Pulsar spectra of radio emission

By O. Maron, J. Kijak, Michael Kramer, R. Wielebinski. 2000

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We have collected pulsar flux density observa- tions and compiled spectra of 281 objects. The database of Lorimer et al. (1995) has been extended to frequencies higher than 1.4 GHz and lower than 300 MHz. Our results show that above 100 MHz the spectra of the majority of pulsars can be described by a simple power law with av- erage value of spectral index = 1:8 0:2. A rigorous analysis of spectral tting revealed only about 10% of spectra which can be modelled by the two power law. Thus, it seems that single power law is a rule and the two power law spectrum is a rather rare exception, of an unknown origin, to this rule. We have recognized a small number of pulsars with almost flat spectrum ( 1:0) in the wide frequency range (from 300 MHz to 20 GHz) as well as few pulsars with a turn-over at unusually high frequency ( 1G Hz).

Subfields: Astronomy and Astrophysics, Instrumentation

View Paper: https://www.semanticscholar.org/paper/c9ab079c66c137cbf58fd738fe1bf4cac2424570

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Citations in the corpus

The pulsar spectral index distribution (2013, methodology): “Maron et al. (2000) also found evidence for ∼ 10% of pulsars in their sample being best fit using a double power law, described by parameters α1 at lower frequencies and α2 at higher frequencies.”
Science with the Murchison Widefield Array (2012, methodology): “It is at MWA frequencies that pulsar emission peaks (Maron et al. 2000; Kondratiev et al. 2012) and that interstellar propagation effects are easiest to study, but this wavelength range has been neglected for years because of difficulties in processing the data and the increasing prevalence of…”
Spectral properties of 441 radio pulsars (2017, background): “Later Maron et al. (2000) extended the work of Lorimer et al. (1995) using mainly the same set of pulsars, but broadened the frequency coverage.”
The Parkes Multibeam Pulsar Survey - III. Young Pulsars and the Discovery and Timing of 200 Pulsars (2003, background): “For a radio spectral index of −1.7 (Maron et al. 2000), these numbers may be converted to the more commonly quoted 400 MHz luminosity by multiplying by 8.4.”
On the birthrates of Galactic neutron stars (2008, background): “The spectra for this emission typically increases with decreasing radio frequency with mean spectral index of −1.8 (Maron et al. 2000) before peaking in the range 100–300 MHz (Malofeev et al. 1994).”
The Parkes Multibeam Pulsar Survey – II. Discovery and timing of 120 pulsars (2002, background): “However, this difference in spectral indices is not confirmed by Malofeev (1996) or Maron et al. (2000).”
THE SECOND FERMI LARGE AREA TELESCOPE CATALOG OF GAMMA-RAY PULSARS (2013, unknown): “For most pulsars α has not been measured, and we use an average value 〈α〉 = −1.7, a middle ground between −1.6 from Lorimer et al. (1995) and −1.8 from Maron et al. (2000).”
Observing pulsars and fast transients with LOFAR (2011, background): “Furthermore, there is evidence for complexity in the shape of pulsar spectra (e.g. Maron et al. 2000), which again is an important signature of the pulsar emission process that LOFAR’s wide-band data can probe.”
On the origin of a highly dispersed coherent radio burst (2012, background): “Pulsar Giant Pulse: Pulsar spectra are typically steep: their mean spectral index is −1.8, with values steeper than −1 being very uncommon (Maron et al. 2000).”