ライフサイエンスコーパス: gamma-ray

1 cells relative to low-LET radiation such as gamma rays.

2 led ~0.87-1.5% energy resolution for 662-keV gamma rays.

3 4)Cu is less effective for cell killing than gamma-rays.

4 rmation is obtained through the detection of gamma-rays.

5 mortality rates in mice exposed to 6-9 Gy of gamma-rays.

6 ormal human cells following irradiation with gamma-rays.

7 stantially lower than to equivalent doses of gamma-rays.

8 es) than by low linear energy transfer X- or gamma-rays.

9 al curve of MCF7 /: HER2-18 cells exposed to gamma-rays.

10 ccus radiodurans to survive extreme doses of gamma-rays (12,000 Gy), 20 times greater than Escherichi

11 ulated in cells with low survival after 2-Gy gamma-rays; 14 genes identified lines more sensitive to

12 t Adobo, sterilized by exposure to high-dose gamma rays (25 kGy) in combination with conventional tre

13 41)Am alpha particles (5.49 MeV) and (241)Am gamma-rays (59.5 keV), with full widths at half-maximum

14 dy, the mortality of mice exposed to 7 Gy of gamma-rays (7 Gy GIARS mice) was completely controlled a

15 major detectable phenomena: a short burst of gamma-rays, a gravitational-wave signal, and a transient

16 ture radiation as the origin of the observed gamma rays above 100 GeV.

17 normal human fibroblasts after exposures to gamma-rays, aiming to elucidate the involvement of ROS a

18 H-pUC19 plasmid samples were irradiated with gamma-rays, alkali-denatured, dephosphorylated, and kina

19 e hydrogen concentrations observed by Dawn's Gamma Ray and Neutron Detector to assess potential volat

20 Using Dawn's Gamma Ray and Neutron Detector, we tested models of Vest

21 RAD9 depletion enhances sensitivity to UV, gamma rays and menadione, but ectopic expression of RAD9

22 adio light curve of GW170817, as well as the gamma-ray and X-ray emission (and possibly also the ultr

23 1m)Cd perturbed angular correlation (PAC) of gamma-rays and (113)Cd NMR spectroscopy.

24 Radiation stability was examined using gamma-rays and 5 MeV He(2+) ions to simulate alpha parti

25 , this outflow is manifested in the pulse of gamma-rays and a long-lived radio afterglow.

26 Gamma-ray bursts (GRBs) are brief flashes of gamma-rays and are considered to be the most energetic e

27 uclides that do not emit either positrons or gamma-rays and are, thus, unsuitable for use with curren

28 n efficiency under continuous irradiation of gamma-rays and light for 1535 h, where gamma-rays have a

29 speeds, the jets should be strong sources of gamma-rays and neutrino emission.

30 pulse in plasma can convert its energy into gamma-rays and then e (-) e (+) pairs via the multi-phot

31 g, we also detected new mutations induced by gamma-rays and UV.

32 bility study of perovskite solar cells under gamma-rays and visible light simultaneously is reported.

33 -photon imaging, images are created from the gamma rays (and occasionally X-rays) directly emitted by

34 inducing agents, including neocarzinostatin, gamma rays, and etoposide, and found that H3K36me3 and H

35 mals irradiated with ultraviolet or ionizing gamma rays, and is the major factor in the conditioned m

36 m in ways that heat the ambient gas, produce gamma rays, and produce light element isotopes.

37 ecently only seven were observed to pulse in gamma rays, and these were all discovered at other wavel

38 HEU has a low neutron emission rate and most gamma rays are low energy and easily shielded.

39 In this scheme, bright gamma-rays are generated by radiation-trapped electrons

40 a from the spectrometer on the International Gamma-Ray Astrophysics Laboratory satellite.

41 ously, the Fermi and INTEGRAL (INTErnational Gamma-Ray Astrophysics Laboratory) telescopes detected a

42 It involves measurement of prompt gamma-rays at 429, 718, and 2125 keV from (10)B(p,alphag

43 The CSS's sensors include a gamma-ray attenuation densitometer to measure bulk densi

44 targets, the Inner Galaxy and the isotropic gamma-ray background.

45 08A, four minutes after its discovery in the gamma-ray band, decreasing to P = 16(+5)(-4) per cent ov

46 The generation of X-rays and gamma-rays based on synchrotron radiation from free elec

47 Our findings require that these gamma rays be produced more than 10 stellar radii from t

48 then used to reconstruct the spectrum of the gamma-ray beam.

