Institution
Netherlands Institute for Space Research
Facility•Utrecht, Netherlands•
About: Netherlands Institute for Space Research is a facility organization based out in Utrecht, Netherlands. It is known for research contribution in the topics: Galaxy & Neutron star. The organization has 737 authors who have published 3026 publications receiving 106632 citations. The organization is also known as: SRON & Space Research Organisation Netherlands.
Topics: Galaxy, Neutron star, Stars, Spectral line, Luminosity
Papers published on a yearly basis
Papers
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Max Planck Society1, University of Minnesota2, University of Amsterdam3, ASTRON4, University of Southampton5, Swinburne University of Technology6, University of Orléans7, Rhodes University8, University of the Western Cape9, Netherlands Institute for Space Research10, Commonwealth Scientific and Industrial Research Organisation11, Harvard University12, University of Edinburgh13, Jacobs University Bremen14, Leibniz Institute for Astrophysics Potsdam15, Radboud University Nijmegen16, Ruhr University Bochum17, University of Oulu18, Center for Information Technology19, National Radio Astronomy Observatory20, Pennsylvania State University21, Deutsche Sammlung von Mikroorganismen und Zellkulturen22, University of Paris-Sud23
TL;DR: In this article, the authors report on the LOFAR discovery that PSR B0823+26 has a weak and sporadically emitting "quiet" (Q) emission mode that is over 100 times weaker (on average) and has a nulling fraction forty-times greater than that of the more regularly-emitting "bright" (B) mode.
Abstract: PSR B0823+26, a 0.53-s radio pulsar, displays a host of emission phenomena over timescales of seconds to (at least) hours, including nulling, subpulse drifting, and mode-changing. Studying pulsars like PSR B0823+26 provides further insight into the relationship between these various emission phenomena and what they might teach us about pulsar magnetospheres. Here we report on the LOFAR discovery that PSR B0823+26 has a weak and sporadically emitting 'quiet' (Q) emission mode that is over 100 times weaker (on average) and has a nulling fraction forty-times greater than that of the more regularly-emitting 'bright' (B) mode. Previously, the pulsar has been undetected in the Q-mode, and was assumed to be nulling continuously. PSR B0823+26 shows a further decrease in average flux just before the transition into the B-mode, and perhaps truly turns off completely at these times. Furthermore, simultaneous observations taken with the LOFAR, Westerbork, Lovell, and Effelsberg telescopes between 110 MHz and 2.7 GHz demonstrate that the transition between the Q-mode and B-mode occurs within one single rotation of the neutron star, and that it is concurrent across the range of frequencies observed.
42 citations
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TL;DR: In this paper, Chandra X-ray observations of four optically-selected tidal disruption events (TDEs) obtained 4-9 years after discovery were used to provide evidence that TDEs transition from an early-time soft state to a late-time hard state many years after disruption.
Abstract: We present Chandra X-ray observations of four optically-selected tidal disruption events (TDEs) obtained 4-9 years after discovery. Three sources were detected with luminosities between 9X10^40 and 3X10^42 erg/s. The spectrum of PTF09axc is consistent with a power law of index 2.5+-0.1, whereas the spectrum of PTF09ge is very soft. The power law spectrum of PTF09axc and prior literature findings, provide evidence that TDEs transition from an early-time soft state to a late-time hard state many years after disruption. We propose that the time to peak luminosity for optical and X-ray emission may differ substantially in TDEs, with X-rays being produced or becoming observable later. This delay helps explain the differences in observed properties such as L_opt/L_ X of optically and X-ray selected TDEs. We update TDE rate predictions for the eROSITA instrument: it ranges from 3 per yr to 990 per yr, depending sensitively on the distribution of black hole spins and the time delay between disruption and peak X-ray brightness. We further predict an asymmetry in the number of retrograde and prograde disks in samples of optically and X-ray selected TDEs. The details of the observational biases can contribute to observed differences between optically and X-ray selected TDEs (with optically selected TDEs being fainter in X-rays for retrograde TDE disks).
42 citations
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TL;DR: In this article, the authors present a catalog of 3387 bursts from low-mass X-ray binaries with recurrence times of less than one hour, that come in multiples of up to four events, from 15 sources.
Abstract: Type I X-ray bursts from low-mass X-ray binaries result from a thermonuclear runaway in the material accreted onto the neutron star. Although typical recurrence times are a few hours, consistent with theoretical ignition model predictions, there are also observations of bursts occurring as promptly as ten minutes or less after the previous event. We present a comprehensive assessment of this phenomenon using a catalog of 3387 bursts observed with the BeppoSAX/WFCs and RXTE/PCA X-ray instruments. This catalog contains 136 bursts with recurrence times of less than one hour, that come in multiples of up to four events, from 15 sources. Short recurrence times are not observed from so-called ultra-compact binaries, indicating that hydrogen burning processes play a crucial role. As far as the neutron star spin frequency is known, these sources all spin fast at over 500 Hz; the rotationally induced mixing may explain burst recurrence times of the order of 10 min. Short recurrence time bursts generally occur at all mass accretion rates where normal bursts are observed, but for individual sources the short recurrence times may be restricted to a smaller interval of accretion rate. The fraction of such bursts is roughly 30%. We also report the shortest known recurrence time of 3.8 minutes.
42 citations
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TL;DR: The Marie Curie Curie Intra-European Fellowship within the 7th European Community Framework Programme, contract No. IEF 274805 as discussed by the authors was proposed by the European Commission.
Abstract: European Commission (Marie Curie Curie Intra-European Fellowship within the 7th European Community Framework Programme, contract No. IEF 274805)
42 citations
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TL;DR: In this paper, the number of quasiparticles saturates to 10?m?3 at temperatures below 160 mK, which is shown to limit the particle lifetime to 4 ms and lead to a generation-recombination noise limited noise equivalent power (NEP) of 1.5 × 10?19 W/Hz1/2.
Abstract: We present measurements of quasiparticle generation-recombination noise in aluminium Microwave Kinetic Inductance Detectors, the fundamental noise source for these detectors. Both the quasiparticle lifetime and the number of quasiparticles can be determined from the noise spectra. The number of quasiparticles saturates to 10 ?m?3 at temperatures below 160 mK, which is shown to limit the quasiparticle lifetime to 4 ms. These numbers lead to a generation-recombination noise limited noise equivalent power (NEP) of 1.5 × 10?19 W/Hz1/2. Since NEP ? Nqp, lowering the number of remnant quasiparticles will be crucial to improve the sensitivity of these detectors. We show that the readout power now limits the number of quasiparticles and thereby the sensitivity.
42 citations
Authors
Showing all 756 results
Name | H-index | Papers | Citations |
---|---|---|---|
George Helou | 144 | 662 | 96338 |
Alexander G. G. M. Tielens | 115 | 722 | 51058 |
Gijs Nelemans | 102 | 433 | 83486 |
Jelle Kaastra | 90 | 677 | 28093 |
Christian Frankenberg | 79 | 286 | 19353 |
Jeroen Homan | 72 | 354 | 15499 |
Nanda Rea | 72 | 446 | 19881 |
Mariano Mendez | 70 | 372 | 14475 |
Jorick S. Vink | 70 | 311 | 18826 |
Peter G. Jonker | 67 | 384 | 28363 |
Michael W. Wise | 64 | 271 | 19580 |
George Heald | 64 | 375 | 16261 |
Pieter R. Roelfsema | 64 | 257 | 18759 |
F. F. S. van der Tak | 63 | 314 | 16781 |
Norbert Werner | 63 | 254 | 10741 |