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  • 1
    Publication Date: 2010-10-29
    Description: Neutron stars are composed of the densest form of matter known to exist in our Universe, the composition and properties of which are still theoretically uncertain. Measurements of the masses or radii of these objects can strongly constrain the neutron star matter equation of state and rule out theoretical models of their composition. The observed range of neutron star masses, however, has hitherto been too narrow to rule out many predictions of 'exotic' non-nucleonic components. The Shapiro delay is a general-relativistic increase in light travel time through the curved space-time near a massive body. For highly inclined (nearly edge-on) binary millisecond radio pulsar systems, this effect allows us to infer the masses of both the neutron star and its binary companion to high precision. Here we present radio timing observations of the binary millisecond pulsar J1614-2230 that show a strong Shapiro delay signature. We calculate the pulsar mass to be (1.97 +/- 0.04)M(middle dot in circle), which rules out almost all currently proposed hyperon or boson condensate equations of state (M(middle dot in circle), solar mass). Quark matter can support a star this massive only if the quarks are strongly interacting and are therefore not 'free' quarks.〈br /〉〈span class="detail_caption"〉Notes: 〈/span〉Demorest, P B -- Pennucci, T -- Ransom, S M -- Roberts, M S E -- Hessels, J W T -- England -- Nature. 2010 Oct 28;467(7319):1081-3. doi: 10.1038/nature09466.〈br /〉〈span class="detail_caption"〉Author address: 〈/span〉National Radio Astronomy Observatory, 520 Edgemont Road, Charlottesville, Virginia 22093, USA. pdemores@nrao.edu〈br /〉〈span class="detail_caption"〉Record origin:〈/span〉 〈a href="http://www.ncbi.nlm.nih.gov/pubmed/20981094" target="_blank"〉PubMed〈/a〉
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  • 2
    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〉
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  • 3
    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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  • 4
    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〉
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  • 5
    Publication Date: 2013-01-26
    Description: Pulsars emit from low-frequency radio waves up to high-energy gamma-rays, generated anywhere from the stellar surface out to the edge of the magnetosphere. Detecting correlated mode changes across the electromagnetic spectrum is therefore key to understanding the physical relationship among the emission sites. Through simultaneous observations, we detected synchronous switching in the radio and x-ray emission properties of PSR B0943+10. When the pulsar is in a sustained radio-"bright" mode, the x-rays show only an unpulsed, nonthermal component. Conversely, when the pulsar is in a radio-"quiet" mode, the x-ray luminosity more than doubles and a 100% pulsed thermal component is observed along with the nonthermal component. This indicates rapid, global changes to the conditions in the magnetosphere, which challenge all proposed pulsar emission theories.〈br /〉〈span class="detail_caption"〉Notes: 〈/span〉Hermsen, W -- Hessels, J W T -- Kuiper, L -- van Leeuwen, J -- Mitra, D -- de Plaa, J -- Rankin, J M -- Stappers, B W -- Wright, G A E -- Basu, R -- Alexov, A -- Coenen, T -- Griessmeier, J-M -- Hassall, T E -- Karastergiou, A -- Keane, E -- Kondratiev, V I -- Kramer, M -- Kuniyoshi, M -- Noutsos, A -- Serylak, M -- Pilia, M -- Sobey, C -- Weltevrede, P -- Zagkouris, K -- Asgekar, A -- Avruch, I M -- Batejat, F -- Bell, M E -- Bell, M R -- Bentum, M J -- Bernardi, G -- Best, P -- Birzan, L -- Bonafede, A -- Breitling, F -- Broderick, J -- Bruggen, M -- Butcher, H R -- Ciardi, B -- Duscha, S -- Eisloffel, J -- Falcke, H -- Fender, R -- Ferrari, C -- Frieswijk, W -- Garrett, M A -- de Gasperin, F -- de Geus, E -- Gunst, A W -- Heald, G -- Hoeft, M -- Horneffer, A -- Iacobelli, M -- Kuper, G -- Maat, P -- Macario, G -- Markoff, S -- McKean, J P -- Mevius, M -- Miller-Jones, J C A -- Morganti, R -- Munk, H -- Orru, E -- Paas, H -- Pandey-Pommier, M -- Pandey, V N -- Pizzo, R -- Polatidis, A G -- Rawlings, S -- Reich, W -- Rottgering, H -- Scaife, A M M -- Schoenmakers, A -- Shulevski, A -- Sluman, J -- Steinmetz, M -- Tagger, M -- Tang, Y -- Tasse, C -- ter Veen, S -- Vermeulen, R -- van de Brink, R H -- van Weeren, R J -- Wijers, R A M J -- Wise, M W -- Wucknitz, O -- Yatawatta, S -- Zarka, P -- New York, N.Y. -- Science. 2013 Jan 25;339(6118):436-9. doi: 10.1126/science.1230960.〈br /〉〈span class="detail_caption"〉Author address: 〈/span〉SRON, Netherlands Institute for Space Research, Sorbonnelaan 2, 3584 CA Utrecht, Netherlands. w.hermsen@sron.nl〈br /〉〈span class="detail_caption"〉Record origin:〈/span〉 〈a href="http://www.ncbi.nlm.nih.gov/pubmed/23349288" target="_blank"〉PubMed〈/a〉