49 he high-resolution spectrometry of high-flux gamma-ray beams with energies per photon in the multi-Ge

50 Globular clusters are expected to emit gamma rays because of the large populations of milliseco

51 Gamma-ray binaries are stellar systems containing a neut

52 A search for gamma-ray binaries with the Fermi Large Area Telescope (

53 1FGL J1018.6-5856 is thus a gamma-ray binary, and its detection suggests the presenc

54 pe Artemis completely restored resistance to gamma-rays, bleomycin and neocarzinostatin, and also res

55 Gamma-ray burst (GRB) 130427A is one of the most energet

56 y be revealed by observing sharp features in gamma-ray burst (GRB) light-curves.

57 aneously with x-rays and gamma rays during a gamma-ray burst (GRB) provides clues about the nature of

58 e initial burst of gamma-rays that defines a gamma-ray burst (GRB), expanding ejecta collide with the

59 trarelativistic, highly collimated ejecta (a gamma-ray burst afterglow).

60 such events nearby and the brightness of the gamma-ray burst afterglow, which dominates the emission

61 ma-ray burst seen off-axis, a low-luminosity gamma-ray burst at high redshift, or a tidal disruption

62 ed rebrightening in the afterglow of a short gamma-ray burst at redshift z = 0.356, although findings

63 8 galaxies that, together with reports of a gamma-ray burst at z approximately 8.2, constitute the e

64 ated by an ultra-relativistic jet within the gamma-ray burst expanding and decelerating into the medi

65 was associated with the ultra-long-duration gamma-ray burst GRB 111209A, at a redshift z of 0.677.

66 per cent in the immediate afterglow of Swift gamma-ray burst GRB 120308A, four minutes after its disc

67 uch an event accompanying the short-duration gamma-ray burst GRB 130603B.

68 h the gravitational-wave source GW170817 and gamma-ray burst GRB 170817A associated with a galaxy at

69 ova SN 2017iuk, which is associated with the gamma-ray burst GRB 171205A.

70 The Gamma-ray Burst Monitor (GBM) on board the Fermi spacecr

71 eral possible explanations including a short gamma-ray burst seen off-axis, a low-luminosity gamma-ra

72 r mergers may not be associated with a short gamma-ray burst(11,12).

73 nsistent with the radio afterglow of a short gamma-ray burst, and its existence and timescale do not

74 ger, GW170817, along with a coincident short gamma-ray burst, GRB 170817A.

75 Hours to days after the gamma-ray burst, polarization levels are low (P < 4 per

76 rgy emission has lasted much longer than any gamma-ray burst, whereas its peak luminosity was approxi

77 ncident with GW170817 and with a weak, short gamma-ray burst.

78 been associated with an ultra-long-duration gamma-ray burst.

79 Gamma-ray bursts (GRBs) are brief flashes of gamma-rays

80 Gamma-ray bursts (GRBs) are bright flashes of gamma rays

81 Gamma-ray bursts (GRBs) are most probably powered by col

82 Gamma-ray bursts (GRBs) are short-lived, luminous explos

83 Long-duration gamma-ray bursts (GRBs) are thought to result from the e

84 Long duration gamma-ray bursts (GRBs) mark the explosive death of some

85 Long-duration gamma-ray bursts (GRBs) originate from ultra-relativisti

86 the jets and the role of magnetic fields in gamma-ray bursts (GRBs) remains unclear.

87 f and intense flashes of gamma-rays known as gamma-ray bursts (GRBs), followed by longer-lived afterg

88 lativistic jets, which have been observed in gamma-ray bursts (GRBs), microquasars, and at the center

89 Long duration gamma-ray bursts (GRBs), the brightest events since the

90 follow-up of gravitational-wave (GW), short gamma-ray bursts (sGRBs) or optical surveys, a large sam

91 ledge gained from the neighbouring fields of gamma-ray bursts and radio pulsars has also offered insi

92 ted (the inner heliosheath, accretion disks, gamma-ray bursts and so on).

93 ergers are the progenitors of short-duration gamma-ray bursts and the sites of significant production

94 f other kinds of transient events, including gamma-ray bursts and tidal disruption events.

95 Long gamma-ray bursts are associated with energetic, broad-li

96 Short-duration gamma-ray bursts are intense flashes of cosmic gamma-ray

97 properties of stars that produce spectacular gamma-ray bursts at the end of their lives.

98 tra-long-duration (more than 10,000 seconds) gamma-ray bursts has recently been suggested.

