Topic
Einstein@Home
About: Einstein@Home is a research topic. Over the lifetime, 40 publications have been published within this topic receiving 1088 citations.
Papers
Max Planck Society1, Columbia University2, Cornell University3, West Virginia University4, Franklin & Marshall College5, United States Naval Research Laboratory6, McGill University7, University of Amsterdam8, ASTRON9, University of Texas at Brownsville10, Arecibo Observatory11, University of Wisconsin–Milwaukee12, University of British Columbia13, University of New Mexico14
TL;DR: In this article, the authors reported the discovery of PSR J1913+1102, a 27.3 ms pulsar found in data from the ongoing Arecibo PALFA pulsar survey.
Abstract: We report here the Einstein@Home discovery of PSR J1913+1102, a 27.3 ms pulsar found in data from the ongoing Arecibo PALFA pulsar survey. The pulsar is in a 4.95 hr double neutron star (DNS) system with an eccentricity of 0.089. From radio timing with the Arecibo 305 m telescope, we measure the rate of advance of periastron to be $\dot{\omega }=5.632(18)$° yr−1. Assuming general relativity accurately models the orbital motion, this corresponds to a total system mass of M tot = 2.875(14) ${M}_{\odot }$, similar to the mass of the most massive DNS known to date, B1913+16, but with a much smaller eccentricity. The small eccentricity indicates that the second-formed neutron star (NS) (the companion of PSR J1913+1102) was born in a supernova with a very small associated kick and mass loss. In that case, this companion is likely, by analogy with other systems, to be a light (~1.2 ${M}_{\odot }$) NS; the system would then be highly asymmetric. A search for radio pulsations from the companion yielded no plausible detections, so we cannot yet confirm this mass asymmetry. By the end of 2016, timing observations should permit the detection of two additional post-Keplerian parameters: the Einstein delay (γ), which will enable precise mass measurements and a verification of the possible mass asymmetry of the system, and the orbital decay due to the emission of gravitational waves (${\dot{P}}_{b}$), which will allow another test of the radiative properties of gravity. The latter effect will cause the system to coalesce in ~0.5 Gyr.
86 citations
TL;DR: In this article, the results of a recent blind search survey for gamma-ray pulsars in Fermi Large Area Telescope (LAT) data being carried out on the distributed volunteer computing system, Einstein@Home.
Abstract: We report on the results of a recent blind search survey for gamma-ray pulsars in Fermi Large Area Telescope (LAT) data being carried out on the distributed volunteer computing system, Ein-stein@Home. The survey has searched for pulsations in 118 unidentified pulsar-like sources, requiring about 10, 000 years of CPU core time. In total, this survey has resulted in the discovery of 17 new gamma-ray pulsars, of which 13 are newly reported in this work, and an accompanying paper. These pulsars are all young, isolated pulsars with characteristic ages between 12 kyr and 2 Myr, and spin-down powers between 10 34 and 4 × 10 36 erg s −1. Two of these are the slowest spinning gamma-ray pulsars yet known. One pulsar experienced a very large glitch ∆f /f ≈ 3.5 × 10 −6 during the Fermi mission. In this, the first of two associated papers, we describe the search scheme used in this survey, and estimate the sensitivity of our search to pulsations in unidentified Fermi-LAT sources. One such estimate results in an upper limit of 57% for the fraction of pulsed emission from the gamma-ray source associated with the Cas A supernova remnant, constraining the pulsed gamma-ray photon flux that can be produced by the neutron star at its center. We also present the results of precise timing analyses for each of the newly detected pulsars.
82 citations
Max Planck Society1, University of Bern2, Leibniz University of Hanover3, University of California, Berkeley4, Franklin & Marshall College5, University of Wisconsin–Milwaukee6, University of Manchester7, West Virginia University8, Stanford University9, Commonwealth Scientific and Industrial Research Organisation10
TL;DR: The Parkes multi-beam pulsar survey (PMPS) data has been used to search for radio pulsars in compact binary systems in this article, employing novel methods to remove the Doppler modulation from binary motion.
Abstract: We have conducted a new search for radio pulsars in compact binary systems in the Parkes multi-beam pulsar survey (PMPS) data, employing novel methods to remove the Doppler modulation from binary motion. This has yielded unparalleled sensitivity to pulsars in compact binaries. The required computation time of approximately 17000 CPU core years was provided by the distributed volunteer computing project Einstein@Home, which has a sustained computing power of about 1 PFlop/s. We discovered 24 new pulsars in our search, of which 18 were isolated pulsars, and six were members of binary systems. Despite the wide filterbank channels and relatively slow sampling time of the PMPS data, we found pulsars with very large ratios of dispersion measure (DM) to spin period. Among those is PSR J1748-3009, the millisecond pulsar with the highest known DM (approximately 420 pc/cc). We also discovered PSR J1840-0643, which is in a binary system with an orbital period of 937 days, the fourth largest known. The new pulsar J1750-2536 likely belongs to the rare class of intermediate-mass binary pulsars. Three of the isolated pulsars show long-term nulling or intermittency in their emission, further increasing this growing family. Our discoveries demonstrate the value of distributed volunteer computing for data-driven astronomy and the importance of applying new analysis methods to extensively searched data.
62 citations
TL;DR: In this article, the authors reported the discovery of PSR J1913+1102, a 27.3-ms pulsar found in data from the ongoing Arecibo PALFA pulsar survey.
Abstract: We report here the Einstein@Home discovery of PSR J1913+1102, a 27.3-ms pulsar found in data from the ongoing Arecibo PALFA pulsar survey. The pulsar is in a 4.95-hr double neutron star (DNS) system with an eccentricity of 0.089. From radio timing with the Arecibo 305-m telescope, we measure the rate of advance of periastron to be 5.632(18) deg/yr. Assuming general relativity accurately models the orbital motion, this corresponds to a total system mass of 2.875(14) solar masses, similar to the mass of the most massive DNS known to date, B1913+16, but with a much smaller eccentricity. The small eccentricity indicates that the second-formed neutron star (the companion of PSR J1913+1102) was born in a supernova with a very small associated kick and mass loss. In that case this companion is likely, by analogy with other systems, to be a light (1.2 solar mass) neutron star; the system would then be highly asymmetric. A search for radio pulsations from the companion yielded no plausible detections, so we can't yet confirm this mass asymmetry. By the end of 2016, timing observations should permit the detection of two additional post-Keplerian parameters: the Einstein delay, which will enable precise mass measurements and a verification of the possible mass asymmetry of the system, and the orbital decay due to the emission of gravitational waves, which will allow another test of the radiative properties of gravity. The latter effect will cause the system to coalesce in ~0.5 Gyr.
51 citations
Related Topics (5)
Performance Metrics
| Year | Papers |
|---|---|
| 2021 | 2 |
| 2020 | 3 |
| 2019 | 1 |
| 2018 | 4 |
| 2017 | 4 |
| 2016 | 9 |