ライフサイエンスコーパス: interstellar

1 , we report on the detection of a continuous interstellar (60)Fe influx on Earth over the past ~33,00

2 The interstellar (60)Fe was extracted from five deep-sea sed

3 toms indicates a continued but low influx of interstellar (60)Fe.

4 Here we report observations of interstellar (7)Li in the low-metallicity gas of the Sma

5 he residual flux in saturated low-ionization interstellar absorption lines for identifying such leaky

6 ional, and astrochemical modeling study that interstellar aldehydes and enols like acetaldehyde (CH3C

7 reactions of molecular anions with abundant interstellar and atmospheric atomic species are largely

8 With nearly 200 molecules detected in interstellar and circumstellar environments, the identif

9 ino and diamino acid structures in simulated interstellar and circumstellar ice environments.

10 n several solar system bodies, as well as in interstellar and circumstellar ice mantles.

11 as well as new spectroscopic observations of interstellar and circumstellar regions are topics presen

12 derstanding their behavior and reactivity in interstellar and combustion environments.

13 tand the products formation from reactors to interstellar atmospheres as well as the growth mechanism

14 of the local interstellar velocity, based on interstellar atom measurements with IBEX, are consistent

15 structure suggests the importance of ionized interstellar atoms ('pickup protons') at the shock.

16 ission during 2009-2010 suggest that neutral interstellar atoms flow into the solar system from a dif

17 The diffuse interstellar bands (DIBs) are absorption lines observed

18 plicated as possible carriers of the diffuse interstellar bands in astronomy, indicating their persis

19 Here we report 13 diffuse interstellar bands in the 1.5-1.8 micrometre interval on

20 rption features collectively called 'diffuse interstellar bands' (DIBs).

21 made to identify the carriers of the diffuse interstellar bands, however, with little success.

22 nating feature in the energetic neutral atom Interstellar Boundary Explorer (IBEX) all-sky maps at lo

23 The Interstellar Boundary Explorer (IBEX) has obtained all-s

24 Observations with the Interstellar Boundary Explorer (IBEX) have shown enhance

25 The dominant feature in Interstellar Boundary Explorer (IBEX) sky maps of helios

26 The recently launched Interstellar Boundary Explorer (IBEX) spacecraft has com

27 Recent observations from the Interstellar Boundary Explorer (IBEX) spacecraft show th

28 some cases, similar to those observed by the Interstellar Boundary Explorer (IBEX) spacecraft, but th

29 Recent results obtained by NASA's Interstellar Boundary Explorer mission during 2009-2010

30 of Life ultimately changes our hypothesis on interstellar carbon chemistry.

31 mation about the potential of the associated interstellar chemistry for seeding newly formed planets

32 Aside from driving interstellar chemistry via ionization, cosmic rays also

33 andidate for observations in atmospheric and interstellar chemistry.

34 l data in order to gain further insight into interstellar chemistry.

35 The age of dense interstellar cloud cores, where stars and planets form,

36 ests that the field orientation in the Local Interstellar Cloud differs from that of a larger-scale i

37 ed in the tenuous and cold environment of an interstellar cloud illuminated by strong ultraviolet (UV

38 mediate interstellar neighborhood, the local interstellar cloud.

39 processes through which anions might form in interstellar clouds and circumstellar envelopes, includi

40 ce processing thought to be present in dense interstellar clouds and circumstellar regions, making a

41 Much of this chemistry occurs in "dense" interstellar clouds and protostellar disks surrounding f

42 Many chemical models of dense interstellar clouds predict that the majority of gas-pha

43 tanding the abundances of molecules in dense interstellar clouds requires knowledge of the rates of g

44 nce in different regions of space, from cold interstellar clouds to warm photon-dominated regions.

45 rbon monoxide (CO) is the primary tracer for interstellar clouds where stars form, but it has never b

46 cle, we review the observations of anions in interstellar clouds, circumstellar envelopes, Titan, and

47 rstellar medium: it mediates the dynamics of interstellar clouds, the energy density of cosmic rays,

48 mportant in the evolution of low-temperature interstellar clouds, where the quantum tunnelling effect

49 density during Earth's passage through local interstellar clouds, which could be expected if the loca

50 oincides with passage of our SS through such interstellar clouds, which have a significantly larger p

51 ghout the majority of both diffuse and dense interstellar clouds.