99 rate offset from the galaxy centre, as short gamma-ray bursts often do(15,16).

100 ii than those producing normal long-duration gamma-ray bursts or in the tidal disruption of a star.

101 highly collimated, energetic and femtosecond gamma-ray bursts that are produced in this way may provi

102 n EM170817 are dissimilar to classical short gamma-ray bursts with ultrarelativistic jets.

103 stars are known to be associated with short gamma-ray bursts(1-4).

104 red an active phase by emitting intense soft gamma-ray bursts(15).

105 arly evolution of supernovae associated with gamma-ray bursts(3).

106 au that follows up to half of observed short gamma-ray bursts(9,10).

107 pped supernovae that are not associated with gamma-ray bursts, an excess of high-velocity (roughly 30

108 Ic supernovae associated with long-duration gamma-ray bursts, and its spectrum is distinctly differe

109 tors for both type Ic-bl supernovae and long gamma-ray bursts, and provide a viable mechanism for the

110 these faint supernovae to some long-duration gamma-ray bursts, because extremely faint, hydrogen-stri

111 om three astrophysical sources - supernovae, gamma-ray bursts, large asteroid impacts, and passing-by

112 ovae have been proposed to produce such long gamma-ray bursts, the afterglows of which do not show ev

113 on-star mergers as the drivers of short hard-gamma-ray bursts.

114 up all supernovae that are connected to long gamma-ray bursts.

115 associated with the emission of ultra-bright gamma-ray bursts.

116 breaks and sublethal-type damage induced by gamma-rays, but not by alpha-particles.

117 oft X-ray free-electron lasers and producing gamma-rays by inverse Compton scattering.

118 detector can be used to acquire an image; no gamma-ray camera is needed.

119 Nuclear imaging using gamma-ray cameras offers the benefits of using small qua

120 Gamma rays can probe their spreading through the ambient

121 amma-ray bursts (GRBs) are bright flashes of gamma rays coming from the cosmos.

122 gents and in cultured human cells exposed to gamma-rays, d(G[8-5m]T) can be recognized and incised by

123 We evaluate the new Bayesian approach using gamma-ray data and are able to identify weapons-grade pl

124 the fluorescence camera (VITOM) to either a gamma-ray detection probe (GP; VITOM-GP) or a portable g

125 the fluorescence camera (VITOM) to either a gamma-ray detection probe (GP; VITOM-GP) or a portable g

126 were surgically localized using blue dye, a gamma-ray detection probe, a portable gamma-camera, and

127 a promising material for efficient X-ray and gamma-ray detection.

128 A single gamma-ray detector can be used to acquire an image; no g

129 om-temperature compound-semiconductor X- and gamma-ray detector material.

130 X- and gamma-ray detectors have broad applications ranging from

131 lood (DTotal) was the sum of mean whole-body gamma-ray dose component (Dgamma) from uncollimated gamm

132 ght generated simultaneously with x-rays and gamma rays during a gamma-ray burst (GRB) provides clues

133 ssue ablation technology, which uses X-rays, gamma rays, electron beams, protons, or high-intensity f

134 nmol F/cm(2)) determined by particle-induced gamma ray emission (PIGE) spectroscopy, measured before

135 i Large Area Telescope detection of variable gamma-ray emission (0.1 to 10 billion electron volts) fr

136 We report simple particle induced gamma-ray emission (PIGE) methods using a 4 MeV proton b

137 d X-ray emission (PIXE) and particle-induced gamma-ray emission (PIGE).

138 opose an all-optical scheme for ultra-bright gamma-ray emission and dense positron production with la

139 ows will be the best candidates for studying gamma-ray emission at energies ranging from gigaelectron

140 atory (HAWC), of extended tera-electron volt gamma-ray emission coincident with the locations of two

141 ation (seconds to tens of minutes) X-ray and gamma-ray emission coming from thunderclouds.

142 ed away from the line of sight, the observed gamma-ray emission could not have originated from such a

143 ctral shape of 47 Tucanae is consistent with gamma-ray emission from a population of millisecond puls

144 he extremely energetic and long-lived prompt gamma-ray emission from GRB 160625B.

