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1. The Gravitational Universe

Author

Consortium, The ELISA, Seoane, P. Amaro, Aoudia, S., Audley, H., Auger, G., Babak, S., Baker, J., Barausse, E., Barke, S., Bassan, M., Beckmann, V., Benacquista, M., Bender, P. L., Berti, E., Binétruy, P., Bogenstahl, J., Bonvin, C., Bortoluzzi, D., Brause, N. C., Brossard, J., Buchman, S., Bykov, I., Camp, J., Caprini, C., Cavalleri, A., Cerdonio, M., Ciani, G., Colpi, M., Congedo, G., Conklin, J., Cornish, N., Danzmann, K., De Vine, G., Debra, D., Freitag, M. Dewi, Di Fiore, L., Aguilo, M. Diaz, Diepholz, I., Dolesi, R., Dotti, M., Barranco, G. Fernández, Ferraioli, L., Ferroni, V., Finetti, N., Fitzsimons, E., Gair, J., Galeazzi, F., Garcia, A., Gerberding, O., Gesa, L., Giardini, D., Gibert, F., Grimani, C., Groot, P., Cervantes, F. Guzman, Haiman, Z., Halloin, H., Heinzel, G., Hogan, C., Holz, D., Hornstrup, A., Hoyland, D., Hoyle, C. D., Hueller, M., Hughes, S., Jetzer, P., Kalogera, V., Karnesis, N., Kilic, M., Killow, C., Klipstein, W., Kochkina, E., Korsakova, N., Krolak, A., Larson, S., Lieser, M., Littenberg, T., Livas, J., Lloro, I., Mance, D., Madau, P., Maghami, P., Mahrdt, C., Marsh, T., Mateos, I., Mayer, L., McClelland, D., Mckenzie, K., McWilliams, S., Merkowitz, S., Miller, Christian, Mitryk, S., Moerschell, J., Mohanty, S., Monsky, A., Mueller, G., MÜller, V., Nelemans, G., Nicolodi, D., Nissanke, S., Nofrarias, M., Numata, K., Ohme, F., Otto, M., Perreur-Lloyd, M., Petiteau, A., Phinney, E. S., Plagnol, E., Pollack, S., Porter, E.K., Prat, P., Preston, A., Prince, T., Reiche, J., Richstone, D., Robertson, D., Rossi, E. M., Rosswog, S., Rubbo, L., Ruiter, A., Sanjuan, J., Sathyaprakash, B. S., Schlamminger, S., Schutz, B., Schütze, D., Sesana, A., Shaddock, D., Shah, S., Sheard, B., Sopuerta, C. F., Spector, A., Spero, R., Stanga, R., Stebbins, R., Stede, G., Steier, F., Sumner, T., Sun, K. -X., Sutton, A., Tanaka, T., Tanner, D., Thorpe, I., Tröbs, M., Tinto, M., Tu, H. -B., Vallisneri, M., Vetrugno, D., Vitale, S., Volonteri, M., Wand, V., Wang, Y., Wanner, G., Ward, H., Ware, B., Wass, P., Weber, W. J., Yu, Y., Yunes, N., Zweifel, P., APC - Cosmologie, 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), APC - Astrophysique des Hautes Energies (APC - AHE), 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), APC - THEORIE, 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), Institute for Problems of Material Science, National Academy of Sciences of Ukraine (NASU), 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), Centre d'Etude de Saclay, Commissariat à l'énergie atomique et aux énergies alternatives (CEA), Laboratoire de Météorologie Dynamique (UMR 8539) (LMD), Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-École polytechnique (X)-École des Ponts ParisTech (ENPC)-Centre National de la Recherche Scientifique (CNRS)-Département des Géosciences - ENS Paris, École normale supérieure - Paris (ENS-PSL), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-École normale supérieure - Paris (ENS-PSL), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL), School of Environmental Sciences [Norwich], University of East Anglia [Norwich] (UEA), Department of Physics, University of Warwick [Coventry], Max-Planck-Institut für Gravitationsphysik ( Albert-Einstein-Institut ) (AEI), Max-Planck-Gesellschaft, 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, Max Planck Institute for Gravitational Physics (Albert Einstein Institute) (AEI), School of Earth and Atmospheric Sciences [Atlanta], Georgia Institute of Technology [Atlanta], 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), Institute of High Energy Physics (IHEP), Chinese Academy of Sciences [Changchun Branch] (CAS), Princeton University, Leibniz Universität Hannover, eLISA, 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), 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), 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, Département des Géosciences - ENS Paris, École normale supérieure - Paris (ENS Paris), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-École normale supérieure - Paris (ENS Paris), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-École des Ponts ParisTech (ENPC)-École polytechnique (X)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Pierre et Marie Curie - Paris 6 (UPMC), 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), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Pierre et Marie Curie - Paris 6 (UPMC), Physique Corpusculaire et Cosmologie - Collège de France (PCC), Collège de France (CdF)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-Collège de France (CdF)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-AstroParticule et Cosmologie (APC (UMR_7164)), 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)-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), 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), PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Institut für theoretische Physik, Centre National de la Recherche Scientifique (CNRS)-Université Paris-Saclay-Commissariat à l'énergie atomique et aux énergies alternatives (CEA), École normale supérieure - Paris (ENS Paris)-École normale supérieure - Paris (ENS Paris), PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Max-Planck-Institut für Gravitationsphysik ( Albert-Einstein-Institut ) (AEI), and Albert Einstein Institute

