A giant γ-ray flare from the magnetar SGR 1806–20

By David M. Palmer, S. Barthelmy, N. Gehrels, R. Kippen, T. Cayton, C. Kouveliotou, David Eichler, R. Wijers, P. Woods, J. Granot and 18 more. Nature, 2005

380 citations recorded by the source corpus.

Subfields: Astronomy and Astrophysics

View Paper: https://www.semanticscholar.org/paper/ac0c60c9b7e25850f17e90036dac43d930a02f72

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In Astronomy and Astrophysics

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Citations in the corpus

• The strongest cosmic magnets: soft gamma-ray repeaters and anomalous X-ray pulsars (2008, background): “No excess of short BATSE bursts is found in the direction of the Virgo cluster (d ∼ 17 Mpc), nor short bursts were consistent with the direction of the closest galaxieswith a high star formation rate (Palmer et al. 2005; Popov and Stern 2006).”
• Millisecond Magnetar Birth Connects FRB 121102 to Superluminous Supernovae and Long-duration Gamma-Ray Bursts (2017, methodology): “If the FRB source were in fact giant magnetic flares, we would expect coincident gamma-ray emission from FRB 121102, of luminosity Lγ ∼ 1047 erg s−1 similar to Giant flares in our galaxy (e.g. Palmer et al. 2005).”
• Discovery of Fast X-Ray Oscillations during the 1998 Giant Flare from SGR 1900+14 (2005, background): “The most recent event, from SGR 1806-20 (hereafter, 1806), was also the most luminous, generating upwards of 10 46 erg in a matter of minutes (Terasawa et al. 2005; Palmer et al. 2005).”
• Detection with RHESSI of High-Frequency X-Ray Oscillations in the Tailof the 2004 Hyperflare from SGR 1806–20 (2005, background): “Three giant flares have been detected since the advent of satellite-borne high energy detectors: in 1979, from SGR 0526-66 (Mazets et al. 1979); in 1998, from SGR 1900+14 (Hurley et al. 1999); and in 2004 from SGR 1806-20 (Terasawa et al. 2005; Palmer et al. 2005).”
• TIME-RESOLVED PROPERTIES AND GLOBAL TRENDS IN dMe FLARES FROM SIMULTANEOUS PHOTOMETRY AND SPECTRA (2013, background): “…called soft gamma ray repeaters (SGRs) that occur relatively close to the Milky Way and account for only a few percent of the short/hard GRB’s (Palmer et al. 2005); the current leading model is the merging of two compact objects, one of which is a neutron star (Blinnikov et al. 1984; Nakar…”
• THE AFTERGLOWS OF SWIFT-ERA GAMMA-RAY BURSTS. II. TYPE I GRB VERSUS TYPE II GRB OPTICAL AFTERGLOWS (2008, background): “…2007a): In analogy to Type Ia and Type II supernovae, GRBs can be classified 1Note that we do not consider the “superflares” of Soft Gamma-Repeaters (SGRs) in this work, which have also been suggested as a source for part of the short GRB population (e.g., Hurley et al. 2005; Palmer et al. 2005).”
• Cosmological Fast Radio Bursts from Binary Neutron Star Mergers (2013, background): “…repeaters (SGRs) are suggested as a promising candidate by Popov & Postnov (2007) and Thornton et al. (2013), because of the event rate consistent with that of FRBs (Ofek 2007) and sufficient total energy to explain the FRB radio flux (Hurley et al. 2005; Palmer et al. 2005; Terasawa et al. 2005).”
• A Flaring Magnetar in FRB 121102? (2017, background): “It radiated E 2 1046~ ´g erg in gamma-rays (Palmer et al. 2005) and was followed by radio afterglow emitted by mildly relativistic ejecta (Gaensler et al. 2005).”
• Five new fast radio bursts from the HTRU high-latitude survey at Parkes: First evidence for two-component bursts (2015, background): “…Thornton et al. 2013; Kulkarni et al. 2014) The initial gamma-ray burst usually lasts just a fraction of a second, and is then followed by hard X-ray emission with power modulated at what is thought to be the spin period of the underlying neutron star (e.g. Hurley et al. 2005; Palmer et al. 2005).”
• Short-hard gamma-ray bursts (2007, methodology): “With a luminosity of ∼ 1047 erg/s such flares can be detected by BATSE up to ≈ 50 Mpc, suggesting that a significant fraction of the BATSE SHB sample is comprised of similar extra-galactic flares (Dar, 2005a,b; Palmer et al. , 2005; Hurley et al. , 2005; Nakar et al. , 2006).”
• Gamma-Ray Bursts in the Swift Era (2009, background): “It has been noted (Hurley et al. 2005, Palmer et al. 2005, Nakar et al. 2006b) that the giant flare (GF) observed from the putative galactic magnetar source SGR1806-20 in December 2004 (Gaensler et al. 2005) could have looked like a typical short GRB had it occurred much farther away, thus making…”
• A Nearby Repeating Fast Radio Burst in the Direction of M81 (2021, background): “Moreover, giant magnetar flares with a total isotropic luminosity of ∼1046 erg, like that from SGR 1806−20 (Palmer et al. 2005), should be easily detectable by the Swift Burst Alert Telescope (BAT) and Fermi/GBM, which have flux sensitivities of ∼10−7 erg cm−2 s−1 in the 15–150 keV band (A.…”
• DISCERNING THE PHYSICAL ORIGINS OF COSMOLOGICAL GAMMA-RAY BURSTS BASED ON MULTIPLE OBSERVATIONAL CRITERIA: THE CASES OF z = 6.7 GRB 080913, z = 8.2 GRB 090423, AND SOME SHORT/HARD GRBs (2009, background): “9 It is widely accepted that at least a fraction of short/hard GRBs are the giant flares of soft gamma-ray repeaters in nearby galaxies (Palmer et al. 2005; Tanvir et al. 2005).”
• Physics of strongly magnetized neutron stars (2006, background): “Such superflares have been observed in three SGR sources, SGR0526-66 (the famous 5th March 1979 event), SGR1900+14 (Hurley et al 1999) and very recently in SGR1806-20 (Hurley et al 2005, Palmer et al 2005).”