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  • American Association for the Advancement of Science (AAAS)  (8)
  • Nature Publishing Group (NPG)  (2)
  • 2010-2014  (8)
  • 2005-2009  (2)
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  • 1
    Publication Date: 2010-01-09
    Description: Recent observations of supernova remnants (SNRs) hint that they accelerate cosmic rays to energies close to ~10(15) electron volts. However, the nature of the particles that produce the emission remains ambiguous. We report observations of SNR W44 with the Fermi Large Area Telescope at energies between 2 x 10(8) electron volts and 3 x10(11) electron volts. The detection of a source with a morphology corresponding to the SNR shell implies that the emission is produced by particles accelerated there. The gamma-ray spectrum is well modeled with emission from protons and nuclei. Its steepening above approximately 10(9) electron volts provides a probe with which to study how particle acceleration responds to environmental effects such as shock propagation in dense clouds and how accelerated particles are released into interstellar space.〈br /〉〈span class="detail_caption"〉Notes: 〈/span〉Abdo, A A -- Ackermann, M -- Ajello, M -- Baldini, L -- Ballet, J -- Barbiellini, G -- Baring, M G -- Bastieri, D -- Baughman, B M -- Bechtol, K -- Bellazzini, R -- Berenji, B -- Blandford, R D -- Bloom, E D -- Bonamente, E -- Borgland, A W -- Bregeon, J -- Brez, A -- Brigida, M -- Bruel, P -- Burnett, T H -- Buson, S -- Caliandro, G A -- Cameron, R A -- Caraveo, P A -- Casandjian, J M -- Cecchi, C -- Celik, O -- Chekhtman, A -- Cheung, C C -- Chiang, J -- Ciprini, S -- Claus, R -- Cognard, I -- Cohen-Tanugi, J -- Cominsky, L R -- Conrad, J -- Cutini, S -- Dermer, C D -- de Angelis, A -- de Palma, F -- Digel, S W -- do Couto e Silva, E -- Drell, P S -- Dubois, R -- Dumora, D -- Espinoza, C -- Farnier, C -- Favuzzi, C -- Fegan, S J -- Focke, W B -- Fortin, P -- Frailis, M -- Fukazawa, Y -- Funk, S -- Fusco, P -- Gargano, F -- Gasparrini, D -- Gehrels, N -- Germani, S -- Giavitto, G -- Giebels, B -- Giglietto, N -- Giordano, F -- Glanzman, T -- Godfrey, G -- Grenier, I A -- Grondin, M-H -- Grove, J E -- Guillemot, L -- Guiriec, S -- Hanabata, Y -- Harding, A K -- Hayashida, M -- Hays, E -- Hughes, R E -- Jackson, M S -- Johannesson, G -- Johnson, A S -- Johnson, T J -- Johnson, W N -- Kamae, T -- Katagiri, H -- Kataoka, J -- Katsuta, J -- Kawai, N -- Kerr, M -- Knodlseder, J -- Kocian, M L -- Kramer, M -- Kuss, M -- Lande, J -- Latronico, L -- Lemoine-Goumard, M -- Longo, F -- Loparco, F -- Lott, B -- Lovellette, M N -- Lubrano, P -- Lyne, A G -- Madejski, G M -- Makeev, A -- Mazziotta, M N -- McEnery, J E -- Meurer, C -- Michelson, P F -- Mitthumsiri, W -- Mizuno, T -- Monte, C -- Monzani, M E -- Morselli, A -- Moskalenko, I V -- Murgia, S -- Nakamori, T -- Nolan, P L -- Norris, J P -- Noutsos, A -- Nuss, E -- Ohsugi, T -- Omodei, N -- Orlando, E -- Ormes, J F -- Paneque, D -- Parent, D -- Pelassa, V -- Pepe, M -- Pesce-Rollins, M -- Piron, F -- Porter, T A -- Raino, S -- Rando, R -- Razzano, M -- Reimer, A -- Reimer, O -- Reposeur, T -- Rochester, L S -- Rodriguez, A Y -- Romani, R W -- Roth, M -- Ryde, F -- Sadrozinski, H F-W -- Sanchez, D -- Sander, A -- Saz Parkinson, P M -- Scargle, J D -- Sgro, C -- Siskind, E J -- Smith, D A -- Smith, P D -- Spandre, G -- Spinelli, P -- Stappers, B W -- Stecker, F W -- Strickman, M S -- Suson, D J -- Tajima, H -- Takahashi, H -- Takahashi, T -- Tanaka, T -- Thayer, J B -- Thayer, J G -- Theureau, G -- Thompson, D J -- Tibaldo, L -- Tibolla, O -- Torres, D F -- Tosti, G -- Tramacere, A -- Uchiyama, Y -- Usher, T L -- Vasileiou, V -- Venter, C -- Vilchez, N -- Vitale, V -- Waite, A P -- Wang, P -- Winer, B L -- Wood, K S -- Yamazaki, R -- Ylinen, T -- Ziegler, M -- New York, N.Y. -- Science. 2010 Feb 26;327(5969):1103-6. doi: 10.1126/science.1182787. Epub 2010 Jan 7.〈br /〉〈span class="detail_caption"〉Author address: 〈/span〉Space Science Division, Naval Research Laboratory, Washington, DC 20375, USA.〈br /〉〈span class="detail_caption"〉Record origin:〈/span〉 〈a href="http://www.ncbi.nlm.nih.gov/pubmed/20056857" target="_blank"〉PubMed〈/a〉
