ライフサイエンスコーパス: interstellar

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

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

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

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

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

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

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

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

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

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

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

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

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

14 The diffuse interstellar bands (DIBs), ubiquitous absorption feature

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

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

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

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

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

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

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

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

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

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

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

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

27 lar gas excited by shocks from outflows, and interstellar 'bullets'.

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

29 nd may provide insights on the formation and interstellar chemistry of unsaturated species such as th

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

31 3+ molecular ion plays a fundamental role in interstellar chemistry, as it initiates a network of che

32 importance: models of steady-state gas-phase interstellar chemistry, together with millimetre-wavelen

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 Organic molecules in dense interstellar clouds may ultimately be traced back to car

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 In dense interstellar clouds, the H3+ abundance is understood usi

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

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

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

52 he boundary layers between diffuse and dense interstellar clouds.

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

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

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

56 ent of the H3+ destruction rate under nearly interstellar conditions.

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

58 can in principle be used to communicate over interstellar distances.

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

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

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

62 The interstellar dust candidates are readily distinguished f

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

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

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

66 ly hidden at optical wavelengths (because of interstellar dust grains); this energy now forms part of

67 ected submillimetre emission originates from interstellar dust in a molecular cloud complex located i

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

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

70 ing structures are infrared echoes, in which interstellar dust is heated by the explosion and by flar

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 nd in meteorites, protoplanetary nebulae and interstellar dusts, as well as in residues of detonation

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 and is shown to be associated globally with interstellar features that have been observed at radio a

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

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

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

86 long been postulated as constituents of the interstellar gas and circumstellar disks.

87 hing with nebular material, dense pockets of interstellar gas excited by shocks from outflows, and in

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

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

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

91 The interstellar gas, mainly consisting of hydrogen molecule

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

93 Synthesized on interstellar grains and eventually incorporated into the

94 5.7-electron volt (2175 angstrom) feature in interstellar grains embedded within interplanetary dust

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

96 Interstellar grains of typical size approximately 0.1 mi

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

98 traviolet photolysis of the analogues of icy interstellar grains.

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

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

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

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

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

104 s is produced by UV photolysis of realistic, interstellar ice analogs, and that some of the component

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

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

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

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

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

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

111 nation of radicals in ultraviolet-photolyzed interstellar ices at low temperatures.

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

113 Evolved interstellar ices observed in dense protostellar molecul

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

115 Interstellar ices, the building blocks of comets, tie up

116 a source of organic molecules in comets and interstellar ices.

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

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

119 y have important implications for the global interstellar interaction.

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

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

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

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

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

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

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

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

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

129 Foreground clouds of interstellar material, however, complicate the interpret

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

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

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

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

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

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

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

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

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

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

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

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

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

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

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

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

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

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

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

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

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

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

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

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

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

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

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

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

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

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

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

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

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

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

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

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

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

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

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

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

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

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

172 The interstellar medium is characterized by a rich and diver

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

174 The interstellar medium is enriched primarily by matter ejec

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

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

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

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

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

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

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

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

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

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

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

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

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

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

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

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

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

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

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

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

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

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

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

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

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

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

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

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

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

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

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

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

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

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

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

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

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

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

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

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

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

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

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

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

219 iated formation of aromatic molecules in the interstellar medium.

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

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

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

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

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

225 gnetic field strength and orientation in the interstellar medium.

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

227 gitude straddling the direction of the local interstellar medium.

228 rowth and carbonaceous dust evolution in the interstellar medium.

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

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

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

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

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

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

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

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

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

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

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

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

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

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

243 ydrodynamic interaction of the wind with the interstellar medium.

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

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

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

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

248 ature formation of organic compounds in cold interstellar molecular clouds can produce carbon and nit

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

250 e a deuterium excess similar to that seen in interstellar molecular clouds, and the formation process

251 n low-pressure environments, such as in cold interstellar molecular clouds, in the outer reaches of t

252 , high-mass stars form in the dense cores of interstellar molecular clouds, where gas densities are n

253 The abundance of interstellar molecular nitrogen (N2) is of considerable

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

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

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

257 Here we report the detection of interstellar N2 at far-ultraviolet wavelengths towards t

258 r with millimetre-wavelength observations of interstellar N2H+ in dense molecular clouds predict that

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

260 'Pick-up ions' that originate as interstellar neutral atoms should be accelerated to tens

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

262 m radio spectrum that traces the intervening interstellar neutral hydrogen clouds.

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

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

265 not represent the main reservoir species for interstellar nitrogen.

266 orelevant molecules as planets form in their interstellar nurseries.

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

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

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

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

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

272 s lower (377%), but still consistent with an interstellar origin.

273 The seven candidate interstellar particles are diverse in elemental composit

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

275 ome meteoritic amino acids are the result of interstellar photochemistry, rather than formation in li

276 hock is that of anomalous cosmic rays and of interstellar pick-up ions.

277 d is apparently dominated by strongly heated interstellar pickup ions.

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

279 1 has crossed the heliopause into the nearby interstellar plasma.

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

281 excesses suggest that some organics have an interstellar/protostellar heritage.

282 ervations at these wavelengths is limited by interstellar scattering.

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

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

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

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

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

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

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

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

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

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

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

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 fraction of the original planetesimals into interstellar space.

298 n astronomy, indicating their persistence in 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