ライフサイエンスコーパス: cosmic ray

1 the termination shock, generating anomalous cosmic rays.

2 kelvin under exposure to proxies of galactic cosmic rays.

3 doped ices through interaction with galactic cosmic rays.

4 electrons produced in the track of galactic cosmic rays.

5 s dramatically impacts the qubit response to cosmic rays.

6 providing insight on the origin of electron cosmic rays.

7 ed to relativistic electron acceleration and cosmic rays.

8 yman-alpha photons, solar wind, and galactic cosmic rays.

9 ic particles such as ultraviolet photons and cosmic rays.

10 ces upon interaction with simulated galactic cosmic rays.

11 through observations of gamma-ray photons or cosmic rays.

12 nding of the oncogenic potential of galactic cosmic rays.

13 using a ground-based analog for exposure to cosmic rays.

14 tes from diverse sources, including galactic cosmic rays(4), trapped-particle (Van Allen) belts(5) an

15 t they could be a notable source of galactic cosmic rays(7-9).

16 dies, including auroral activity on Jupiter, cosmic-ray acceleration in supernova remnants, colliding

17 ltogether in looking for isolated regions of cosmic-ray acceleration.

18 many predictions, the intensity of anomalous cosmic ray (ACR) helium did not peak at the shock, indic

19 of tens to hundreds of megaelectronvolts) is cosmic-ray albedo neutron decay (CRAND).

20 s are not the only source of pulsed heating; cosmic rays also can heat interstellar grains in a pulse

21 iving interstellar chemistry via ionization, cosmic rays also interact with the interstellar medium i

22 er began making detailed measurements of the cosmic ray and energetic particle radiation environment

23 bon monoxide ((14)CO), produced naturally by cosmic rays and almost exclusively removed by OH, is a t

24 on of high-energy (tera-electron volts, TeV) cosmic rays and diffusive propagation from supernova sou

25 nd-level neutron monitor design for studying cosmic rays and fluxes of solar energetic particles at t

26 tic cosmic ray ions and electrons, anomalous cosmic rays and low-energy ions.

27 rays', as well as to re-accelerate Galactic cosmic rays and low-energy particles from the inner Sola

28 ssess the damage caused to such materials by cosmic rays and neutrons, which pose a variety of hazard

29 clude that SN 1006 is an efficient source of cosmic rays and obtain an observational support for the

30 nsoon connection is dominated most likely by cosmic rays and oceanic circulation (both associated to

31 ative termination shock is that of anomalous cosmic rays and of interstellar pick-up ions.

32 orbed dose and dose equivalent from galactic cosmic rays and solar energetic particles on the martian

33 cts of meteorites and micrometeorites and of cosmic rays and solar-wind particles are major causes of

34 r qubits responded to essentially all of the cosmic rays and their secondary particles incident on th

35 mistry includes high-energy particles (e.g., cosmic rays) and high-energy photons (e.g., extreme-UV).

36 f interstellar clouds, the energy density of cosmic rays, and the formation of stars.

37 ns, to help determine the source of Galactic cosmic rays, and to date circumstellar grains.

38 Cosmic rays are charged particles arriving at the Earth

39 Cosmic rays are energetic charged particles from extrate

40 Cosmic rays are the highest-energy particles found in na

41 rse, demands a mechanism for ionization, and cosmic rays are the ideal candidate as they can operate

42 s shock is expected to accelerate 'anomalous cosmic rays', as well as to re-accelerate Galactic cosmi

43 at hundreds to thousands of eV and galactic cosmic rays at tens of TeV has wide-ranging implications

44 the prime candidates to produce the observed cosmic rays at the highest energies.

45 yager 2 did not find the source of anomalous cosmic rays at the shock, suggesting that the source is

46 The origin of high-energy cosmic rays, atomic nuclei that continuously impact Eart

47 mation, and could guide a wind of hot gas or cosmic rays away from the central region.

48 a were obtained by exploiting the negligible cosmic-ray background deep underground at the Laboratory

49 gh a variety of processes (such as solar and cosmic ray bombardment, micro-meteorite bombardment, and

50 meteorites, solar wind, energetic x-rays and cosmic ray bombardment.

