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  • 1
    Publication Date: 2006-01-18
    Description: We have discovered a 716-hertz eclipsing binary radio pulsar in the globular cluster Terzan 5 using the Green Bank Telescope. It is the fastest spinning neutron star found to date, breaking the 24-year record held by the 642-hertz pulsar B1937+21. The difficulty in detecting this pulsar, because of its very low flux density and high eclipse fraction (approximately 40% of the orbit), suggests that even faster spinning neutron stars exist. If the pulsar has a mass less than twice the mass of the Sun, then its radius must be constrained by the spin rate to be 〈16 kilometers. The short period of this pulsar also constrains models that suggest that gravitational radiation, through an r-mode (Rossby wave) instability, limits the maximum spin frequency of neutron stars.〈br /〉〈span class="detail_caption"〉Notes: 〈/span〉Hessels, Jason W T -- Ransom, Scott M -- Stairs, Ingrid H -- Freire, Paulo C C -- Kaspi, Victoria M -- Camilo, Fernando -- New York, N.Y. -- Science. 2006 Mar 31;311(5769):1901-4. Epub 2006 Jan 12.〈br /〉〈span class="detail_caption"〉Author address: 〈/span〉Department of Physics, McGill University, Montreal, QC H3A 2T8, Canada. hessels@physics.mcgill.ca〈br /〉〈span class="detail_caption"〉Record origin:〈/span〉 〈a href="http://www.ncbi.nlm.nih.gov/pubmed/16410486" target="_blank"〉PubMed〈/a〉
    Print ISSN: 0036-8075
    Electronic ISSN: 1095-9203
    Topics: Biology , Chemistry and Pharmacology , Computer Science , Medicine , Natural Sciences in General , Physics
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  • 2
    Publication Date: 2008-05-17
    Description: Binary pulsar systems are superb probes of stellar and binary evolution and the physics of extreme environments. In a survey with the Arecibo telescope, we have found PSR J1903+0327, a radio pulsar with a rotational period of 2.15 milliseconds in a highly eccentric (e = 0.44) 95-day orbit around a solar mass (M(middle dot in circle)) companion. Infrared observations identify a possible main-sequence companion star. Conventional binary stellar evolution models predict neither large orbital eccentricities nor main-sequence companions around millisecond pulsars. Alternative formation scenarios involve recycling a neutron star in a globular cluster, then ejecting it into the Galactic disk, or membership in a hierarchical triple system. A relativistic analysis of timing observations of the pulsar finds its mass to be 1.74 +/- 0.04 M solar symbol, an unusually high value.〈br /〉〈span class="detail_caption"〉Notes: 〈/span〉Champion, David J -- Ransom, Scott M -- Lazarus, Patrick -- Camilo, Fernando -- Bassa, Cees -- Kaspi, Victoria M -- Nice, David J -- Freire, Paulo C C -- Stairs, Ingrid H -- van Leeuwen, Joeri -- Stappers, Ben W -- Cordes, James M -- Hessels, Jason W T -- Lorimer, Duncan R -- Arzoumanian, Zaven -- Backer, Don C -- Bhat, N D Ramesh -- Chatterjee, Shami -- Cognard, Ismael -- Deneva, Julia S -- Faucher-Giguere, Claude-Andre -- Gaensler, Bryan M -- Han, Jinlin -- Jenet, Fredrick A -- Kasian, Laura -- Kondratiev, Vlad I -- Kramer, Michael -- Lazio, Joseph -- McLaughlin, Maura A -- Venkataraman, Arun -- Vlemmings, Wouter -- New York, N.Y. -- Science. 2008 Jun 6;320(5881):1309-12. doi: 10.1126/science.1157580. Epub 2008 May 15.〈br /〉〈span class="detail_caption"〉Author address: 〈/span〉Department of Physics, McGill University, Montreal, QC H3A 2T8, Canada. David.Champion@atnf.csiro.au〈br /〉〈span class="detail_caption"〉Record origin:〈/span〉 〈a href="http://www.ncbi.nlm.nih.gov/pubmed/18483399" target="_blank"〉PubMed〈/a〉
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  • 3
    Publication Date: 2010-08-14
    Description: Einstein@Home aggregates the computer power of hundreds of thousands of volunteers from 192 countries to mine large data sets. It has now found a 40.8-hertz isolated pulsar in radio survey data from the Arecibo Observatory taken in February 2007. Additional timing observations indicate that this pulsar is likely a disrupted recycled pulsar. PSR J2007+2722's pulse profile is remarkably wide with emission over almost the entire spin period; the pulsar likely has closely aligned magnetic and spin axes. The massive computing power provided by volunteers should enable many more such discoveries.