145 Here we report observations of gamma-ray emission from the microquasar V404 Cygni durin

146 Variable x-ray and gamma-ray emission is characteristic of the most extreme

147 icle-induced X-ray emission-particle-induced gamma-ray emission mappings and of the color and TM elem

148 he extraordinarily bright prompt optical and gamma-ray emission of GRB 080319B that provide diagnosti

149 ontaining a neutron star or black hole, with gamma-ray emission produced by an interaction between th

150 Particle-induced X-ray and gamma-ray emission spectroscopy (PIXE, PIGE) techniques

151 hows a sharp maximum coinciding with maximum gamma-ray emission, as well as an O6V((f)) star optical

152 are bright sources of very-high-energy (VHE) gamma-ray emission, it is not yet known where the VHE em

153 ve been discovered exclusively through their gamma-ray emission, yet it is expected that a larger pop

154 he seed photon population at the location of gamma-ray emission.

155 We report the detection of gamma-ray emissions above 200 megaelectron volts at a si

156 nfiguration is employed to record the prompt gamma rays emitted along the proton path.

157 due to the high penetration of the energetic gamma rays emitted by (137)Cs, the individual will be ex

158 d within radiation portal monitors to detect gamma rays emitted from conveyances crossing ports of en

159 Both the 79 keV x-rays and the 440 keV gamma-rays emitted by (213)Bi could be imaged.

160 d among novae, explaining why many novae are gamma-ray emitters.

161 s were labelled with both alpha-particle and gamma-ray emitting isotopes, at high specific activities

162 report high-resolution radio imaging of the gamma-ray-emitting nova V959 Mon.

163 agnetically active species with positron- or gamma-ray-emitting radionuclides.

164 a-ray repeater (SGR) bursts were detected in gamma-ray energies.

165 anisms for applications in X-ray imaging and gamma-ray energy spectroscopy.

166 thermally driven stochastic switching in the gamma ray environment.

167 Knockout and mutant cells were sensitive to gamma-rays, etoposide, temozolamide, and endogenously ge

168 ignal in normal human cells following gamma (gamma)-ray exposure, but are not required for its recept

169 ity to image high-intensity fast-neutron and gamma-ray fields simultaneously.

170 , revealing a period of extremely strong VHE gamma-ray flares accompanied by a strong increase of the

171 Terrestrial gamma ray flashes (TGFs) are a class of enigmatic electr

172 coveries, such as sprites, jets, terrestrial gamma ray flashes, and fast positive breakdown, highligh

173 hen compared with events such as terrestrial gamma-ray flashes.

174 EA), the same process underlying terrestrial gamma-ray flashes.

175 During these outbursts, the gamma-ray flux from the nebula increased by factors of f

176 For this glow, the gamma-ray flux observed is close to the value at which r

177 The optical and >100-megaelectron volt (MeV) gamma-ray flux show a close correlation during the first

178 s calculations, leading to the prediction of gamma-ray fluxes from as many as several hundred dark cl

179 DT) neutron generator to detect neutrons and gamma rays from induced fission in HEU.

180 We report the detection of pulsed gamma rays from the Crab pulsar at energies above 100 gi

181 We have detected polarized gamma rays from the vicinity of the Crab pulsar using da

182 celerated effectively to produce pi(0) decay gamma-rays from proton-proton interactions.

183 00-kilovolt accelerator(11) and detected the gamma-rays from the nuclear reaction under study with a

184 ory that was radiated from 1961 to 1978 with gamma rays (Gamma Forest), the ecosystem has not yet ful

185 Gamma-ray 'glows' are long duration (seconds to tens of

186 from the source, in association with a soft gamma-ray/hard-X-ray flare(18-21).

187 on of gamma-rays and light for 1535 h, where gamma-rays have an accumulated dose of 2.3 Mrad.

188 e demonstrated by reconstructing neutron and gamma-ray images.

189 0 obtained with the MAGIC (Major Atmospheric Gamma-ray Imaging Cherenkov) telescopes, revealing varia

190 nergy stereoscopic system, major atmospheric gamma-ray imaging Cherenkov, and very energetic radiatio

191 a and to account for the self-attenuation of gamma rays in high-TDS oil and gas fluids when they are

192 showed that an attenuation of 27%-35% of the gamma rays in the flat panel could be achieved by decrea

193 the bright diffuse emission of annihilation gamma-rays in the bulge region of our Galaxy.

194 then leads to highly directional emission of gamma-rays induced by the plasma magnetic field.

195 Using 440 keV gamma-rays instead of 79 keV x-rays in image reconstruct

196 etector signals and reconstructs the maximum gamma-ray intensity peak position, in full 3 dimensions.