52 process for the physics and the chemistry of interstellar clouds.

53 t and which occurs both in diffuse and dense interstellar clouds.

54 he boundary layers between diffuse and dense interstellar clouds.

55 cal mol(-1), is an important source of HF in interstellar clouds; however, the dynamics of this quant

56 The chirality inherent within actual interstellar (cometary) ice environments will be conside

57 oming from the heating and/or irradiation of interstellar/cometary ice analogues (VAHIIA system) thro

58 sophistication have demonstrated that known interstellar COMs as well as the prebiotically interesti

59 We determined interstellar cosmic ray exposure ages of 40 large presol

60 We report an interstellar detection of a branched alkyl molecule, iso

61 lity of transfer of biological material over interstellar distances, as in panspermia scenarios.

62 Interstellar dust (ISD) is the condensed phase of the in

63 ructed spatial distribution of extinction by interstellar dust along the Galactic plane.

64 ations are similar to the value inferred for interstellar dust and support the idea that such grains

65 The interstellar dust candidates are readily distinguished f

66 and asteroid impact sites, the formation of interstellar dust clouds, ballistic penetrators, spacecr

67 eutic agents, and have even been observed in interstellar dust clouds.

68 Seven particles captured by the Stardust Interstellar Dust Collector and returned to Earth for la

69 continuum emission indicates a deficiency of interstellar dust in the galaxy.

70 diverge from any one representative model of interstellar dust inferred from astronomical observation

71 the chemistry that occurs on the surfaces of interstellar dust particles profoundly affects the growt

72 ins the nitrogen anomalies in meteorites and interstellar dust particles, as nitrogen fractionation i

73 pic anomalies are observed in meteorites and interstellar dust particles.

74 Interstellar dust plays a crucial role in the evolution

75 onsistent with an origin in the contemporary interstellar dust stream.

76 mation, the first step in the process is for interstellar dust to coagulate within a protoplanetary d

77 optical wavelengths because of absorption by interstellar dust, and distances are very large and hard

78 ive hydrocarbon chemistry in low-temperature interstellar environments, such as that of the Taurus Mo

79 cules by OH is widespread in low-temperature interstellar environments.

80 in chemical vapor deposition techniques and interstellar environments.

81 associated with a wide variety of different interstellar environments.

82 liopause to show that the plane of the local interstellar field is approximately 60 degrees to 90 deg

83 servations, indicates that the trend for the interstellar flow ecliptic longitude to increase linearl

84 further out in the heliosheath or the local interstellar Galactic cosmic ray intensity is lower than

85 energies is the hydrogen, helium, and oxygen interstellar gas flow.

86 The field associated with ionized interstellar gas has been determined through observation

87 average value of B = 6 microG in the neutral interstellar gas of our Galaxy.

88 The interstellar gas, mainly consisting of hydrogen molecule

89 ins that are much larger than predictions of interstellar grain models, and many of these are high-te

90 Synthesized on interstellar grains and eventually incorporated into the

91 of pulsed heating; cosmic rays also can heat interstellar grains in a pulsed manner.

92 Interstellar grains of typical size approximately 0.1 mi

93 We determine the mass distribution of 36 interstellar grains, their elemental composition, and a

94 s, and refractory organic material with some interstellar heritage.

95 nger link to be made between observations of interstellar HF and the abundance of the most common int

96 It is, however, the only source of interstellar HF, which has been detected in a wide range

97 Clues that connect this interstellar hot core chemistry to the solar system can

98 prebiotic molecules, including ribose, in an interstellar ice analog experiment.

99 om UV-photoprocessing followed by warm-up of interstellar ice analogs, are a hydrocarbon material ric

100 teorites, interplanetary dust particles, and interstellar ice analogs, gaining significant insight in

101 he formation of amino acid structures within interstellar ice analogues as a means towards furthering

102 ormation of H(2) from H atoms might occur in interstellar ice grains.

103 Radicals form readily when interstellar ices (composed of water and other volatiles

104 lar system's formation was typical, abundant interstellar ices are available to all nascent planetary

105 ex organics even deep within low-temperature interstellar ices at 10 K.