Subjects
General Relativity and Quantum Cosmology, [PHYS.GRQC]Physics [physics]/General Relativity and Quantum Cosmology [gr-qc], Astrophysics::Cosmology and Extragalactic Astrophysics
Abstract

20 pages; submitted to the European Space Agency on May 24th, 2013 for the L2/L3 selection of ESA's Cosmic Vision program; The last century has seen enormous progress in our understanding of the Universe. We know the life cycles of stars, the structure of galaxies, the remnants of the big bang, and have a general understanding of how the Universe evolved. We have come remarkably far using electromagnetic radiation as our tool for observing the Universe. However, gravity is the engine behind many of the processes in the Universe, and much of its action is dark. Opening a gravitational window on the Universe will let us go further than any alternative. Gravity has its own messenger: Gravitational waves, ripples in the fabric of spacetime. They travel essentially undisturbed and let us peer deep into the formation of the first seed black holes, exploring redshifts as large as z ~ 20, prior to the epoch of cosmic re-ionisation. Exquisite and unprecedented measurements of black hole masses and spins will make it possible to trace the history of black holes across all stages of galaxy evolution, and at the same time constrain any deviation from the Kerr metric of General Relativity. eLISA will be the first ever mission to study the entire Universe with gravitational waves. eLISA is an all-sky monitor and will offer a wide view of a dynamic cosmos using gravitational waves as new and unique messengers to unveil The Gravitational Universe. It provides the closest ever view of the early processes at TeV energies, has guaranteed sources in the form of verification binaries in the Milky Way, and can probe the entire Universe, from its smallest scales around singularities and black holes, all the way to cosmological dimensions.

Published
2013

2. Finding and Using Electromagnetic Counterparts of Gravitational Wave Sources

Author

Phinney, E. S.

Subjects
High Energy Astrophysical Phenomena (astro-ph.HE), General Relativity and Quantum Cosmology, Cosmology and Nongalactic Astrophysics (astro-ph.CO), Astrophysics::Instrumentation and Methods for Astrophysics, FOS: Physical sciences, Astrophysics - High Energy Astrophysical Phenomena, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract

The principal goal of this whitepaper is not so much to demonstrate that gravitational wave detectors like LIGO and LISA will help answer many central questions in astronomy and astrophysics, but to make the case that they can help answer a far greater range of questions if we prepare to make the (sometimes substantial) effort to identify electromagnetic counterparts to the gravitational wave sources., Science White Paper submitted to the Astro2010 Decadal Survey

Published
2009

3. LISA: Probing the Universe with Gravitational Waves

Author

Prince, T. A., Binétruy, P., Centrella, J., Finn, L. S., Hogan, C., Nelemans, G., Phinney, E. S., Schutz, B., 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), LISA, 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)-Institut für theoretische Physik, 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, and Lantz, Simone