51 Terrestrial nuclear reactions or cosmic-ray bombardment are not sufficient to generate su

52 from spallation reactions (in which Galactic cosmic rays break apart larger nuclei in the interstella

53 ter while simultaneously being shielded from cosmic rays by overlying ice.

54 istance does not greatly exceed the distance cosmic rays can diffuse over this time, 1 kiloparsec.

55 Cosmic rays caused correlated errors at a rate of [Formu

56 has raised the intriguing possibility that a cosmic ray-cloud interaction may help explain how a rela

57 a deposits that experienced less exposure to cosmic rays compared to the samples with ages of 4 Ma.

58 by cosmic rays for different grain sizes and cosmic ray components.

59 expectations, the extragalactic component of cosmic rays contributes substantially to the total flux

60 from environmental radioactive materials and cosmic rays contributes to this observed difference.

61 Here, we directly measured the cosmic-ray contribution to spatiotemporally correlated q

62 mechanisms have been proposed to explain how cosmic rays could affect clouds, but they need to be inv

63 Cosmic rays (CRs) play an important role in affecting pl

64 ent was a major contributor to the increased cosmic-ray density in the Galactic Centre, and is in tur

65 The Pierre Auger Observatory is the largest cosmic-ray detector on Earth, and as such is beginning t

66 ccomplished this by synchronously monitoring cosmic-ray detectors and qubit energy-relaxation dynamic

67 Interplanetary cosmic-ray dose equivalent rates in Orion were as much a

68 We report the spectra of galactic cosmic rays down to ~3 x 10(6) electron volts per nucleo

69 Herein, the formation of glyoxylic acid via cosmic-ray driven, non-equilibrium chemistry in polar in

70 This paper formulates the cosmic ray-driven electron-induced reaction as a univers

71 nyl alcohol (C2H3OH) act as key tracers of a cosmic-ray-driven nonequilibrium chemistry leading to co

72 l that was irradiated at low temperatures by cosmic rays during its interstellar journey, and experie

73 volts per nucleon and an increasing galactic cosmic-ray electron intensity down to ~10 x 10(6) electr

74 he puzzle of the origin of ultra high energy cosmic ray electrons.

75 Here we consider neutrino and cosmic-ray emission from multiple emission regions since

76 The presented (36)Cl Cosmic Ray Exposure ages demonstrate that the cliff over

77 We determined interstellar cosmic ray exposure ages of 40 large presolar silicon ca

78 Its pre-atmospheric orbit and cosmic-ray exposure age confirm that it arrived on Earth

79 The cosmic-ray exposure age of Ost 65 shows that it may be a

80 meteorites, this time scale is less than the cosmic-ray exposure age, which measures when they were e

81 xistence of associated dust bands(8-10), the cosmic-ray exposure ages of H-chondrite meteorites(11,12

82 Based on new and published cosmic-ray exposure chronologies, we show that glacier e

83 This interpretation relies mainly on cosmic-ray exposure dating of glacial deposits.

84 The cosmic ray flux is reduced symmetrically at all latitude

85 If such a high cosmic-ray flux is ubiquitous in diffuse clouds, the dis

86 Here, we calculate the heating by cosmic rays for different grain sizes and cosmic ray com

87 s linked with either ultraviolet or galactic cosmic ray (GCR) effects on atmospheric particles.

88 er risk is an important concern for galactic cosmic ray (GCR) exposures, which consist of a wide-ener

89 agnetic field causes an increase in galactic cosmic ray (GCR) flux.

90 The influence of solar forcing and Galactic Cosmic Rays (GCR) ionization on the global distribution

91 Galactic Cosmic Rays (GCRs) are charged particles, originating fr

92 methanol ices exposed to proxies of galactic cosmic rays (GCRs).

93 irradiation of organic materials by galactic cosmic rays (GCRs).