106 lyoxylic acid, an organic molecule formed in interstellar ices before subliming in star-forming regio

107 ass forming complex organic molecules inside interstellar ices before their sublimation in star-formi

108 Evolved interstellar ices observed in dense protostellar molecul

109 y driven, non-equilibrium chemistry in polar interstellar ices of carbon monoxide (CO) and water (H(2

110 nitrogen such as NH(3) should be present on interstellar ices, promoting the eventual formation of n

111 urces of radical production and chemistry in interstellar ices: electrons, ions, and X-rays.

112 has completed its first all-sky maps of the interstellar interaction at the edge of the heliosphere

113 y have important implications for the global interstellar interaction.

114 A majority of the grains have interstellar lifetimes of <300 Ma, which is shorter than

115 Establishing a consistent local interstellar magnetic field direction using IBEX ENAs at

116 to correct for possible systematic errors in interstellar magnetic field estimates, this result offer

117 r theories, that may be ordered by the local interstellar magnetic field interacting with the heliosp

118 The orientation of the local interstellar magnetic field introduces asymmetries in th

119 ar Cloud differs from that of a larger-scale interstellar magnetic field thought to parallel the gala

120 ould indicate an asymmetric pressure from an interstellar magnetic field, from transient-induced shoc

121 pressure is comparable to that of the local interstellar magnetic field.

122 degrees, appears to be ordered by the local interstellar magnetic field.

123 al samples, such as cometary, asteroidal, or interstellar material from sample return missions or inc

124 wed through a sufficient quantity of diffuse interstellar material reveals a number of absorption fea

125 This motion drives a wind of interstellar material through the heliosphere that has b

126 this could represent the delivery of exotic interstellar material to the inner solar system via impa

127 , interactions of energetic cosmic rays with interstellar matter, evolved low-mass stars, novae, and

128 s consistent with mixing of solar system and interstellar matter.

129 In this review, gas-phase chemistry of interstellar media and some planetary atmospheres is ext

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

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

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

133 ssure conditions, but their existence in the interstellar medium (ISM) remains unknown.

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

135 ttribute this to the high Mach number in the interstellar medium (ISM), although the exact details of

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

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

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

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

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

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

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

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

144 The solar system (SS) moves through the interstellar medium and collects these nucleosynthesis p

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

146 tually to carbonaceous nanostructures in the interstellar medium and in combustion systems.

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

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

149 In the interstellar medium and molecular clouds, compressible t

150 the bulk of their cosmogenic nuclides in the interstellar medium and not by exposure to an enhanced p

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

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

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

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

155 diative energy input and the dynamics of the interstellar medium around massive stars.

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

157 sition of mass, momentum and energy into the interstellar medium by massive stars ('feedback') are th

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

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

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

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

162 rticle density compared to the local average interstellar medium embedding our SS for the past few mi

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

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

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

166 s indiscernible from Faraday rotation in the interstellar medium for typical GHz observations frequen

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

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

169 150 years, the prevailing view of the local interstellar medium has been based on a peculiarity know

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

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

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

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

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

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

176 The interstellar medium is characterized by a rich and diver

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

178 The interstellar medium is enriched primarily by matter ejec

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

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

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

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

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

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

185 cted if they had propagated only through the interstellar medium of the Milky Way-indicate extragalac

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

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

188 nated in a very cold environment such as the interstellar medium or outer region of the solar nebula,

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

190 erved the icy grains originally found in the interstellar medium prior to solar system formation.

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

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

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

194 estimate that the irradiated objects in the interstellar medium were up to 30 times larger than the

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

196 actants, this reaction is viable in the cold interstellar medium where several methyl-substituted mol

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

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

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

200 produces cloud and intercloud phases in the interstellar medium, and disrupts molecular clouds (the

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

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

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

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

205 e molecules, H(2)S, are both detected in the interstellar medium, but the returned SH(X)/H(2)S abunda

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

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

208 r second(7), must 'sweep up' the surrounding interstellar medium, creating cavities in space around t

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

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

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

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

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

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

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

216 -bearing dust particles still permeating the interstellar medium.

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

218 ydrodynamic interaction of the wind with the interstellar medium.

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

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

221 organic matter, probably originating in the interstellar medium.

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

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

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

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

226 ields than in stellar ejectae or the diffuse interstellar medium.

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

228 ntributing to deuterium fractionation in the interstellar medium.

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

230 iated formation of aromatic molecules in the interstellar medium.

