ライフサイエンスコーパス: interstellar medium

1 cosmic rays break apart larger nuclei in the interstellar medium).

2 s via pyridine to NPAH-type molecules in the interstellar medium.

3 traviolet) spectral signature of dust in the interstellar medium.

4 licates that are abundant in IDPs and in the interstellar medium.

5 ealing new insight into the chemistry of the interstellar medium.

6 st abundant nitrogen-bearing molecule in the interstellar medium.

7 lar dust (ISD) is the condensed phase of the interstellar medium.

8 ar objects and collides with the surrounding interstellar medium.

9 the physical and chemical conditions in the interstellar medium.

10 nlikely to survive in high abundances in the interstellar medium.

11 that the EUV flux cannot be an effect of the interstellar medium.

12 encounters to synthesize C3H radicals in the interstellar medium.

13 he complex molecular species observed in the interstellar medium.

14 distribution, and chemistry of anions in the interstellar medium.

15 onments, from the atmosphere of Titan to the interstellar medium.

16 ydrodynamic interaction of the wind with the interstellar medium.

17 uter heliosphere, to about 0.1 cm(-3) in the interstellar medium.

18 rature ices relevant to the solar system and interstellar medium.

19 between the solar plasma and the much cooler interstellar medium.

20 s by twisting of field lines frozen into the interstellar medium.

21 ow-density environments of the Earth and the interstellar medium.

22 liosheath depletion region), rather than the interstellar medium.

23 -3), very close to the value expected in the interstellar medium.

24 e the synthesis of the very first PAH in the interstellar medium.

25 iated formation of aromatic molecules in the interstellar medium.

26 cently detected in the denser regions of the interstellar medium.

27 a new model of the formation of H(2) in the interstellar medium.

28 It governs the chemistry and physics of the interstellar medium.

29 enized, likely by repeated processing in the interstellar medium.

30 ture and the direction of motion through the interstellar medium.

31 gnetic field strength and orientation in the interstellar medium.

32 and forms a bubble of solar material in the interstellar medium.

33 gitude straddling the direction of the local interstellar medium.

34 rowth and carbonaceous dust evolution in the interstellar medium.

35 undly affects the growth of molecules in the interstellar medium.

36 monolayers in cold and dense regions of the interstellar medium.

37 n lengths than those observed in the diffuse interstellar medium.

38 formation of carbon-bearing molecules in the interstellar medium.

39 celerates to begin its merger into the local interstellar medium.

40 n of these isomers in the laboratory and the interstellar medium.

41 2.3 x 10(-5) is consistent with that in the interstellar medium (after allowing for Galactic chemica

42 iamonds due to grain-grain collisions in the interstellar medium although a low-pressure mechanism of

43 d most easily studied sample of the Galactic interstellar medium, an understanding of which is essent

44 ction dominates at energies relevant for the interstellar medium and alone may explain observations i

45 mportance to form PAH-like structures in the interstellar medium and also in hydrocarbon-rich, low-te

46 t bare carbon molecule, is ubiquitous in the interstellar medium and in combustion flames.

47 cies under low-temperature conditions in the interstellar medium and in hydrocarbon-rich atmospheres

48 f cyano-substituted naphthalene cores in the interstellar medium and in planetary atmospheres.

49 nt roles in extreme environments such as the interstellar medium and planetary atmospheres (CN, SiN a

50 ionizing environments such as regions of the interstellar medium and solar nebulae.

51 where the Sun was born was isolated from the interstellar medium and the birth of the Sun.

52 atter in meteorites might have formed in the interstellar medium and/or the solar nebula, but was alm

53 ned in conditions approximating those of the interstellar medium, and measured over the entire spectr

54 oduce heavy elements, inject energy into the interstellar medium, and possibly regulate the star form

55 that the models of nitrogen chemistry in the interstellar medium are incomplete.

56 are the best analogues to investigating the interstellar medium at a quasi-primitive environment in

57 generally thought to have originated in the interstellar medium, but it might have formed in the sol

58 agrees with the present value for the local interstellar medium, but seems to be incompatible with t

59 ecules in the astrochemical evolution of the interstellar medium, but the formation mechanism of even

60 y role in the astrochemical evolution of the interstellar medium, but the formation mechanism of even

61 es a change in the average properties of the interstellar medium, but the measurements are systematic

62 es of dust grains that are recycled into the interstellar medium by stars.

63 n accelerated by fast shocks driven into the interstellar medium by the expanding radio jets.

64 tents, and their ratio, are examined for the interstellar medium, comets, chondritic meteorites, and

65 otter than the 1,000,000 to 2,000,000 kelvin interstellar medium component in the Milky Way Galaxy.

66 The Sun moves through the local interstellar medium, continuously emitting ionized, supe

67 the Sun through the dynamically active local interstellar medium creates an evolving heliosphere envi

68 Previous attempts to measure the interstellar medium directly in normal galaxies at these

69 We conclude that the interstellar medium field is turbulent or has a distorti

70 tilted approximately 20-30 degrees from the interstellar medium flow direction (resulting from the p

71 Neutral gas of the local interstellar medium flows through the inner solar system

72 enerated by cosmic-ray interactions with the interstellar medium, focusing primarily on the relevance

73 approximately 10(3) times that of the local interstellar medium (for example, owing to an O or B sta

74 and thereby prevents the metallicity of the interstellar medium from increasing steadily with time.

