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

3 ormal human cells following irradiation with gamma-rays.

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

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

6 ink lesion in HeLa-S3 cells upon exposure to gamma-rays.

7 cells subsequently exposed to 2 Gy doses of gamma-rays.

8 nner in human Hela-S3 cells upon exposure to gamma-rays.

9 orylated p53 and p21 after exposing cells to gamma-rays.

10 common origin for the optical light and the gamma-rays.

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

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

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

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

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

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

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

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

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

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

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

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

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

24 ive than wild-type cells to irradiation with gamma rays and UV light and to treatment with hydrogen p

25 ray observatories together with high-energy gamma-ray and neutrino observatories are well positioned

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

27 1m)Cd perturbed angular correlation (PAC) of gamma-rays and (113)Cd NMR spectroscopy.

28 Doses as low as 2-mGy gamma-rays and 0.29-mGy alpha-particles were sufficient

29 fect saturates at very low doses (50 mGy for gamma-rays and 25 mGy for alpha-particles).

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

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

32 Exposure of isolated DNA to X/gamma-rays and Fenton reagents was shown to lead to the

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

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

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

36 cially after low LET radiation such as X- or gamma-rays and whether the same signal transmission path

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

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

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

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

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

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

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

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

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

46 a cells exposed to continuous irradiation by gamma-rays at various dose rates.

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

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

49 08A, four minutes after its discovery in the gamma-ray band, decreasing to P = 16(+5)(-4) per cent ov

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

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

52 Gamma-ray binaries are stellar systems containing a neut

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

54 1FGL J1018.6-5856 is thus a gamma-ray binary, and its detection suggests the presenc

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

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

57 We report the optical polarization of a gamma-ray burst (GRB) afterglow, obtained 203 seconds af

58 Gamma-ray burst (GRB) afterglows have provided important

59 tical first few minutes after the onset of a gamma-ray burst (GRB) defines two broad classes: prompt

60 at arrives with the gamma-rays from a cosmic gamma-ray burst (GRB) is a signature of the engine power

61 The explosion that results in a cosmic gamma-ray burst (GRB) is thought to produce emission fro

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

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

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

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

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

67 8 galaxies that, together with reports of a gamma-ray burst at z approximately 8.2, constitute the e

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

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

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

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

72 The gamma-ray burst sources may provide a way to reach even

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 ativistic explosion known as a long-duration gamma-ray burst.

78 to be a short-duration, hard-spectrum cosmic gamma-ray burst.

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

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

81 Gamma-ray bursts (GRBs) and their afterglows are the mos

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

83 Despite a rich phenomenology, gamma-ray bursts (GRBs) are divided into two classes bas

84 Gamma-ray bursts (GRBs) are known to come in two duratio

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

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

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

88 Gamma-ray bursts (GRBs) fall into two classes: short-har

89 e past decade, our physical understanding of gamma-ray bursts (GRBs) has progressed rapidly, thanks t

90 Two short (< 2 s) gamma-ray bursts (GRBs) have recently been localized and

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

92 Long-duration gamma-ray bursts (GRBs) release copious amounts of energ

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

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

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

96 Over the past decade, long-duration gamma-ray bursts (GRBs)--including the subclass of X-ray

97 One would then expect that these long gamma-ray bursts and core-collapse supernovae should be

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

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

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

101 her these results suggest that long-duration gamma-ray bursts are associated with the most extremely

102 We find that the gamma-ray bursts are far more concentrated in the very b

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

104 Our results directly imply that long gamma-ray bursts are relatively rare in galaxies such as

105 Furthermore, the host galaxies of the long gamma-ray bursts are significantly fainter and more irre

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

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

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

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

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

111 s, associations of supernovae with long-soft gamma-ray bursts, and asymmetries in late-time emission-

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

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

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

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

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

117 ons for the production of the short class of gamma-ray bursts, which recent observations suggest may

118 g X-ray and radio sources and most recently, gamma-ray bursts.

119 afterglow model that is usually invoked for gamma-ray bursts.