94 simplified five-ion, space-relevant galactic cosmic ray (GCRsim) radiation at 15 and 50 cGy, to simul

95 aelectron volt electrons, ACRs, and galactic cosmic rays have steadily increased since late 2004 as t

96 The small intensity gradient of Galactic cosmic ray helium indicates that either the gradient is

97 pectral energy distribution of the anomalous cosmic rays, however, indicates that Voyager 1 still has

98 he detection of supernova-produced (60)Fe in cosmic rays implies that the time required for accelerat

99 It provides an example to study the youth of cosmic rays in a superbubble environment before they mer

100 d by variations in the intensity of galactic cosmic rays in the atmosphere.

101 We find that ions from Galactic cosmic rays increase the nucleation rate by one to two o

102 August 2012, while those of galactic origin (cosmic rays) increased by 9.3% at the same time.

103 Noble gases produced by galactic cosmic rays, indicating a ~5 million year exposure, and

104 ced from natural (e.g. volcanic activity and cosmic ray-induced spallation) and anthropogenic process

105 offers an environment with an extremely low cosmic-ray-induced background(8).

106 Cosmic rays initiate air showers--cascades of secondary

107 l stems from an observed correlation between cosmic ray intensity and Earth's average cloud cover ove

108 hat for the processes studied, variations in cosmic ray intensity do not appreciably affect climate t

109 The cosmic ray intensity increased when B was relatively lar

110 liosheath or the local interstellar Galactic cosmic ray intensity is lower than expected.

111 However, cosmic rays interact with matter near their sources and

112 paper we review the observables generated by cosmic-ray interactions with the interstellar medium, fo

113 rs in the interstellar medium in response to cosmic ray ionization is summarized, and a review of the

114 drated electron (e(pre)(-)) flux produced by cosmic ray ionization on atmospheric particle surfaces,

115 From these, we find that the cosmic-ray ionization rate along this line of sight is 4

116 rge amounts of warm molecular gas(5), a high cosmic-ray ionization rate(6), unusual gas chemistry, en

117 ectrons (e-), the electron fraction, and the cosmic-ray ionization rate.

118 here was a simultaneous increase in Galactic cosmic ray ions and electrons, anomalous cosmic rays and

119 The origin of Galactic cosmic-ray ions has remained an enigma for almost a cent

120 The origin of Galactic cosmic rays is a century-long puzzle.

121 The origin of cosmic rays is a pivotal open issue of high-energy astro

122 Radio detection of cosmic rays is a rapidly developing technique for determ

123 y support the idea that the bulk of galactic cosmic rays is accelerated in such remnants by a Fermi m

124 nstructing the incident direction of primary cosmic rays is demonstrated and possible interdisciplina

125 We argue that the radial anisotropy of the cosmic rays is expected to be small in the foreshock reg

126 ing interactions with externally accelerated cosmic rays, Jupiter's magnetosphere powers this oxygen

127 thanol in cold molecular clouds via galactic cosmic rays-mediated nonequilibrium chemistries.

128 rock overburden of this facility reduces the cosmic ray muon flux by over 99% compared to laboratorie

129 To address this challenge, cosmic ray muons (CRMs) are used as an alternative NDE r

130 Cosmic ray muons have been considered as a non-conventio

131 To utilize cosmic ray muons in engineering applications, two import

132 ion associated with absorption of y-rays and cosmic-ray muons in the qubit substrate.

133 on and bulk material geometry in a realistic cosmic ray neutron field.

134 ned inside the heliosphere, the intensity of cosmic ray nuclei from outside the heliosphere abruptly

135 It is thought that Galactic cosmic-ray nuclei are gradually accelerated to high ener

136 The search for the origin(s) of Galactic cosmic-ray nuclei may be closing in on the long-suspecte

137 sequent enrichment of the gas by stellar and cosmic-ray nucleosynthesis.

138 hadron-like particle ("cygnet") indicated by cosmic ray observations on certain neutron stars is pred

139 Newly constructed ultrahigh-energy cosmic ray observatories together with high-energy gamma

140 anisotropy maps of ground-based high-energy cosmic-ray observatories (Milagro, Asgamma, and IceCube)

141 comes from accelerators capable of producing cosmic rays of these energies.