〈br /〉〈span class="detail_caption"〉Notes: 〈/span〉Knispel, B -- Allen, B -- Cordes, J M -- Deneva, J S -- Anderson, D -- Aulbert, C -- Bhat, N D R -- Bock, O -- Bogdanov, S -- Brazier, A -- Camilo, F -- Champion, D J -- Chatterjee, S -- Crawford, F -- Demorest, P B -- Fehrmann, H -- Freire, P C C -- Gonzalez, M E -- Hammer, D -- Hessels, J W T -- Jenet, F A -- Kasian, L -- Kaspi, V M -- Kramer, M -- Lazarus, P -- van Leeuwen, J -- Lorimer, D R -- Lyne, A G -- Machenschalk, B -- McLaughlin, M A -- Messenger, C -- Nice, D J -- Papa, M A -- Pletsch, H J -- Prix, R -- Ransom, S M -- Siemens, X -- Stairs, I H -- Stappers, B W -- Stovall, K -- Venkataraman, A -- New York, N.Y. -- Science. 2010 Sep 10;329(5997):1305. doi: 10.1126/science.1195253. Epub 2010 Aug 12.〈br /〉〈span class="detail_caption"〉Author address: 〈/span〉Albert-Einstein-Institut, Max-Planck-Institut fur Gravitationsphysik, D-30167 Hannover, Germany. benjamin.knispel@aei.mpg.de〈br /〉〈span class="detail_caption"〉Record origin:〈/span〉 〈a href="http://www.ncbi.nlm.nih.gov/pubmed/20705813" target="_blank"〉PubMed〈/a〉
    Print ISSN: 0036-8075
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  • 4
    Publication Date: 2003-07-12
    Description: The pulsar B1620-26 has two companions, one of stellar mass and one of planetary mass. We detected the stellar companion with the use of Hubble Space Telescope observations. The color and magnitude of the stellar companion indicate that it is an undermassive white dwarf (0.34 +/- 0.04 solar mass) of age 480 x 10(6) +/- 140 x 10(6) years. This places a constraint on the recent history of this triple system and supports a scenario in which the current configuration arose through a dynamical exchange interaction in the cluster core. This implies that planets may be relatively common in low-metallicity globular clusters and that planet formation is more widespread and has happened earlier than previously believed.〈br /〉〈span class="detail_caption"〉Notes: 〈/span〉Sigurdsson, Steinn -- Richer, Harvey B -- Hansen, Brad M -- Stairs, Ingrid H -- Thorsett, Stephen E -- New York, N.Y. -- Science. 2003 Jul 11;301(5630):193-6.〈br /〉〈span class="detail_caption"〉Author address: 〈/span〉525 Davey Laboratory, Department of Astronomy, Pennsylvania State University, University Park, PA 16802, USA. steinn@astro.psu.edu〈br /〉〈span class="detail_caption"〉Record origin:〈/span〉 〈a href="http://www.ncbi.nlm.nih.gov/pubmed/12855802" target="_blank"〉PubMed〈/a〉
    Print ISSN: 0036-8075
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  • 5
    Publication Date: 2005-01-18
    Description: We have identified 21 millisecond pulsars (MSPs) in globular cluster Terzan 5 by using the Green Bank Telescope, bringing the total of known MSPs in Terzan 5 to 24. These discoveries confirm fundamental predictions of globular cluster and binary system evolution. Thirteen of the new MSPs are in binaries, of which two show eclipses and two have highly eccentric orbits. The relativistic periastron advance for the two eccentric systems indicates that at least one of these pulsars has a mass 1.68 times greater than the mass of the Sun at 95% confidence. Such large neutron star masses constrain the equation of state of matter at or beyond the nuclear equilibrium density.〈br /〉〈span class="detail_caption"〉Notes: 〈/span〉Ransom, Scott M -- Hessels, Jason W T -- Stairs, Ingrid H -- Freire, Paulo C C -- Camilo, Fernando -- Kaspi, Victoria M -- Kaplan, David L -- New York, N.Y. -- Science. 2005 Feb 11;307(5711):892-6. Epub 2005 Jan 13.〈br /〉〈span class="detail_caption"〉Author address: 〈/span〉National Radio Astronomy Observatory, 520 Edgemont Road, Charlottesville, VA 22903, USA. sransom@nrao.edu〈br /〉〈span class="detail_caption"〉Record origin:〈/span〉 〈a href="http://www.ncbi.nlm.nih.gov/pubmed/15653465" target="_blank"〉PubMed〈/a〉
    Print ISSN: 0036-8075
    Electronic ISSN: 1095-9203
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  • 6
    Publication Date: 2004-04-24
    Description: Radio pulsars in binary orbits often have short millisecond spin periods as a result of mass transfer from their companion stars. They therefore act as very precise, stable, moving clocks that allow us to investigate a large set of otherwise inaccessible astrophysical problems. The orbital parameters derived from high-precision binary pulsar timing provide constraints on binary evolution, characteristics of the binary pulsar population, and the masses of neutron stars with different mass-transfer histories. These binary systems also test gravitational theories, setting strong limits on deviations from general relativity. Surveys for new pulsars yield new binary systems that increase our understanding of all these fields and may open up whole new areas of physics, as most spectacularly evidenced by the recent discovery of an extremely relativistic double-pulsar system.〈br /〉〈span class="detail_caption"〉Notes: 〈/span〉Stairs, Ingrid H -- New York, N.Y. -- Science. 2004 Apr 23;304(5670):547-52.〈br /〉〈span class="detail_caption"〉Author address: 〈/span〉Department of Physics and Astronomy, University of British Columbia, 6224 Agricultural Road, Vancouver, BC V6T 1Z1, Canada. stairs@astro.ubc.ca〈br /〉〈span class="detail_caption"〉Record origin:〈/span〉 〈a href="http://www.ncbi.nlm.nih.gov/pubmed/15105492" target="_blank"〉PubMed〈/a〉