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  • 2
    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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  • 3
    Publication Date: 2013-11-02
    Description: Pulsars are highly magnetized rotating neutron stars and are well known for the stability of their signature pulse shapes, allowing high-precision studies of their rotation. However, during the past 22 years, the radio pulse profile of the Crab pulsar has shown a steady increase in the separation of the main pulse and interpulse components at 0.62 degrees +/- 0.03 degrees per century. There are also secular changes in the relative strengths of several components of the profile. The changing component separation indicates that the axis of the dipolar magnetic field, embedded in the neutron star, is moving toward the stellar equator. This evolution of the magnetic field could explain why the pulsar does not spin down as expected from simple braking by a rotating dipolar magnetic field.〈br /〉〈span class="detail_caption"〉Notes: 〈/span〉Lyne, Andrew -- Graham-Smith, Francis -- Weltevrede, Patrick -- Jordan, Christine -- Stappers, Ben -- Bassa, Cees -- Kramer, Michael -- New York, N.Y. -- Science. 2013 Nov 1;342(6158):598-601. doi: 10.1126/science.1243254.〈br /〉〈span class="detail_caption"〉Author address: 〈/span〉Jodrell Bank Centre for Astrophysics, School of Physics and Astronomy, University of Manchester, Manchester, M13 9PL, UK.〈br /〉〈span class="detail_caption"〉Record origin:〈/span〉 〈a href="http://www.ncbi.nlm.nih.gov/pubmed/24179221" target="_blank"〉PubMed〈/a〉
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  • 4
    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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  • 5
    Publication Date: 2013-08-16
    Description: Earth's nearest candidate supermassive black hole lies at the centre of the Milky Way. Its electromagnetic emission is thought to be powered by radiatively inefficient accretion of gas from its environment, which is a standard mode of energy supply for most galactic nuclei. X-ray measurements have already resolved a tenuous hot gas component from which the black hole can be fed. The magnetization of the gas, however, which is a crucial parameter determining the structure of the accretion flow, remains unknown. Strong magnetic fields can influence the dynamics of accretion, remove angular momentum from the infalling gas, expel matter through relativistic jets and lead to synchrotron emission such as that previously observed. Here we report multi-frequency radio measurements of a newly discovered pulsar close to the Galactic Centre and show that the pulsar's unusually large Faraday rotation (the rotation of the plane of polarization of the emission in the presence of an external magnetic field) indicates that there is a dynamically important magnetic field near the black hole. If this field is accreted down to the event horizon it provides enough magnetic flux to explain the observed emission--from radio to X-ray wavelengths--from the black hole.