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

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

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

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

235 gnetic field strength and orientation in the interstellar medium.

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

237 gitude straddling the direction of the local interstellar medium.

238 rowth and carbonaceous dust evolution in the interstellar medium.

239 tion of sulfur between solids and gas of the interstellar medium.

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

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

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

243 xyl radicals (OH) play a central role in the interstellar medium.

244 nally excited OH(X) radicals observed in the interstellar medium.

245 er mille, close to compositions in the local interstellar medium.

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

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

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

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

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

251 lyzed grains were parts of aggregates in the interstellar medium: The large difference in nuclear rec

252 ced formation of glycerol in low-temperature interstellar model ices is facile.

253 anes, formed by exposure of methanol-based - interstellar model ices to ionizing radiation in the for

254 surements with IBEX, are consistent with the interstellar modulation of high-energy (tera-electron vo

255 ometric observations of high-mass regions in interstellar molecular clouds have revealed hot molecula

256 lex organosulfur molecules are ubiquitous in interstellar molecular clouds, but their fundamental for

257 llar HF and the abundance of the most common interstellar molecule, H2, and hence a more accurate est

258 It is the most abundantly produced interstellar molecule, next only to H(2), although its s

259 Aldehydes are widespread and abundant interstellar molecules; that they came to be present, su

260 m is passed by ISD grains from our immediate interstellar neighborhood, the local interstellar cloud.

261 by charge exchange of suprathermal ions with interstellar neutral atoms.

262 ational inferences or modelling in which the interstellar neutral hydrogen was not taken into account

263 We show that the amount of interstellar nitrogen present as N(2) depends on the com

264 not represent the main reservoir species for interstellar nitrogen.

265 orelevant molecules as planets form in their interstellar nurseries.

266 The high predicted number density of icy interstellar objects (2.4 x 10(-4) per cubic astronomica

267 re likely to result in the detection of more interstellar objects in the coming years.

268 previous estimates of the number density of interstellar objects, based on the assumption that all s

269 n recent years, evidence from laboratory and interstellar observations has emerged to suggest a 'top-

270 Recent interstellar observations have shown a strong correlatio

271 rimental evidence that it can be produced in interstellar or cometary environments.

272 some of the meteoritic keto acids points to interstellar or presolar origins, indicating that such c

273 not seem to reflect any large changes in the interstellar particle density during Earth's passage thr

274 The seven candidate interstellar particles are diverse in elemental composit

275 in some particles indicates that individual interstellar particles diverge from any one representati

276 h plasma, which is of solar origin, from the interstellar plasma, which is of local Galactic origin.

277 1 has crossed the heliopause into the nearby interstellar plasma.

278 , the border between the heliosheath and the interstellar plasma.

279 f Gamma, the H(2)S parent absorption and the interstellar radiation field implies that only ~26% of p

280 ervations at these wavelengths is limited by interstellar scattering.

281 all such stars enriched the local region in interstellar silicate and oxide dust.

282 olar wind plasma and carving out a cavity in interstellar space called the heliosphere.

283 rmation of the existence of HeH(+) in nearby interstellar space constrains our understanding of the c

284 nderstandings on this fundamental species in interstellar space obtained from our infrared observatio

285 nitiates chains of ion-molecule reactions in interstellar space thus leading to formation of complex

286 system early in its history, thus populating interstellar space with diffuse GWs.

287 volt X-rays, coupled with the discovery that interstellar space within about a hundred parsecs of the

288 ve been detected extraterrestrially, even in interstellar space, and are known to form nonenzymatical

289 the environment (natural waters, atmosphere, interstellar space, etc.), including biological systems

290 ecule, which has been postulated to exist in interstellar space, has thus far only been observed at l

291 is the case of the most abundant molecule in interstellar space, hydrogen, for which two spin isomers

292 ther with the known multitude of nitriles in interstellar space, suggest that the compound might also

293 n astronomy, indicating their persistence in interstellar space.

294 y disappeared as the ions streamed away into interstellar space.

295 be constituents of stellar/circumstellar and interstellar space.

296 how accelerated particles are released into interstellar space.

297 n has so far eluded unequivocal detection in interstellar space.

298 fraction of the original planetesimals into interstellar space.

299 mass ratio, which probably differ from their interstellar values.

300 show that recent determinations of the local interstellar velocity, based on interstellar atom measur