Subjects
[SDU.ASTR.CO] Sciences of the Universe [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], General Relativity and Quantum Cosmology, [PHYS.ASTR.CO] Physics [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO], [SDU.ASTR.CO]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO], Physics::Space Physics, Astrophysics::Instrumentation and Methods for Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics::Galaxy Astrophysics
Abstract

2007 AAS/AAPT Joint Meeting, American Astronomical Society Meeting 209, #74.01; International audience; LISA is a joint NASA/ESA space mission for detection and study of low-frequency gravitational waves in the band from 0.1 mHz to 0.1 Hz. The mission consists of three satellites separated by a nominal distance of 5 million kilometers, with precision metrology provided by laser ranging. LISA will detect many new sources of gravitational waves including: the inspiral and merger of supermassive black holes resulting from galaxy mergers anywhere in the observable universe, emission from thousands of individual ultra-compact binaries in our galaxy, and numerous cases of inspiral of small black holes, neutrons stars, and white dwarfs into the supermassive black holes that reside in the nuclei of most galaxies. These sources not only provide unique astrophysical information about the evolution of galaxies and stars, but the systems can also be used as "laboratories" for making precision measurements of physical phenomena that will lead to new insights into fundamental physics and cosmology. In addition to radiation from well-known astrophysical sources, some of the most exciting science may come from LISA searches for gravitational waves from the very early universe, such as waves from fundamental phase transitions or from the dynamics of cosmic superstrings. We survey the science goals of LISA and their impact on physics and astrophysics.

Published
2007

4. Discovery of a Radio Source following the 27 December 2004 Giant Flare from SGR 1806-20

Author

Cameron, P. B., Chandra, P., Ray, A., Kulkarni, S. R., Frail, D. A., Wieringa, M. H., Nakar, E., Phinney, E. S., Miyazaki, Atsushi, Tsuboi, Masato, Okumura, Sachiko, Kawai, N., Menten, K. M., and Bertoldi, F.

Subjects
Astrophysics::High Energy Astrophysical Phenomena, Astrophysics (astro-ph), FOS: Physical sciences, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, Astrophysics::Galaxy Astrophysics
Abstract

Over a decade ago it was established that the remarkable high energy transients, known as soft gamma-ray repeaters (SGRs), are a Galactic population and originate from neutron stars with intense (~ 0.3 erg/cm^2) was detected from SGR 1806-20. Here we report the discovery of a fading radio counterpart. We began a monitoring program from 0.2GHz to 250GHz and obtained a high resolution 21-cm radio spectrum which traces the intervening interstellar neutral Hydrogen clouds. Analysis of the spectrum yields the first direct distance measurement of SGR 1806-20. The source is located at a distance greater than 6.4 kpc and we argue that it is nearer than 9.8 kpc. If true, our distance estimate lowers the total energy of the explosion and relaxes the demands on theoretical models. The energetics and the rapid decay of the radio source are not compatible with the afterglow model that is usually invoked for gamma-ray bursts. Instead we suggest that the rapidly decaying radio emission arises from the debris ejected during the explosion., Comment: 16 pages, 2 figures, submitted to Nature (substantial revisions)

Published
2005

5. A Practical Theorem on Gravitational Wave Backgrounds

Author

Phinney, E. S.

Subjects
General Relativity and Quantum Cosmology, Astrophysics (astro-ph), FOS: Physical sciences, General Relativity and Quantum Cosmology (gr-qc), Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics
Abstract

There is an extremely simple relationship between the spectrum of the gravitational wave background produced by a cosmological distribution of discrete gravitational wave sources, the total time-integrated energy spectrum of an individual source, and the present-day comoving number density of remnants. Stated in this way, the background is entirely independent of the cosmology, and only weakly dependent on the evolutionary history of the sources. This relationship allows one easily to compute the amplitude and spectrum of cosmic gravitational wave backgrounds from a broad range of astrophysical sources, and to evaluate the uncertainties therein., 7 pages, no figures, uses mn2e.cls; submitted to MNRAS

Published
2001

6. Why pulsars rotate and move: kicks at birth

Author

Spruit, H. and Phinney, E. S.