197 Relative to controls and gamma-ray, intestinal tumor frequency and grade was sign

198 dated by the single-crystal structure of the gamma-ray irradiated material, and subsequently leads to

199 tron paramagnetic resonance (EPR) spectra of gamma-ray-irradiated newberyite from Synthesis 1 contain

200 tron paramagnetic resonance (EPR) spectra of gamma-ray-irradiated struvite disclose five [AsO3](2-) r

201 data of [Formula: see text]-H2AX yields for gamma ray irradiation.

202 Defect density characterization reveals that gamma-ray irradiation does not induce electronic trap st

203 y loss from the early degradation induced by gamma-ray irradiation.

204 Sensitive imaging of gamma rays is widely used; however, radioactive decay is

205 energy transfer (low-LET) radiation such as gamma-ray is highlighted by the studies in atom bomb sur

206 gy charged particles compared with X-rays or gamma-rays is determined largely by the spatial distribu

207 se as compared with low-LET IR (such as X or gamma rays) is due to inefficient NHEJ.

208 s power prompt, brief and intense flashes of gamma-rays known as gamma-ray bursts (GRBs), followed by

209 mma-ray bursts are intense flashes of cosmic gamma-rays, lasting less than about two seconds, whose o

210 The observed gamma-ray luminosity implies an upper limit of 60 millis

211 wer carried by accelerated particles and the gamma-ray luminosity, with AGN and GRBs lying at the low

212 my, we generated ethyl methanesulfonate- and gamma-ray-mutagenized populations of the C(4) species so

213 By contrast, optical and gamma-ray observations during the prompt phase have led

214 , approaching the size of the Galaxy itself, gamma-ray observations have revealed the so-called 'Ferm

215 Here we report on gamma-ray observations of the radio galaxy IC 310 obtain

216 ia HL60 cell clones radioresistant to either gamma-rays or alpha-particles to understand possible mec

217 in the radio-frequency spectrum relative to gamma-rays or X-rays suggests that radio searches may un

218 ated with conventional radiation (X-rays and gamma rays) or particle radiation (protons and carbon io

219 a paediatric head and neck case, the prompt gamma-ray origin can be determined from the width of the

220 the emerging fields of coherent and quantum gamma-ray photon optics, providing a basis for the reali

221 Here, we describe two separate gamma-ray (photon energy greater than 100 mega-electron

222 cs, providing a basis for the realization of gamma-ray-photon/nuclear-ensemble interfaces and quantum

223 oherent manipulation of interactions between gamma-ray photons and nuclear ensembles remains limited.

224 efficient method to control the waveforms of gamma-ray photons coherently.

225 rate the conversion of individual recoilless gamma-ray photons into a coherent, ultrashort pulse trai

226 spectrometer relies on the conversion of the gamma-ray photons into electron-positron pairs in a soli

227 is is generally done through observations of gamma-ray photons or cosmic rays.

228 thod is based on the resonant interaction of gamma-ray photons with an ensemble of nuclei with a reso

229 ng us to shape the waveforms of the incident gamma-ray photons.

230 used ionizing irradiation sources such as X/gamma-ray photons.

231 ust be measured; however, previous claims of gamma-ray polarization have been controversial.

232 theoretically show that the higher harmonic gamma-ray produced by nonlinear inverse Thomson scatteri

233 Subhaloes boost gamma-ray production from dark matter annihilation by fa

234 eration, thereby pinpointing the location of gamma-ray production.

235 Direct detection of gamma-ray pulsars enables studies of emission mechanisms

236 We report the detection of 16 gamma-ray pulsars in blind frequency searches using the

237 tars (NSs) are rotation-powered radio and/or gamma-ray pulsars.

238 spectral properties resemble those of young gamma-ray pulsars.

239 Strong gamma-ray pulsations were detected for eight MSPs.

240 The pulsar, discovered through its gamma-ray pulsations, has a period of 316.86 millisecond

241 ible to pinpoint neutron stars through their gamma-ray pulsations.

242 The gamma-ray pulse profiles and spectral properties resembl

243 sional PIC simulations show that a brilliant gamma-ray pulse with unprecedented power of 6.7 PW and p

244 otions and hence emitting brilliant vortical gamma-ray pulses in the quantum electrodynamic (QED) reg

245 imultaneous spectral energy distributions of gamma-ray quasars, we find a seed factor distribution wh

246 100 kiloelectronvolts, corresponding to soft gamma-ray radiation (the term used when the radiation is

247 Here, we present a new regime of betatron gamma-ray radiation generated by stimulating a large-amp

248 radiation from LWFA to be extended to bright gamma-ray radiation, which is beyond the capability of 3

249 ficant fraction of their kinetic energy into gamma-ray radiation.