〈br /〉〈span class="detail_caption"〉Notes: 〈/span〉Eatough, R P -- Falcke, H -- Karuppusamy, R -- Lee, K J -- Champion, D J -- Keane, E F -- Desvignes, G -- Schnitzeler, D H F M -- Spitler, L G -- Kramer, M -- Klein, B -- Bassa, C -- Bower, G C -- Brunthaler, A -- Cognard, I -- Deller, A T -- Demorest, P B -- Freire, P C C -- Kraus, A -- Lyne, A G -- Noutsos, A -- Stappers, B -- Wex, N -- England -- Nature. 2013 Sep 19;501(7467):391-4. doi: 10.1038/nature12499. Epub 2013 Aug 14.〈br /〉〈span class="detail_caption"〉Author address: 〈/span〉Max-Planck-Institut fur Radioastronomie, Auf dem Hugel 69, D-53121 Bonn, Germany. reatough@mpifr-bonn.mpg.de〈br /〉〈span class="detail_caption"〉Record origin:〈/span〉 〈a href="http://www.ncbi.nlm.nih.gov/pubmed/23945588" target="_blank"〉PubMed〈/a〉
    Print ISSN: 0028-0836
    Electronic ISSN: 1476-4687
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  • 6
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    Nature Publishing Group (NPG)
    Publication Date: 2012-08-31
    Description: 〈br /〉〈span class="detail_caption"〉Notes: 〈/span〉Smith, Francis Graham -- Davies, Rodney -- Lyne, Andrew -- England -- Nature. 2012 Aug 30;488(7413):592. doi: 10.1038/488592a.〈br /〉〈span class="detail_caption"〉Author address: 〈/span〉University of Manchester, UK. fgs@jb.man.ac.uk〈br /〉〈span class="detail_caption"〉Record origin:〈/span〉 〈a href="http://www.ncbi.nlm.nih.gov/pubmed/22932377" target="_blank"〉PubMed〈/a〉
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  • 7
    Publication Date: 2006-02-25
    Description: PSR B1931+24 (J1933+2421) behaves as an ordinary isolated radio pulsar during active phases that are 5 to 10 days long. However, when the radio emission ceases, it switches off in less than 10 seconds and remains undetectable for the next 25 to 35 days, then switches on again. This pattern repeats quasi-periodically. The origin of this behavior is unclear. Even more remarkably, the pulsar rotation slows down 50% faster when it is on than when it is off. This indicates a massive increase in magnetospheric currents when the pulsar switches on, proving that pulsar wind plays a substantial role in pulsar spin-down. This allows us, for the first time, to estimate the magnetospheric currents in a pulsar magnetosphere during the occurrence of radio emission.〈br /〉〈span class="detail_caption"〉Notes: 〈/span〉Kramer, M -- Lyne, A G -- O'Brien, J T -- Jordan, C A -- Lorimer, D R -- New York, N.Y. -- Science. 2006 Apr 28;312(5773):549-51. Epub 2006 Feb 23.〈br /〉〈span class="detail_caption"〉Author address: 〈/span〉Jodrell Bank Observatory, University of Manchester, Macclesfield, SK11 9DL, UK.〈br /〉〈span class="detail_caption"〉Record origin:〈/span〉 〈a href="http://www.ncbi.nlm.nih.gov/pubmed/16497886" target="_blank"〉PubMed〈/a〉
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  • 8
    Publication Date: 2010-12-24
    Description: We systematically generated large-scale data sets to improve genome annotation for the nematode Caenorhabditis elegans, a key model organism. These data sets include transcriptome profiling across a developmental time course, genome-wide identification of transcription factor-binding sites, and maps of chromatin organization. From this, we created more complete and accurate gene models, including alternative splice forms and candidate noncoding RNAs. We constructed hierarchical networks of transcription factor-binding and microRNA interactions and discovered chromosomal locations bound by an unusually large number of transcription factors. Different patterns of chromatin composition and histone modification were revealed between chromosome arms and centers, with similarly prominent differences between autosomes and the X chromosome. Integrating data types, we built statistical models relating chromatin, transcription factor binding, and gene expression. Overall, our analyses ascribed putative functions to most of the conserved genome.