Subjects
Astrophysics::High Energy Astrophysical Phenomena, Astrophysics (astro-ph), FOS: Physical sciences, Astrophysics
Abstract

RADIO pulsars are thought to born with spin periods of 0.02-0.5 s and space velocities of 100-1000 km/s, and they are inferred to have initial dipole magnetic fields of 10^{11}-10^{13}. The average space velocity of a normal star in the Milky Way is only 30 km/s, which means that pulsars must receive a substantial 'kick' at birth. Here we propose that the birth characteristics of pulsars have a simple physical connection with each other. Magnetic fields maintained by differential rotation between the core and envelope of the progenitor would keep the whole star in a state of approximately uniform rotation until 10 years before the explosion. Such a slowly rotating core has 1000 times less angular momentum than required to explain the rotation of pulsars. Although the specific physical process that 'kicks' the neutron star at birth has not been identified, unless its force is exerted exactly head-on, it will also cause the neutron star to rotate. We identify this process as the origin of the spin of pulsars. Such kicks will cause a correlation between the velocity and spin vectors of pulsars. We predict that many neutron stars are born with periods longer than 2 s, and never become radio pulsars., To appear in Nature. Press embargo till published

Published
1998

7. Stability criteria for mass transfer in binary stellar evolution

Author

Soberman, G. E., Phinney, E. S., Heuvel, E. P. J. van den, and High Energy Astrophys. & Astropart. Phys (API, FNWI)

Subjects
Astrophysics (astro-ph), Astrophysics::Solar and Stellar Astrophysics, FOS: Physical sciences, Astrophysics::Earth and Planetary Astrophysics, Astrophysics, Astrophysics::Galaxy Astrophysics
Abstract

The evolution of a binary star system by various analytic approximations of mass transfer is discussed, with particular attention payed to the stability of these processes against runaway on the thermal and dynamical timescales of the mass donating star. Mass transfer in red giant - neutron star binary systems is used as a specific example of such mass transfer, and is investigated. Hjellming and Webbink's (1987) results on the dynamic timescale response of a convective star with a core to mass loss are applied, with new results. It is found that mass transfer is usually stable, so long as the the wind's specific angular momentum does not exceed the angular momentum per reduced mass of the system. This holds for both dynamical and thermal timescales. Those systems which are not stable will usually transfer mass on the thermal timescale. Included are graphs illustrating the variation of the Roche radius exponent with mass ratio in the binary, for various parameters in the non-conservative mass transfer, as well as evolutionary paths of interacting red giant neutron star binaries., Comment: 18 pages, 11 figures, LaTeX, l-aa.sty and psfig.sty macros incl. to appear in Astronomy and Astrophysics

Published
1997

8. Analysis of the pulsar P-Ṗ distribution

Author

Phinney, E. S. and Blandford, R. D.

Subjects
Astrophysics::High Energy Astrophysical Phenomena
Abstract

A new technique for the systematic evaluation of models of pulsar period evolution on the basis of a complete observational sample is outlined and applied to the existing incomplete sample. Possible selection effects are discussed. It is concluded that the simple law for the rate of change of period P, Ṗ ∝ P^(2−n) is incompatible with the assumption of stationarity and pulsar ‘death’ at large periods, if n > 2. Models with n < 2, or with n ≳ 2.5 and torque decay on a time-scale of 1 Myr are consistent with the data. Another possibility is that the beaming fraction decreases by a factor ∼5 as a pulsar slows down. A new procedure for deriving a rigorous lower limit to the creation rate of pulsars within the sample is presented, and it is shown that most pulsars appear to be born with large values of Ṗ.

Published
1981

9. Reversed vein bypass to infrapopliteal arteries. Modern results are superior to or equivalent to in-situ bypass for patency and for vein utilization

Author

Taylor, L M, Edwards, J M, Phinney, E S, and Porter, J M

Subjects
Adult, Aged, 80 and over, Reoperation, Leg, Arterial Occlusive Diseases, Arteries, Middle Aged, Amputation, Surgical, Evaluation Studies as Topic, Ischemia, Methods, Humans, Saphenous Vein, Vascular Patency, Research Article, Aged, Follow-Up Studies
Abstract