75 Molecular gas is the phase of the interstellar medium from which stars form, so these outf

76 e variation of about 0.06 to 0.3 seen in the interstellar medium from which the stars form.

77 However, the interstellar medium has been found to be markedly inhomo

78 ellar feedback (the momentum return into the interstellar medium) has been considered incapable of ra

79 which may themselves be very abundant in the interstellar medium, has led to the suggestion that ioni

80 udy interplanetary dust, Venus' tail and the interstellar medium.) Here we report the serendipitous d

81 ay, and the absorption of soft X-rays in the interstellar medium hinders the determination of the cau

82 l properties and elemental abundances of the interstellar medium in galaxies during cosmic reionizati

83 Depending on the character of the interstellar medium in our galaxy, this emission could b

84 The chemistry that occurs in the interstellar medium in response to cosmic ray ionization

85 a strong evolution in the properties of the interstellar medium in the early Universe.

86 masses of highly excited, chemically evolved interstellar medium in this galaxy, which constitutes at

87 nization, cosmic rays also interact with the interstellar medium in ways that heat the ambient gas, p

88 We find that the field strength in the local interstellar medium is 3.7-5.5 microG.

89 The interstellar medium is characterized by a rich and diver

90 Gas-phase chemistry in the interstellar medium is driven by fast ion-molecule react

91 The interstellar medium is enriched primarily by matter ejec

92 Understanding their origin in the interstellar medium is one of the oldest problems in ast

93 logical constant) in which the inhomogeneous interstellar medium is resolved.

94 lative motion of the Sun with respect to the interstellar medium is slower and in a somewhat differen

95 redshifts of two to three, by which time the interstellar medium is sufficiently enriched with metals

96 c hydrocarbons (PAHs) are omnipresent in the interstellar medium (ISM) and also in carbonaceous meteo

97 y role in the astrochemical evolution of the interstellar medium (ISM) and in the chemistry of combus

98 largest noncyclic molecules detected in the interstellar medium (ISM) are organic with a straight-ch

99 large fraction of their original mass to the interstellar medium (ISM) through a processed, dusty, mo

100 arbons in ionizing environments, such as the interstellar medium (ISM), and some combustion condition

101 In the interstellar medium, it has been thought to be mostly mo

102 g our Galaxy is a crucial constituent of the interstellar medium: it mediates the dynamics of interst

103 As the Sun moves through the local interstellar medium, its supersonic, ionized solar wind

104 of the heliosphere indicates that the local interstellar medium (LISM) magnetic field (B(LISM)) is t

105 ikely centered on the direction of the local interstellar medium (LISM) magnetic field.

106 e solar wind termination shock and the local interstellar medium (LISM).

107 the extended solar atmosphere and the local interstellar medium (LISM).

108 gnetic bubble, the heliosphere, in the local interstellar medium (mostly neutral gas) flowing by the

109 strength and orientation of the field in the interstellar medium near the heliosphere has been poorly

110 ecules (rather than from dust grains) in the interstellar medium, no consensus has been reached regar

111 ich the AGN drives an outflow, expelling the interstellar medium of its host and transforming the gal

112 Measurements of the D/H ratio in the interstellar medium of our Galaxy place a strict lower l

113 hot ionized intracluster medium and the cold interstellar medium of spiral galaxies.

114 irs that extend well beyond the star-forming interstellar medium of these galaxies.

115 ost scenarios advocate cold synthesis in the interstellar medium or in the outer solar system.

116 eorites are interpreted as a heritage of the interstellar medium or resulting from ion-molecule react

117 ) release huge quantities of energy into the interstellar medium, potentially clearing the surroundin

118 ational transitions, so its abundance in the interstellar medium remains poorly known.

119 ombination with our current knowledge of the interstellar medium revealed that the EUV flux cannot be

120 tars do not produce enough 3He to enrich the interstellar medium significantly.

121 mark of gas-phase chemical processing in the interstellar medium, suggesting that interstellar gases

122 been formed from material inherited from the interstellar medium that suffered little processing in t

123 cular species that have been detected in the interstellar medium, the singlet carbene cyclopropenylid

124 ingle-collision conditions as present in the interstellar medium, this core loses a hydrogen atom to

125 supersonic (with respect to the surrounding interstellar medium) to being subsonic.

126 ds, H3+ has now been observed in the diffuse interstellar medium toward Cygnus OB2 No. 12.

127 ecies have been definitively detected in the interstellar medium via their rotational, infrared, and/

128 The presence of H3+ in the interstellar medium was first suggested in 1961, and its

129 butadiyne (MeC5N), a molecule present in the interstellar medium, was established in order to circumv

130 c C(6) ring in hydrocarbon flames and in the interstellar medium where concentrations of dicarbon tra

131 inated by heated solar plasma, and the local interstellar medium, which is expected to contain cold n

132 s provide the basis for studies of C3 in the interstellar medium with far-infrared astronomy.

133 and therefore how fast they will enrich the interstellar medium with fresh material.

134 ronomy, primarily because the opacity of the interstellar medium would prevent observations at these