250 ies and response toward ionizing neutron and gamma-ray radiation.

251 rradiation with high-energy electron-beam or gamma-ray radiations.

252 show that the energy fluxes in the X-ray and gamma-ray range and their photon indices remain comparab

253 During the third session, 29 soft-gamma-ray repeater (SGR) bursts were detected in gamma-r

254 fast radio burst in association with a soft gamma-ray repeater suggests that magnetar engines can pr

255 ale C57BL/6 mice to 0, 1.5, 3, 6 or 10 Gy of gamma rays, sacrificing groups of the mice at 1, 2, 3, 5

256 The response of those genes to gamma-rays seems to be unaffected by the myriad of genet

257 The weak gamma rays seen in EM170817 are dissimilar to classical

258 ent multiwavelength observations of a unique gamma-ray-selected transient detected by the Swift satel

259 d to be very promising candidates for X- and gamma-ray semiconductor detectors.

260 due to mixed fields of neutrons and photons (gamma-rays), shielding from buildings, and proximity to

261 No temporally coincident x- or gamma-ray signature was identified in association with t

262 are coincident with previously unidentified gamma-ray sources, and many are associated with supernov

263 the Large Area Telescope on board the Fermi Gamma-ray Space Telescope.

264 h the Large Area Telescope onboard the Fermi Gamma-ray Space Telescope.

265 The Gamma Ray Spectrometer on the Lunar Prospector orbiter p

266 The MESSENGER Gamma-Ray Spectrometer measured the average surface abun

267 Gamma-ray spectrometry and X-ray fluorescence analysis o

268 toring surveys (since April 2011) or in situ gamma-ray spectrometry of bare soil areas (since summer

269 nt in final formulation was quantified using gamma-ray spectrometry.

270 he doping concentrations were measured using gamma-ray spectroscopy and confirmed using SIMS analysis

271 ith the diagnosis ultimately being made with gamma-ray spectroscopy of a urine sample.

272 Urine analysis using gamma-ray spectroscopy on day 22 showed a characteristic

273 device noise and charge collection, enabling gamma-ray spectrum collection at room temperature.

274 The gamma-ray spectrum generated in collisions of the accele

275 The gamma-ray spectrum is well modeled with emission from pr

276 ion, homeland security, medical imaging, and gamma-ray telescopes.

277 It is based on the detection of the prompt gamma rays that are emitted naturally during the deliver

278 After the initial burst of gamma-rays that defines a gamma-ray burst (GRB), expandi

279 When irradiated with (60)Co gamma ray, the EPR spectra completely changed their patt

280 ngulfing the jet explains the low-luminosity gamma rays, the high-luminosity ultraviolet-optical-infr

281 n exposure of normal human cells to low-dose gamma rays, the TCTP protein level was greatly increased

282 width of the electromagnetic spectrum, from gamma rays to radio waves, and sound.

283 impaired resistance of mice irradiated with gamma-rays to bacterial translocation and subsequent sep

284 trophysics Laboratory) telescopes detected a gamma-ray transient, GRB 170817A.

285 population of radio, ultraviolet, X-ray and gamma-ray transients in the local Universe.

286 and quantum interference effects at nuclear gamma-ray transitions.

287 )Zr) nuclei are radioactive and emit intense gamma-rays upon decay, allowing sensitive detection of m

288 egrees in the altitude direction, imaging of gamma rays using organic scintillators, and imaging of m

289 review the status of indirect searches with gamma rays using two promising targets, the Inner Galaxy

290 would be an indispensable tool for exploring gamma-ray vortex science.

291 promising radiation process for realizing a gamma-ray vortex source based on currently available las

292 cattering of circularly polarized light is a gamma-ray vortex, which means that it possesses a helica

293 Our work implies that gamma-ray vortices should be produced in various situati

294 CTP, repair of chromosomal damage induced by gamma rays was compromised significantly.

295 e now routinely detected at gigaelectronvolt gamma-ray wavelengths, suggesting that relativistic part

296 The brevity of the flares implies that the gamma rays were emitted via synchrotron radiation from p

297 ce irradiated with or without 5 Gy [(137)Cs] gamma-rays were orally infected with 10(6) CFU/mouse E.

298 than the relative equivalent dose of low-LET gamma-rays, which has implications in therapeutic develo

299 GRBs typically emit most of their energy via gamma-rays with energies in the kiloelectronvolt-to-mega

300 It has been proposed that the observed gamma-ray, X-ray and radio emission is due to an ultra-r