In recent years many reports have attributed improved patency and improved vein utilization with lower extremity arterial bypass to infrapopliteal arteries to the use of the in-situ vein graft technique (ISVB). This report describes 110 reversed vein bypasses (RVB) to infrapopliteal arteries performed from 1980-1986. Thirty-three per cent of these patients did not have an intact ipsilateral greater saphenous vein. One hundred per cent of patients had autogenous RVB performed using a variety of techniques, including vein splicing, use of arm veins, lesser saphenous veins, branch veins, and use of graft origins distal to the common femoral artery. The life table patency figures for these grafts are 90%, 85%, and 85% at 1 year, 3 years, and 5 years, respectively. The life table limb salvage at 5 years is 93%. These figures for patency, vein utilization, and limb salvage for modern RVB to infrapopliteal arteries are clearly equal to or superior to any reported figures for ISVB. Results for RVB are greatly improved when compared with historic controls, as are results for ISVB. There is no evidence to date demonstrating superiority of one technique versus another.

Published
1987

10. How fast can a blob go?

Author

Phinney, E. S., Zensus, J. Anton, Pearson, Timothy J., and Cohen, Marshall H.

Abstract

[no abstract]

Published
1987

12. The astrophysics of ultra-compact binaries

Author

Nelemans, G., Wood, M., Paul Groot, Anderson, S., Belczynski, K., Benacquista, M., Charles, P., Cumming, A., Deloye, C., Jonker, P., Kalogera, V., Knigge, C., Marsh, T., Motl, P., Napiwotzki, R., O Brien, K., Phinney, E. S., Ramsay, G., Shahbaz, T., Solheim, J. -E, Steeghs, D., Sluys, M., Verbunt, F., Warner, B., Werner, K., Wu, K., and Yungelson, L. R.

Subjects
High Energy Astrophysical Phenomena (astro-ph.HE), Astrophysics - Solar and Stellar Astrophysics, FOS: Physical sciences, General Relativity and Quantum Cosmology (gr-qc), Astrophysics - High Energy Astrophysical Phenomena, Solar and Stellar Astrophysics (astro-ph.SR), General Relativity and Quantum Cosmology
Abstract

This white paper briefly describes the astrophysics of ultra-compact binaries, with emphasis of the challenges and opportunities in the next decade., White paper for the the National Academies Astro2010 decadal survey

13. LISA: Probing the Universe with Gravitational Waves

Author

Prince, Thomas A., Binetruy, P., Centrella, J., Finn, L. S., Hogan, C., Gijs Nelemans, Phinney, E. S., Schutz, B., and Lisa, International Science Team

Subjects
General Relativity and Quantum Cosmology, Astronomy, Physics::Space Physics, Astrophysics::Instrumentation and Methods for Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics::Galaxy Astrophysics
Abstract

Item does not contain fulltext LISA is a joint NASA/ESA space mission for detection and study of low-frequency gravitational waves in the band from 0.1 mHz to 0.1 Hz. The mission consists of three satellites separated by a nominal distance of 5 million kilometers, with precision metrology provided by laser ranging. LISA will detect many new sources of gravitational waves including: the inspiral and merger of supermassive black holes resulting from galaxy mergers anywhere in the observable universe, emission from thousands of individual ultra-compact binaries in our galaxy, and numerous cases of inspiral of small black holes, neutrons stars, and white dwarfs into the supermassive black holes that reside in the nuclei of most galaxies. These sources not only provide unique astrophysical information about the evolution of galaxies and stars, but the systems can also be used as ``laboratories'' for making precision measurements of physical phenomena that will lead to new insights into fundamental physics and cosmology. In addition to radiation from well-known astrophysical sources, some of the most exciting science may come from LISA searches for gravitational waves from the very early universe, such as waves from fundamental phase transitions or from the dynamics of cosmic superstrings. We survey the science goals of LISA and their impact on physics and astrophysics.

