes and compact stars into central galactic black holes; several millions of ultracompact binaries, both detached and mass transferring, in the Galaxy; and possibly unforeseen sources such as the relic gravitational-wave radiation from the early Universe. eLISA's high signal-to-noise measurements will provide new insight into the structure and history of the Universe, and they will test general relativity in its strong-field dynamical regime., Comment: 20 pages, 8 figures, proceedings of the 9th Amaldi Conference on Gravitational Waves. Final journal version. For a longer exposition of the eLISA science case, see http://arxiv.org/abs/1201.3621

Published
2012

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