2019
DOI: 10.1093/mnrasl/slz140 View full text |Buy / Rent full text
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Abstract: We present statistical analysis of a fluence limited sample of over 1100 giant pulses from the Crab pulsar, with fluence > 130 Jy ms at ∼1330 MHz. These were detected in ∼260 hours of observation with the National Centre for Radio Astrophysics (NCRA)-15m radio telescope. We find that the pulse energy distribution follows a power law with index α ≈ −3 at least up to a fluence of ∼ 5 Jy s. The power law index agrees well with that found for lower energy pulses in the range 3-30 Jy ms. The fluence distribution of… Show more

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“…Normal pulses from pulsars tend to follow a log-normal energy distribution (see e.g. Burke-Spolaor et al 2012), whereas cumulative energies of giant pulses follow a power-law with index 𝛾 = −2 for the Crab pulsar (Popov & Stappers 2007;Bera & Chengalur 2019) and −2.63 ± 0.02 for J1823−3021A (Knight 2007;Abbate et al 2020). For magnetars a 𝛾 of −0.7 to −0.6 was found in X-rays (Göǧüş et al 1999;Göǧüş et al 2000).…”
Section: Burst Energy Distributionmentioning
“…Burke-Spolaor et al 2012), whereas energies of giant pulses follow a power-law (see e.g. Bera & Chengalur 2019;Abbate et al 2020). Similarly burst energies of magnetars also show log-normal distributions with a tail at high energies (Lynch et al 2015) and power-laws in X-rays (Göǧüş et al 1999;Göǧüş et al 2000).…”
Section: Introductionmentioning
“…So far, only the Crab pulsar is known to emit SGPs. The Crab GRP rate is a power-law function of F; from Bera & Chengalur (2019), we expect N (> F) = 10 −2 hr −1 (F/10 MJy µs) −1.8 . Assuming the typical pulse is broad band in frequency and that known sources such as the Crab will be coherently dedispersed, GReX could detect a 1 µs pulse at a fluence of a few MJy µs.…”
Section: Galactic Magnetarsmentioning
“…Stars show representative GPs or their components from the studies where both peak flux density and widths were measured, with the latter not biased by scattering (but still possibly below time resolution). Light blue color marks the Crab pulsar (Hankins et al 2003;Hankins & Eilek 2007;Karuppusamy et al 2010;Popov et al 2009;Bera & Chengalur 2019;Bhat et al 2008), beige corresponds to PSR B1937+21 (Kinkhabwala & Thorsett 2000;Soglasnov et al 2004;McKee et al 2019), yellow to PSR B1821-24A (Knight et al 2006;Bilous et al 2015), pink to PSR B0540-69 (Geyer et al 2021), and light violet to PSR B1957+21 (Main et al 2017). Finally, upward red triangle shows unresolved microstructure component for PSR B0950+08 from Hankins & Boriakoff (1978).…”
Section: What Can Psr B0950+08 Tell Us About Frbsmentioning
“…E ∼ 10 35 erg s −1 marks a transition between γ-ray and non γ-ray pulsars with implications for magnetospheric physics (Muslimov & Harding 2004;Watters et al 2009;Pierbattista et al 2012;Philippov & Spitkovsky 2018;Kalapotharakos et al 2019). Finally, the Crab pulsar, the most energetic pulsar in the Galaxy may emit radiation at up to 100 TeV and beyond (MAGIC Collaboration et al 2020) and continues to intrigue at lower energies (Yan et al 2018;Bera & Chengalur 2019).…”
Section: Introductionmentioning