14. The Gravitational Universe

Author

Consortium, The Elisa, Seoane, P. Amaro, Aoudia, S., Audley, H., Auger, G., Babak, S., Baker, J., Barausse, E., Barke, S., Bassan, M., Beckmann, V., Benacquista, M., Bender, P. L., Berti, E., Binétruy, P., Bogenstahl, J., Bonvin, C., Bortoluzzi, D., Brause, N. C., Brossard, J., Buchman, S., Bykov, I., Camp, J., Caprini, C., Cavalleri, A., Cerdonio, M., Ciani, G., Colpi, M., Congedo, G., Conklin, J., Cornish, N., Danzmann, K., Vine, G., Debra, D., Dewi Freitag, M., Di Fiore, L., Diaz Aguilo, M., Diepholz, I., Dolesi, R., Dotti, M., Fernández Barranco, G., Ferraioli, L., Ferroni, V., Finetti, N., Fitzsimons, E., Gair, J., Galeazzi, F., Garcia, A., Gerberding, O., Gesa, L., Giardini, D., Gibert, F., Grimani, C., Paul Groot, Guzman Cervantes, F., Haiman, Z., Halloin, H., Heinzel, G., Hewitson, M., Hogan, C., Holz, D., Hornstrup, A., Hoyland, D., Hoyle, C. D., Hueller, M., Hughes, S., Jetzer, P., Kalogera, V., Karnesis, N., Kilic, M., Killow, C., Klipstein, W., Kochkina, E., Korsakova, N., Krolak, A., Larson, S., Lieser, M., Littenberg, T., Livas, J., Lloro, I., Mance, D., Madau, P., Maghami, P., Mahrdt, C., Marsh, T., Mateos, I., Mayer, L., Mcclelland, D., Mckenzie, K., Mcwilliams, S., Merkowitz, S., Miller, C., Mitryk, S., Moerschell, J., Mohanty, S., Monsky, A., Mueller, G., Müller, V., Nelemans, G., Nicolodi, D., Nissanke, S., Nofrarias, M., Numata, K., Ohme, F., Otto, M., Perreur-Lloyd, M., Petiteau, A., Phinney, E. S., Plagnol, E., Pollack, S., Porter, E., Prat, P., Preston, A., Prince, T., Reiche, J., Richstone, D., Robertson, D., Rossi, E. M., Rosswog, S., Rubbo, L., Ruiter, A., Sanjuan, J., Sathyaprakash, B. S., Schlamminger, S., Schutz, B., Schütze, D., Sesana, A., Shaddock, D., Shah, S., Sheard, B., Sopuerta, C. F., Spector, A., Spero, R., Stanga, R., Stebbins, R., Stede, G., Steier, F., Sumner, T., Sun, K. -X, Sutton, A., Tanaka, T., Tanner, D., Thorpe, I., Tröbs, M., Tinto, M., Tu, H. -B, Vallisneri, M., Vetrugno, D., Vitale, S., Volonteri, M., Wand, V., Wang, Y., Wanner, G., Ward, H., Ware, B., Wass, P., Weber, W. J., Yu, Y., Yunes, N., and Zweifel, P.

Subjects
General Relativity and Quantum Cosmology, Cosmology and Nongalactic Astrophysics (astro-ph.CO), FOS: Physical sciences, Astrophysics::Cosmology and Extragalactic Astrophysics, General Relativity and Quantum Cosmology (gr-qc), Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract

The last century has seen enormous progress in our understanding of the Universe. We know the life cycles of stars, the structure of galaxies, the remnants of the big bang, and have a general understanding of how the Universe evolved. We have come remarkably far using electromagnetic radiation as our tool for observing the Universe. However, gravity is the engine behind many of the processes in the Universe, and much of its action is dark. Opening a gravitational window on the Universe will let us go further than any alternative. Gravity has its own messenger: Gravitational waves, ripples in the fabric of spacetime. They travel essentially undisturbed and let us peer deep into the formation of the first seed black holes, exploring redshifts as large as z ~ 20, prior to the epoch of cosmic re-ionisation. Exquisite and unprecedented measurements of black hole masses and spins will make it possible to trace the history of black holes across all stages of galaxy evolution, and at the same time constrain any deviation from the Kerr metric of General Relativity. eLISA will be the first ever mission to study the entire Universe with gravitational waves. eLISA is an all-sky monitor and will offer a wide view of a dynamic cosmos using gravitational waves as new and unique messengers to unveil The Gravitational Universe. It provides the closest ever view of the early processes at TeV energies, has guaranteed sources in the form of verification binaries in the Milky Way, and can probe the entire Universe, from its smallest scales around singularities and black holes, all the way to cosmological dimensions., Comment: 20 pages; submitted to the European Space Agency on May 24th, 2013 for the L2/L3 selection of ESA's Cosmic Vision program

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