〈br /〉〈br /〉〈a href="https://www.ncbi.nlm.nih.gov/pmc/articles/PMC3142569/" target="_blank"〉〈img src="https://static.pubmed.gov/portal/portal3rc.fcgi/4089621/img/3977009" border="0"〉〈/a〉   〈a href="https://www.ncbi.nlm.nih.gov/pmc/articles/PMC3142569/" target="_blank"〉This paper as free author manuscript - peer-reviewed and accepted for publication〈/a〉〈br /〉〈br /〉〈span class="detail_caption"〉Notes: 〈/span〉Gerstein, Mark B -- Lu, Zhi John -- Van Nostrand, Eric L -- Cheng, Chao -- Arshinoff, Bradley I -- Liu, Tao -- Yip, Kevin Y -- Robilotto, Rebecca -- Rechtsteiner, Andreas -- Ikegami, Kohta -- Alves, Pedro -- Chateigner, Aurelien -- Perry, Marc -- Morris, Mitzi -- Auerbach, Raymond K -- Feng, Xin -- Leng, Jing -- Vielle, Anne -- Niu, Wei -- Rhrissorrakrai, Kahn -- Agarwal, Ashish -- Alexander, Roger P -- Barber, Galt -- Brdlik, Cathleen M -- Brennan, Jennifer -- Brouillet, Jeremy Jean -- Carr, Adrian -- Cheung, Ming-Sin -- Clawson, Hiram -- Contrino, Sergio -- Dannenberg, Luke O -- Dernburg, Abby F -- Desai, Arshad -- Dick, Lindsay -- Dose, Andrea C -- Du, Jiang -- Egelhofer, Thea -- Ercan, Sevinc -- Euskirchen, Ghia -- Ewing, Brent -- Feingold, Elise A -- Gassmann, Reto -- Good, Peter J -- Green, Phil -- Gullier, Francois -- Gutwein, Michelle -- Guyer, Mark S -- Habegger, Lukas -- Han, Ting -- Henikoff, Jorja G -- Henz, Stefan R -- Hinrichs, Angie -- Holster, Heather -- Hyman, Tony -- Iniguez, A Leo -- Janette, Judith -- Jensen, Morten -- Kato, Masaomi -- Kent, W James -- Kephart, Ellen -- Khivansara, Vishal -- Khurana, Ekta -- Kim, John K -- Kolasinska-Zwierz, Paulina -- Lai, Eric C -- Latorre, Isabel -- Leahey, Amber -- Lewis, Suzanna -- Lloyd, Paul -- Lochovsky, Lucas -- Lowdon, Rebecca F -- Lubling, Yaniv -- Lyne, Rachel -- MacCoss, Michael -- Mackowiak, Sebastian D -- Mangone, Marco -- McKay, Sheldon -- Mecenas, Desirea -- Merrihew, Gennifer -- Miller, David M 3rd -- Muroyama, Andrew -- Murray, John I -- Ooi, Siew-Loon -- Pham, Hoang -- Phippen, Taryn -- Preston, Elicia A -- Rajewsky, Nikolaus -- Ratsch, Gunnar -- Rosenbaum, Heidi -- Rozowsky, Joel -- Rutherford, Kim -- Ruzanov, Peter -- Sarov, Mihail -- Sasidharan, Rajkumar -- Sboner, Andrea -- Scheid, Paul -- Segal, Eran -- Shin, Hyunjin -- Shou, Chong -- Slack, Frank J -- Slightam, Cindie -- Smith, Richard -- Spencer, William C -- Stinson, E O -- Taing, Scott -- Takasaki, Teruaki -- Vafeados, Dionne -- Voronina, Ksenia -- Wang, Guilin -- Washington, Nicole L -- Whittle, Christina M -- Wu, Beijing -- Yan, Koon-Kiu -- Zeller, Georg -- Zha, Zheng -- Zhong, Mei -- Zhou, Xingliang -- modENCODE Consortium -- Ahringer, Julie -- Strome, Susan -- Gunsalus, Kristin C -- Micklem, Gos -- Liu, X Shirley -- Reinke, Valerie -- Kim, Stuart K -- Hillier, LaDeana W -- Henikoff, Steven -- Piano, Fabio -- Snyder, Michael -- Stein, Lincoln -- Lieb, Jason D -- Waterston, Robert H -- 054523/Wellcome Trust/United Kingdom -- R01 GM088565/GM/NIGMS NIH HHS/ -- R01 GM088565-03/GM/NIGMS NIH HHS/ -- R01GM088565/GM/NIGMS NIH HHS/ -- Howard Hughes Medical Institute/ -- Wellcome Trust/United Kingdom -- New York, N.Y. -- Science. 2010 Dec 24;330(6012):1775-87. doi: 10.1126/science.1196914. Epub 2010 Dec 22.〈br /〉〈span class="detail_caption"〉Author address: 〈/span〉Program in Computational Biology and Bioinformatics, Yale University, Bass 432, 266 Whitney Avenue, New Haven, CT 06520, USA. modencode.worm.pi@gersteinlab.org〈br /〉〈span class="detail_caption"〉Record origin:〈/span〉 〈a href="http://www.ncbi.nlm.nih.gov/pubmed/21177976" target="_blank"〉PubMed〈/a〉