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  • 6
    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〉
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  • 7
    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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  • 8
    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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  • 9
    Publication Date: 2009-05-23
    Description: Radio pulsars with millisecond spin periods are thought to have been spun up by the transfer of matter and angular momentum from a low-mass companion star during an x-ray-emitting phase. The spin periods of the neutron stars in several such low-mass x-ray binary (LMXB) systems have been shown to be in the millisecond regime, but no radio pulsations have been detected. Here we report on detection and follow-up observations of a nearby radio millisecond pulsar (MSP) in a circular binary orbit with an optically identified companion star. Optical observations indicate that an accretion disk was present in this system within the past decade. Our optical data show no evidence that one exists today, suggesting that the radio MSP has turned on after a recent LMXB phase.〈br /〉〈span class="detail_caption"〉Notes: 〈/span〉Archibald, Anne M -- Stairs, Ingrid H -- Ransom, Scott M -- Kaspi, Victoria M -- Kondratiev, Vladislav I -- Lorimer, Duncan R -- McLaughlin, Maura A -- Boyles, Jason -- Hessels, Jason W T -- Lynch, Ryan -- van Leeuwen, Joeri -- Roberts, Mallory S E -- Jenet, Frederick -- Champion, David J -- Rosen, Rachel -- Barlow, Brad N -- Dunlap, Bart H -- Remillard, Ronald A -- New York, N.Y. -- Science. 2009 Jun 12;324(5933):1411-4. doi: 10.1126/science.1172740. Epub 2009 May 21.〈br /〉〈span class="detail_caption"〉Author address: 〈/span〉Department of Physics, McGill University, 3600 Rue University, Montreal, Quebec, H3A 2T8, Canada. aarchiba@physics.mcgill.ca〈br /〉〈span class="detail_caption"〉Record origin:〈/span〉 〈a href="http://www.ncbi.nlm.nih.gov/pubmed/19460964" target="_blank"〉PubMed〈/a〉
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  • 10
    Publication Date: 2013-04-27
    Description: Many physically motivated extensions to general relativity (GR) predict substantial deviations in the properties of spacetime surrounding massive neutron stars. We report the measurement of a 2.01 +/- 0.04 solar mass (Mmiddle dot in circle) pulsar in a 2.46-hour orbit with a 0.172 +/- 0.003 Mmiddle dot in circle white dwarf. The high pulsar mass and the compact orbit make this system a sensitive laboratory of a previously untested strong-field gravity regime. Thus far, the observed orbital decay agrees with GR, supporting its validity even for the extreme conditions present in the system. The resulting constraints on deviations support the use of GR-based templates for ground-based gravitational wave detectors. Additionally, the system strengthens recent constraints on the properties of dense matter and provides insight to binary stellar astrophysics and pulsar recycling.〈br /〉〈span class="detail_caption"〉Notes: 〈/span〉Antoniadis, John -- Freire, Paulo C C -- Wex, Norbert -- Tauris, Thomas M -- Lynch, Ryan S -- van Kerkwijk, Marten H -- Kramer, Michael -- Bassa, Cees -- Dhillon, Vik S -- Driebe, Thomas -- Hessels, Jason W T -- Kaspi, Victoria M -- Kondratiev, Vladislav I -- Langer, Norbert -- Marsh, Thomas R -- McLaughlin, Maura A -- Pennucci, Timothy T -- Ransom, Scott M -- Stairs, Ingrid H -- van Leeuwen, Joeri -- Verbiest, Joris P W -- Whelan, David G -- New York, N.Y. -- Science. 2013 Apr 26;340(6131):448, 1233232. doi: 10.1126/science.1233232.〈br /〉〈span class="detail_caption"〉Author address: 〈/span〉Max-Planck-Institut fur Radioastronomie, Auf dem Hugel 69, Bonn, Germany. jantoniadis@mpifr-bonn.mpg.de〈br /〉〈span class="detail_caption"〉Record origin:〈/span〉 〈a href="http://www.ncbi.nlm.nih.gov/pubmed/23620056" target="_blank"〉PubMed〈/a〉
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