    Print ISSN: 0036-8075
    Electronic ISSN: 1095-9203
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  • 7
    Publication Date: 2006-09-16
    Description: The double pulsar system PSR J0737-3039A/B is unique in that both neutron stars are detectable as radio pulsars. They are also known to have much higher mean orbital velocities and accelerations than those of other binary pulsars. The system is therefore a good candidate for testing Einstein's theory of general relativity and alternative theories of gravity in the strong-field regime. We report on precision timing observations taken over the 2.5 years since its discovery and present four independent strong-field tests of general relativity. These tests use the theory-independent mass ratio of the two stars. By measuring relativistic corrections to the Keplerian description of the orbital motion, we find that the "post-Keplerian" parameter s agrees with the value predicted by general relativity within an uncertainty of 0.05%, the most precise test yet obtained. We also show that the transverse velocity of the system's center of mass is extremely small. Combined with the system's location near the Sun, this result suggests that future tests of gravitational theories with the double pulsar will supersede the best current solar system tests. It also implies that the second-born pulsar may not have formed through the core collapse of a helium star, as is usually assumed.〈br /〉〈span class="detail_caption"〉Notes: 〈/span〉Kramer, M -- Stairs, I H -- Manchester, R N -- McLaughlin, M A -- Lyne, A G -- Ferdman, R D -- Burgay, M -- Lorimer, D R -- Possenti, A -- D'Amico, N -- Sarkissian, J M -- Hobbs, G B -- Reynolds, J E -- Freire, P C C -- Camilo, F -- New York, N.Y. -- Science. 2006 Oct 6;314(5796):97-102. Epub 2006 Sep 14.〈br /〉〈span class="detail_caption"〉Author address: 〈/span〉University of Manchester, Jodrell Bank Observatory, Macclesfield SK11 9DL, UK. mkramer@jb.man.ac.uk〈br /〉〈span class="detail_caption"〉Record origin:〈/span〉 〈a href="http://www.ncbi.nlm.nih.gov/pubmed/16973838" target="_blank"〉PubMed〈/a〉
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  • 8
    Publication Date: 2016-03-10
    Description: A repeating fast radio burst Nature 531, 7593 (2016). doi:10.1038/nature17168 Authors: L. G. Spitler, P. Scholz, J. W. T. Hessels, S. Bogdanov, A. Brazier, F. Camilo, S. Chatterjee, J. M. Cordes, F. Crawford, J. Deneva, R. D. Ferdman, P. C. C. Freire, V. M. Kaspi, P. Lazarus, R. Lynch, E. C. Madsen, M. A. McLaughlin, C. Patel, S. M. Ransom, A. Seymour, I. H. Stairs, B. W. Stappers, J. van Leeuwen & W. W. Zhu Fast radio bursts are millisecond-duration astronomical radio pulses of unknown physical origin that appear to come from extragalactic distances. Previous follow-up observations have failed to find additional bursts at the same dispersion measure (that is, the integrated column density of free electrons between source and telescope) and sky position as the original detections. The apparent non-repeating nature of these bursts has led to the suggestion that they originate in cataclysmic events. Here we report observations of ten additional bursts from the direction of the fast radio burst FRB 121102. These bursts have dispersion measures and sky positions consistent with the original burst. This unambiguously identifies FRB 121102 as repeating and demonstrates that its source survives the energetic events that cause the bursts. Additionally, the bursts from FRB 121102 show a wide range of spectral shapes that appear to be predominantly intrinsic to the source and which vary on timescales of minutes or less. Although there may be multiple physical origins for the population of fast radio bursts, these repeat bursts with high dispersion measure and variable spectra specifically seen from the direction of FRB 121102 support an origin in a young, highly magnetized, extragalactic neutron star.
