ライフサイエンスコーパス: cosmic ray

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

2 nding of the oncogenic potential of galactic cosmic rays.

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

4 the termination shock, generating anomalous cosmic rays.

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

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

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

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

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

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

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

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

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

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

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

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

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

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

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

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

21 Cosmic rays are charged particles arriving at the Earth

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

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

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

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

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

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

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

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

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

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

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

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

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

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

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

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

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

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

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

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

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

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

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

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

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

47 The cosmic ray flux is reduced symmetrically at all latitude

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

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

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

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

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

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

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

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

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

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

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

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

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

61 Cosmic rays initiate air showers--cascades of secondary

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

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

64 The cosmic ray intensity increased when B was relatively lar

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

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

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

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

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

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

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

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

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

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

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

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

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

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

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

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

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

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

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

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

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

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

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

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

89 700 years ago), based on new measurements of cosmic-ray-produced beryllium and aluminium isotopes ((1

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

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

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

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

94 Cosmic ray sources are likely to involve the most energe

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

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

97 0Be) in excess of that expected from in situ cosmic ray spallation reactions is present in lunar surf

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

99 50-parsec-wide cocoon of freshly accelerated cosmic rays that flood the cavities carved by the stella

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

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

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

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

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

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

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

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

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

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

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

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

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