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

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

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

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

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

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

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

127 Gamma rays can probe their spreading through the ambient

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

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

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

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

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

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

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

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

136 sure to low (10-cGy X-ray) versus high (5-Gy gamma-ray) doses of radiation.

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

138 A subsecond intense 'spike' of gamma-rays during a giant flare from the Galactic soft g

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

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

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

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

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

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

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

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

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

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

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

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

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

152 continuing for hundreds of seconds after the gamma-ray emission has ended.

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

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

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

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

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

158 ompt optical emission correlated with prompt gamma-ray emission, and early optical afterglow emission

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

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

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

162 cal afterglow emission uncorrelated with the gamma-ray emission.

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

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

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

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

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

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

169 of radiation from optical frequencies to TeV gamma-ray energies, as well as a delayed outburst at rad

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

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

172 peroxide), ionizing radiations (neutron and gamma-ray exposures), and other DNA-damaging agents (ult

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

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

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

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

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

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

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

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

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

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

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

184 rompt optical emission that arrives with the gamma-rays from a cosmic gamma-ray burst (GRB) is a sign

185 ained 203 seconds after the initial burst of gamma-rays from GRB 060418, using a ring polarimeter on

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

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

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

189 is able to reconstruct a genome shattered by gamma rays has now been revealed.

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

191 0 obtained with the MAGIC (Major Atmospheric Gamma-ray Imaging Cherenkov) telescopes, revealing varia

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

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

194 t is variable and correlated with the prompt gamma-rays, indicating a common origin for the optical l

195 Drosophila embryos are highly sensitive to gamma-ray-induced apoptosis at early but not later, more

196 spontaneous recombination and the repair of gamma-ray-induced double-strand breaks.

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

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

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

200 lysate microarrays from an isogenic pair of gamma-ray-irradiated cell lysates from HCT116 (p53(+/+)

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

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

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

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

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

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

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

208 searches, the Large Hadron Collider, and the Gamma-ray Large Area Space Telescope offer promising opp

209 stone on the path to produce an annihilation gamma-ray laser.

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

211 gy transfer (LET) alpha-particles or low-LET gamma-rays leads to stimulation of intercellular inducti

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

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

214 e to be compatible with existing neutron and gamma-ray measurements.

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

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

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

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

219 d Cys), and methionine after oxidation using gamma-rays or synchrotron X-rays and have compared these

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

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

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

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

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

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

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

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

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

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

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

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

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

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

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

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

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

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

241 The gamma-ray pulse profiles and spectral properties resembl

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

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

244 100 kiloelectronvolts, corresponding to soft gamma-ray radiation (the term used when the radiation is

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

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

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

248 X-rays, gamma rays, radiofrequency signals, and ultrasound waves

249 PSMA-targeted small molecule and demonstrate gamma-ray radioscintigraphic imaging of living human pro

250 during a giant flare from the Galactic soft gamma-ray repeater, SGR 1806-20, reopened an old debate

251 Soft gamma-ray repeaters (SGRs) are 'magnetars', a small clas

252 Soft-gamma-ray repeaters (SGRs) are galactic X-ray stars that

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

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

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

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

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

258 We speculate that most unidentified Galactic gamma-ray sources associated with star-forming regions a

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

260 The Fermi Gamma-Ray Space Telescope has unveiled a radio quiet pul

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

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

263 Long bursts, which on average have softer gamma-ray spectra, are known to be associated with stell

264 The Gamma Ray Spectrometer on the Lunar Prospector orbiter p

265 e concentrations of hydrogen detected by the Gamma Ray Spectrometer suite of instruments on the Mars

266 ootprint (several hundred kilometres) of the Gamma Ray Spectrometer suite, preventing the observation

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

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

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

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

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

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

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

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

281 ine and a few tripeptides were irradiated by gamma-rays, the products were analyzed by electrospray m

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 rse spectrum of induced DNA damage including gamma-rays, ultraviolet (UV)-C radiation, and methyl met

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

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

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

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

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

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

294 of atomic-mass difference, Delta(m), and of gamma-ray wavelengths to determine E, the nuclear bindin

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

296 isolated neutron stars observed at X-ray and gamma-ray wavelengths.

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

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

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

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