    Print ISSN: 0028-0836
    Electronic ISSN: 1476-4687
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    Published by Springer Nature
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  • 9
    Publication Date: 2013-09-27
    Description: It is thought that neutron stars in low-mass binary systems can accrete matter and angular momentum from the companion star and be spun-up to millisecond rotational periods. During the accretion stage, the system is called a low-mass X-ray binary, and bright X-ray emission is observed. When the rate of mass transfer decreases in the later evolutionary stages, these binaries host a radio millisecond pulsar whose emission is powered by the neutron star's rotating magnetic field. This evolutionary model is supported by the detection of millisecond X-ray pulsations from several accreting neutron stars and also by the evidence for a past accretion disc in a rotation-powered millisecond pulsar. It has been proposed that a rotation-powered pulsar may temporarily switch on during periods of low mass inflow in some such systems. Only indirect evidence for this transition has hitherto been observed. Here we report observations of accretion-powered, millisecond X-ray pulsations from a neutron star previously seen as a rotation-powered radio pulsar. Within a few days after a month-long X-ray outburst, radio pulses were again detected. This not only shows the evolutionary link between accretion and rotation-powered millisecond pulsars, but also that some systems can swing between the two states on very short timescales.〈br /〉〈span class="detail_caption"〉Notes: 〈/span〉Papitto, A -- Ferrigno, C -- Bozzo, E -- Rea, N -- Pavan, L -- Burderi, L -- Burgay, M -- Campana, S -- Di Salvo, T -- Falanga, M -- Filipovic, M D -- Freire, P C C -- Hessels, J W T -- Possenti, A -- Ransom, S M -- Riggio, A -- Romano, P -- Sarkissian, J M -- Stairs, I H -- Stella, L -- Torres, D F -- Wieringa, M H -- Wong, G F -- England -- Nature. 2013 Sep 26;501(7468):517-20. doi: 10.1038/nature12470.〈br /〉〈span class="detail_caption"〉Author address: 〈/span〉Institute of Space Sciences (ICE; IEEC-CSIC), Campus UAB, Faculty of Science, Torre C5, Parell, 2a Planta, E-08193 Barcelona, Spain. papitto@ice.csic.es〈br /〉〈span class="detail_caption"〉Record origin:〈/span〉 〈a href="http://www.ncbi.nlm.nih.gov/pubmed/24067710" target="_blank"〉PubMed〈/a〉
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  • 10
    Publication Date: 2014-01-07
    Description: Gravitationally bound three-body systems have been studied for hundreds of years and are common in our Galaxy. They show complex orbital interactions, which can constrain the compositions, masses and interior structures of the bodies and test theories of gravity, if sufficiently precise measurements are available. A triple system containing a radio pulsar could provide such measurements, but the only previously known such system, PSR B1620-26 (refs 7, 8; with a millisecond pulsar, a white dwarf, and a planetary-mass object in an orbit of several decades), shows only weak interactions. Here we report precision timing and multiwavelength observations of PSR J0337+1715, a millisecond pulsar in a hierarchical triple system with two other stars. Strong gravitational interactions are apparent and provide the masses of the pulsar M[Symbol: see text](1.4378(13), where M[Symbol: see text]is the solar mass and the parentheses contain the uncertainty in the final decimal places) and the two white dwarf companions (0.19751(15)M[Symbol: see text] and 0.4101(3))M[Symbol: see text], as well as the inclinations of the orbits (both about 39.2 degrees ). The unexpectedly coplanar and nearly circular orbits indicate a complex and exotic evolutionary past that differs from those of known stellar systems. The gravitational field of the outer white dwarf strongly accelerates the inner binary containing the neutron star, and the system will thus provide an ideal laboratory in which to test the strong equivalence principle of general relativity.