THE<i>FERMI</i>GAMMA-RAY BURST MONITOR

Meegan, C.; Lichti, G.; Bhat, P. N.; Bissaldi, E.; Briggs, M. S.; Connaughton, V.; Diehl, R.; Fishman, G. J.; Greiner, J.; Hoover, A.; Horst, A. J. van der; Kienlin, A. von; Kippen, R. M.; Kouveliotou, C.; McBreen, S.; Pačiesas, W. S.; Preece, R.; Steinle, H.; Wallace, Mark; Wilson, Robert B.; Wilson-Hodge, C.

doi:10.1088/0004-637x/702/1/791

Cited by 1,423 publications

(1,319 citation statements)

References 21 publications

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“…Among the 101 events, only one that was observed simultaneously with RHESSI had emission above 1 MeV: the X1.8-class flare on October 23, 2012. We also checked the data from the Gamma-Ray Burst Monitor (GBM) [28] onboard the Fermi spacecraft and found another event with emission above 1 MeV: the M7.9-class flare on June 25, 2015.…”

Section: Event Selectionmentioning

confidence: 99%

Capability of the accelerated protons as the origin of white-light emission of solar flare

Watanabe¹,

Masuda²,

Ohno³

2017

Proceedings of 35th International Cosmic Ray Conference — PoS(ICRC2017)

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In association with strong solar flares, we sometimes observe enhancements of visible continuum radiation, which is known as a "white-light flare". As most white-light (WL) events show close correlations in time and location with hard X-rays and/or radio emission, there is some consensus that WL emission originates from accelerated particles, especially non-thermal electrons. One model proposes that WL is emitted near the photosphere; however, non-thermal electrons are thermalized in the chromosphere and cannot reach the photosphere. Thus, there is a problem: how can the energy of non-thermal electrons − and/or other accelerated particles such as high-energy protons − propagate to the photosphere and produce WL emission? In the present study, we investigate the possibility that accelerated protons may produce the WL emission of solar flares. We found 51 WL events observed by Hinode/SOT. Among them, gamma-rays with energies greater than 1 MeV were observed only in the X1.8-class flare on October 23, 2012 and in the M7.9-class flare on June 25, 2015. Focusing on these flare events, we compare the energetics of WL emission and of accelerated ion fluxes. We find that it is difficult for accelerated ions to provide sufficient energy to account for WL emission.

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Section: Event Selectionmentioning

confidence: 99%

Capability of the accelerated protons as the origin of white-light emission of solar flare

Watanabe¹,

Masuda²,

Ohno³

2017

Proceedings of 35th International Cosmic Ray Conference — PoS(ICRC2017)

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“…GBM is an all-sky monitor whose primary objective is to extend the energy range over which gamma-ray bursts are observed in the Large Area Telescope on Fermi (Meegan et al 2009). GBM consists of 12 NaI detectors with a diameter of 12.7 cm and a thickness of 1.27 cm and two bismuth germanate (BGO) detectors with a diameter and thickness of 12.7 cm.…”

Section: The Fermi-gbm X-ray Burst Monitormentioning

confidence: 99%

“…Due to the gradual rollover in the expected photon spectrum between 12 and 25 keV and the steep drop in effective area in data from CTIME channel 0 (∼8-12 keV) (Meegan et al 2009), channel 1 (12-25 keV) is the channel most sensitive to these XRBs. The choice of 8.2 s timing resolution for channel 1 data is a compromise between the desire to maximize our sensitivity to these events and the time demands of this labor-intensive process, and limits the minimal detectable burst duration to around 10 s. Variations in background count rate over the Fermi orbit, caused both by changes in geomagnetic latitude and by varying spacecraft attitude, prevent visual identification of very long bursts.…”

Section: Data Selectionmentioning

confidence: 99%

“…The Gamma-ray Burst Monitor (GBM) onboard the Fermi observatory has an instantaneous FOV of about 75% of the sky (Meegan et al 2009) and is sensitive to photon energies down to 8 keV. Even though it was designed to detect and characterize gamma-ray bursts (GRBs), these characteristics make GBM a unique instrument to detect rare, short, and bright X-ray bursts (XRBs).…”

Section: Introductionmentioning

confidence: 99%

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The Fermi–gbm Three-Year X-Ray Burst Catalog

Jenke

Linares

Connaughton

et al. 2016

ApJ

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The Fermi Gamma-ray Burst Monitor (GBM) is an all-sky gamma-ray monitor well known in the gamma-ray burst (GRB) community. Although GBM excels in detecting the hard, bright extragalactic GRBs, its sensitivity above 8 keV and its all-sky view make it an excellent instrument for the detection of rare, short-lived Galactic transients. In 2010 March, we initiated a systematic search for transients using GBM data. We conclude this phase of the search by presenting a three-year catalog of 1084 X-ray bursts. Using spectral analysis, location, and spatial distributions we classified the 1084 events into 752 thermonuclear X-ray bursts, 267 transient events from accretion flares and X-ray pulses, and 65 untriggered gamma-ray bursts. All thermonuclear bursts have peak blackbody temperatures broadly consistent with photospheric radius expansion (PRE) bursts. We find an average rate of 1.4 PRE bursts per day, integrated over all Galactic bursters within about 10 kpc. These include 33 and 10 bursts from the ultra-compact X-ray binaries 4U0614+09 and 2S0918-549, respectively. We discuss these recurrence times and estimate the total mass ejected by PRE bursts in our Galaxy.

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“…For Fermi-GBM the threshold is p th = 0.71 photons cm −2 s −1 in the energy range of 50-300 keV (Meegan et al 2009). In this case we write…”

Section: Gamma-ray Burstsmentioning

confidence: 99%

Implications ofFermi-LAT observations on the origin of IceCube neutrinos

Wang¹,

Zhao²,

Li³

2014

J. Cosmol. Astropart. Phys.

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The IceCube (IC) collaboration recently reported the detection of TeV-PeV extraterrestrial neutrinos whose origin is yet unknown. By the photon-neutrino connection in pp and pγ interactions, we use the Fermi-LAT observations to constrain the origin of the IC detected neutrinos. We find that Galactic origins, i.e., the diffuse Galactic neutrinos due to cosmic ray (CR) propagation in the Milky Way, and the neutrinos from the Galactic point sources, may not produce the IC neutrino flux, thus these neutrinos should be of extragalactic origin. Moreover, the extragalactic gamma-ray bursts (GRBs) may not account for the IC neutrino flux, the jets of active galactic nuclei may not produce the IC neutrino spectrum, but the starburst galaxies (SBGs) may be promising sources. As suggested by the consistency between the IC detected neutrino flux and the Waxman-Bahcall bound, GRBs in SBGs may be the sources of both the ultrahigh energy, 10 19 eV, CRs and the 1 − 100 PeV CRs that produce the IC detected TeV-PeV neutrinos.

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THEFERMIGAMMA-RAY BURST MONITOR

Cited by 1,423 publications

References 21 publications

Capability of the accelerated protons as the origin of white-light emission of solar flare

Capability of the accelerated protons as the origin of white-light emission of solar flare

The Fermi–gbm Three-Year X-Ray Burst Catalog

Implications ofFermi-LAT observations on the origin of IceCube neutrinos

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