ORCID Profile
0000-0002-3516-2152
Current Organisation
University of Amsterdam
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Publisher: American Association for the Advancement of Science (AAAS)
Date: 04-10-2002
Abstract: We have detected, at x-ray and radio wavelengths, large-scale moving jets from the microquasar XTE J1550–564. Plasma ejected from near the black hole traveled at relativistic velocities for at least 4 years. We present direct evidence for gradual deceleration in a relativistic jet. The broadband spectrum of the jets is consistent with synchrotron emission from high-energy (up to 10 tera–electron volts) particles that were accelerated in the shock waves formed within the relativistic ejecta or by the interaction of the jets with the interstellar medium. XTE J1550–564 offers a rare opportunity to study the dynamical evolution of relativistic jets on time scales inaccessible for active galactic nuclei jets, with implications for our understanding of relativistic jets from Galactic x-ray binaries and active galactic nuclei.
Publisher: American Astronomical Society
Date: 10-04-2006
DOI: 10.1086/500399
Publisher: Oxford University Press (OUP)
Date: 11-01-2010
Publisher: American Astronomical Society
Date: 10-02-2002
DOI: 10.1086/338038
Publisher: Oxford University Press (OUP)
Date: 13-11-2017
Publisher: Oxford University Press (OUP)
Date: 15-12-2017
Publisher: American Astronomical Society
Date: 12-2021
Abstract: 3FGL J1544.6−1125 is a candidate transitional millisecond pulsar (tMSP). Similar to the well-established tMSPs—PSR J1023+0038, IGR J18245−2452, and XSS J12270−4859—3FGL J1544.6−1125 shows γ -ray emission and discrete X-ray “low” and “high” modes during its low-luminosity accretion-disk state. Coordinated radio/X-ray observations of PSR J1023+0038 in its current low-luminosity accretion-disk state showed rapidly variable radio continuum emission—possibly originating from a compact, self-absorbed jet, the “propellering” of accretion material, and/or pulsar moding. 3FGL J1544.6−1125 is currently the only other (candidate) tMSP system in this state, and can be studied to see whether tMSPs are typically radio-loud compared to other neutron star binaries. In this work, we present a quasi-simultaneous Very Large Array and Swift radio/X-ray c aign on 3FGL J1544.6−1125. We detect 10 GHz radio emission varying in flux density from 47.7 ± 6.0 μ Jy down to ≲15 μ Jy (3 σ upper limit) at four epochs spanning three weeks. At the brightest epoch, the radio luminosity is L 5 GHz = (2.17 ± 0.17) × 10 27 erg s −1 for a quasi-simultaneous X-ray luminosity L 2–10 keV = (4.32 ± 0.23) × 10 33 erg s −1 (for an assumed distance of 3.8 kpc). These luminosities are close to those of PSR J1023+0038, and the results strengthen the case that 3FGL J1544.6−1125 is a tMSP showing similar phenomenology to PSR J1023+0038.
Publisher: American Astronomical Society
Date: 20-02-2002
DOI: 10.1086/338140
Publisher: Oxford University Press (OUP)
Date: 15-10-2013
Publisher: Elsevier BV
Date: 06-2015
Publisher: Springer Science and Business Media LLC
Date: 26-09-2018
DOI: 10.1038/S41586-018-0524-1
Abstract: Relativistic jets are observed throughout the Universe and strongly affect their surrounding environments on a range of physical scales, from Galactic binary systems
Publisher: American Astronomical Society
Date: 20-02-2018
Publisher: Springer Science and Business Media LLC
Date: 07-2003
DOI: 10.1038/NATURE01732
Publisher: American Astronomical Society
Date: 04-12-2013
Publisher: American Astronomical Society
Date: 02-2003
DOI: 10.1086/368105
Publisher: EDP Sciences
Date: 2016
Publisher: American Astronomical Society
Date: 08-08-2003
DOI: 10.1086/378260
Publisher: American Astronomical Society
Date: 15-06-2015
Publisher: American Astronomical Society
Date: 07-2015
Publisher: Oxford University Press (OUP)
Date: 16-05-2012
Publisher: American Astronomical Society
Date: 14-06-2019
Publisher: Oxford University Press (OUP)
Date: 04-07-2016
Publisher: American Astronomical Society
Date: 11-12-2018
Publisher: Elsevier BV
Date: 06-2004
Publisher: Oxford University Press (OUP)
Date: 19-05-2017
Publisher: American Astronomical Society
Date: 10-12-2007
DOI: 10.1086/522516
Publisher: Oxford University Press (OUP)
Date: 12-01-2018
DOI: 10.1093/MNRAS/STY081
Publisher: EDP Sciences
Date: 24-03-2006
Publisher: Oxford University Press (OUP)
Date: 24-06-2016
Publisher: American Astronomical Society
Date: 29-08-2018
Publisher: American Astronomical Society
Date: 15-04-2009
Publisher: Elsevier BV
Date: 10-2003
Publisher: American Astronomical Society
Date: 10-01-2003
DOI: 10.1086/344540
Publisher: Oxford University Press (OUP)
Date: 21-12-2018
Publisher: Oxford University Press (OUP)
Date: 11-06-2018
Publisher: Oxford University Press (OUP)
Date: 31-12-2015
Publisher: American Astronomical Society
Date: 27-12-2016
Publisher: Oxford University Press (OUP)
Date: 02-03-2019
DOI: 10.1093/MNRAS/STZ616
Abstract: We report on observations of black hole Swift J1357.2–0933, a member of the modest population of very faint X-ray transients. This source has previously shown intense dips in the optical light curve, a phenomena that has been linked to the existence of a ‘unique toroidal structure’ in the inner region of the disc, seen at a high inclination. Our observations, carried out by the Neil Gehrels Swift and NuSTAR X-ray observatories, do not show the presence of intense dips in the optical light curves. We find that the X-ray light curves do not show any features that would straightforwardly support an edge-on configuration or high inclination configuration of the orbit. This is similar to what was seen in the X-ray observations of the source during its 2011 outburst. Moreover, the broad-band spectra were well described with an absorbed power-law model without any signatures of cut-off at energies above 10 keV, or any reflection from the disc or the putative torus. Thus, the X-ray data do not support the unique ‘obscuring torus’ scenario proposed for J1357. We also performed a multiwavelength study using the data of X-ray telescope and Ultraviolet/Optical Telescope aboard Swift, taken during the ∼4.5 months duration of the 2017 outburst. This is consistent with what was previously inferred for this source. We found a correlation between the simultaneous X-ray and ultraviolet/optical data and our study suggests that most of the reprocessed flux must be coming out in the ultraviolet.
Publisher: EDP Sciences
Date: 29-01-2016
Publisher: Oxford University Press (OUP)
Date: 11-02-2009
Location: United Kingdom of Great Britain and Northern Ireland
Location: United States of America
No related grants have been discovered for Rudi Wijnands.