〈br /〉〈span class="detail_caption"〉Notes: 〈/span〉Ransom, S M -- Stairs, I H -- Archibald, A M -- Hessels, J W T -- Kaplan, D L -- van Kerkwijk, M H -- Boyles, J -- Deller, A T -- Chatterjee, S -- Schechtman-Rook, A -- Berndsen, A -- Lynch, R S -- Lorimer, D R -- Karako-Argaman, C -- Kaspi, V M -- Kondratiev, V I -- McLaughlin, M A -- van Leeuwen, J -- Rosen, R -- Roberts, M S E -- Stovall, K -- England -- Nature. 2014 Jan 23;505(7484):520-4. doi: 10.1038/nature12917. Epub 2014 Jan 5.〈br /〉〈span class="detail_caption"〉Author address: 〈/span〉National Radio Astronomy Observatory, 520 Edgemont Road, Charlottesville, Virginia 22903-2475, USA. ; Department of Physics and Astronomy, University of British Columbia, 6224 Agricultural Road, Vancouver, British Columbia V6T 1Z1, Canada. ; 1] Netherlands Institute for Radio Astronomy (ASTRON), Postbus 2, 7990 AA Dwingeloo, The Netherlands [2] Department of Physics, McGill University, 3600 University Street, Montreal, Quebec H3A 2T8, Canada. ; 1] Netherlands Institute for Radio Astronomy (ASTRON), Postbus 2, 7990 AA Dwingeloo, The Netherlands [2] Astronomical Institute 'Anton Pannekoek', University of Amsterdam, Science Park 904, 1098 XH Amsterdam, The Netherlands. ; 1] Physics Department, University of Wisconsin-Milwaukee, PO Box 413, Milwaukee, Wisconsin 53201, USA [2] Department of Astronomy, University of Wisconsin-Madison, 475 North Charter Street, Madison, Wisconsin 53706-1582, USA. ; Department of Astronomy and Astrophysics, University of Toronto, 50 St George Street, Toronto, Ontario M5S 3H4, Canada. ; 1] Department of Physics and Astronomy, West Virginia University, White Hall, Box 6315, Morgantown, West Virginia 26506-6315, USA [2] Physics and Astronomy Department, Western Kentucky University, 1906 College Heights Boulevard, Bowling Green, Kentucky 42101-1077, USA. ; Netherlands Institute for Radio Astronomy (ASTRON), Postbus 2, 7990 AA Dwingeloo, The Netherlands. ; Center for Radiophysics and Space Research, Cornell University, 524 Space Sciences Building, Ithaca, New York 14853, USA. ; Department of Astronomy, University of Wisconsin-Madison, 475 North Charter Street, Madison, Wisconsin 53706-1582, USA. ; Department of Physics, McGill University, 3600 University Street, Montreal, Quebec H3A 2T8, Canada. ; Department of Physics and Astronomy, West Virginia University, White Hall, Box 6315, Morgantown, West Virginia 26506-6315, USA. ; 1] Netherlands Institute for Radio Astronomy (ASTRON), Postbus 2, 7990 AA Dwingeloo, The Netherlands [2] Astro Space Center of the Lebedev Physical Institute, 53 Leninskij Prospekt, Moscow 119991, Russia. ; 1] National Radio Astronomy Observatory, 520 Edgemont Road, Charlottesville, Virginia 22903-2475, USA [2] Department of Physics and Astronomy, West Virginia University, White Hall, Box 6315, Morgantown, West Virginia 26506-6315, USA. ; 1] Eureka Scientific Inc., 2452 Delmer Street, Suite 100, Oakland, California 94602-3017, USA [2] Physics Department, New York University at Abu Dhabi, PO Box 129188, Abu Dhabi, United Arab Emirates. ; 1] Department of Physics and Astronomy, University of Texas at Brownsville, One West University Boulevard, Brownsville, Texas 78520, USA [2] Physics and Astronomy Department, University of New Mexico, 1919 Lomas Boulevard NE, Albuquerque, New Mexico 87131-0001, USA.〈br /〉〈span class="detail_caption"〉Record origin:〈/span〉 〈a href="http://www.ncbi.nlm.nih.gov/pubmed/24390352" target="_blank"〉PubMed〈/a〉
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