    Keywords: Animals ; Caenorhabditis elegans/*genetics/growth & development/metabolism ; Caenorhabditis elegans Proteins/genetics/metabolism ; Chromatin/genetics/metabolism/ultrastructure ; *Chromosomes/genetics/metabolism/ultrastructure ; Computational Biology/methods ; Conserved Sequence ; Evolution, Molecular ; *Gene Expression Profiling ; *Gene Expression Regulation ; Gene Regulatory Networks ; Genes, Helminth ; *Genome, Helminth ; Genomics/methods ; Histones/metabolism ; Models, Genetic ; *Molecular Sequence Annotation ; RNA, Helminth/genetics/metabolism ; RNA, Untranslated/genetics/metabolism ; Regulatory Sequences, Nucleic Acid ; Transcription Factors/genetics/metabolism
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  • 9
    Publication Date: 2010-06-26
    Description: Pulsars are famed for their rotational clocklike stability and their highly repeatable pulse shapes. However, it has long been known that there are unexplained deviations (often termed timing noise) from the rate at which we predict these clocks should run. We show that timing behavior often results from two different spin-down rates. Pulsars switch abruptly between these states, often quasi-periodically, leading to the observed spin-down patterns. We show that for six pulsars the timing noise is correlated with changes in the pulse shape. Many pulsar phenomena, including mode changing, nulling, intermittency, pulse-shape variability, and timing noise, are therefore linked and are caused by changes in the pulsar's magnetosphere. We consider the possibility that high-precision monitoring of pulse profiles could lead to the formation of highly stable pulsar clocks.〈br /〉〈span class="detail_caption"〉Notes: 〈/span〉Lyne, Andrew -- Hobbs, George -- Kramer, Michael -- Stairs, Ingrid -- Stappers, Ben -- New York, N.Y. -- Science. 2010 Jul 23;329(5990):408-12. doi: 10.1126/science.1186683. Epub 2010 Jun 24.〈br /〉〈span class="detail_caption"〉Author address: 〈/span〉Jodrell Bank Centre for Astrophysics, School of Physics and Astronomy, University of Manchester, Manchester M13 9PL, UK. andrew.lyne@manchester.ac.uk〈br /〉〈span class="detail_caption"〉Record origin:〈/span〉 〈a href="http://www.ncbi.nlm.nih.gov/pubmed/20576852" target="_blank"〉PubMed〈/a〉
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  • 10
    Publication Date: 2011-08-27
    Description: Millisecond pulsars are thought to be neutron stars that have been spun-up by accretion of matter from a binary companion. Although most are in binary systems, some 30% are solitary, and their origin is therefore mysterious. PSR J1719-1438, a 5.7-millisecond pulsar, was detected in a recent survey with the Parkes 64-meter radio telescope. We show that this pulsar is in a binary system with an orbital period of 2.2 hours. The mass of its companion is near that of Jupiter, but its minimum density of 23 grams per cubic centimeter suggests that it may be an ultralow-mass carbon white dwarf. This system may thus have once been an ultracompact low-mass x-ray binary, where the companion narrowly avoided complete destruction.〈br /〉〈span class="detail_caption"〉Notes: 〈/span〉Bailes, M -- Bates, S D -- Bhalerao, V -- Bhat, N D R -- Burgay, M -- Burke-Spolaor, S -- D'Amico, N -- Johnston, S -- Keith, M J -- Kramer, M -- Kulkarni, S R -- Levin, L -- Lyne, A G -- Milia, S -- Possenti, A -- Spitler, L -- Stappers, B -- van Straten, W -- New York, N.Y. -- Science. 2011 Sep 23;333(6050):1717-20. doi: 10.1126/science.1208890. Epub 2011 Aug 25.〈br /〉〈span class="detail_caption"〉Author address: 〈/span〉Centre for Astrophysics and Supercomputing and ARC Centre for All-Sky Astrophysics (CAASTRO), Swinburne University of Technology, Post Office Box 218 Hawthorn, VIC 3122, Australia. mbailes@swin.edu.au〈br /〉〈span class="detail_caption"〉Record origin:〈/span〉 〈a href="http://www.ncbi.nlm.nih.gov/pubmed/21868629" target="_blank"〉PubMed〈/a〉
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