142 tes secondary electrons produced by galactic cosmic rays, one of few sources of energy that penetrate

143 nova remnants can power the observed flux of cosmic rays only if they transfer a significant fraction

144 tical difficulties associated with shielding cosmic rays, our results indicate the importance of radi

145 ut any external agents (e.g., superenergetic cosmic ray particles) or extraordinary in-cloud conditio

146 The Galaxy is filled with cosmic-ray particles, mostly protons with kinetic energi

147 The unexpectedly high flux of cosmic-ray positrons detected at Earth may originate fro

148 ns in cold molecular clouds through galactic cosmic rays processing at 5 K to sulfanes (H(2)S(n); n =

149 deflection by interstellar magnetic fields, cosmic rays produced within the Milky Way arrive at Eart

150 Cosmic-ray produced radionuclides, such as (10)Be and (1

151 Here we show that the cosmic ray-produced nuclides beryllium-10 and aluminum-2

152 To extend this timeline, cosmic ray-produced radionuclides like (14)C in tree-rin

153 Cosmic-ray-produced (3)He, (21)Ne, and (36)Ar yield conc

154 700 years ago), based on new measurements of cosmic-ray-produced beryllium and aluminium isotopes ((1

155 Local cosmic ray production is also enhanced, typically by a f

156 of stellar evolution, binary formation, and cosmic-ray production in the Galactic Centre.

157 tensive air showers induced from high-energy cosmic rays provide a window into understanding the most

158 oxide (CO(2)) ices upon exposure to galactic cosmic ray proxies in the form of energetic electrons.

159 ens downstream of the bend point, indicating cosmic-ray reacceleration.

160 For data pretreatment, we developed a unique cosmic ray removal method and used an automated baseline

161 ources, dark matter, or unknown processes of cosmic-ray secondary production.

162 this scenario, the shock energy channeled to cosmic rays should induce a higher post-shock density th

163 that synthetic torpor protects animals from cosmic ray-simulated radiation and the mechanism involve

164 re to a single-dose of a simplified galactic cosmic ray simulation (simGCRsim) only in males with fun

165 Cosmic ray sources are likely to involve the most energe

166 Stellar nucleosynthesis and cosmic ray spallation are ruled out as causes of the ano

167 o discussed and shown to be a consequence of cosmic ray spallation processes rather than primordial n

168 e large difference in nuclear recoil loss of cosmic ray spallation products (3)He and (21)Ne enabled

169 0Be) in excess of that expected from in situ cosmic ray spallation reactions is present in lunar surf

170 After consideration of cosmic-ray spallation and degassing processes, our resul

171 Raman spectra, including photoluminescence, cosmic rays, stray light, artefacts caused by spectromet

172 on that could inflict damage by accelerating cosmic rays that can deliver ionizing radiation for up t

173 50-parsec-wide cocoon of freshly accelerated cosmic rays that flood the cavities carved by the stella

174 ew stars and are the source of the energetic cosmic rays that irradiate us on the Earth.

175 In this process, cosmic rays that reach the upper atmosphere interact wit

176 Iron-60 ((60)Fe) is a radioactive isotope in cosmic rays that serves as a clock to infer an upper lim

177 ong candidates to be the Galactic factory of cosmic rays, their blast waves being powerful particle a

178 va remnants (SNRs) hint that they accelerate cosmic rays to energies close to ~10(15) electron volts.

179 e environments for efficient acceleration of cosmic rays to very high energies.

180 les us to determine the mass spectrum of the cosmic rays: we find a mixed composition, with a light-m

181 E particles (high charge and energy galactic cosmic rays were observed, yielding an overall average m

182 nets, astronauts will be exposed to galactic cosmic rays which are composed of heavy particles (such

183 Second, beryllium-7 is a product of cosmic rays which are themselves directly linked to sola

184 the most energetic particles ever observed, cosmic rays, will begin to be revealed in the next few y

185 uare centimetre for air showers initiated by cosmic rays with energies of 10(17)-10(17.5) electronvol

186 Measurements of the mass composition of cosmic rays with energies of 10(17)-10(18) electronvolts

187 g nucleosynthesis, interactions of energetic cosmic rays with interstellar matter, evolved low-mass s

188 side the sun, or produced in interactions of cosmic rays with the atmosphere, have allowed the first

189 i's classic result on the energy spectrum of cosmic rays, with the universal exponent -2, which is in