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1 cosmic rays break apart larger nuclei in the interstellar medium).
2 -bearing dust particles still permeating the interstellar medium.
3 ntributing to deuterium fractionation in the interstellar medium.
4 ture and the direction of motion through the interstellar medium.
5 gnetic field strength and orientation in the interstellar medium.
6 and forms a bubble of solar material in the interstellar medium.
7 gitude straddling the direction of the local interstellar medium.
8 rowth and carbonaceous dust evolution in the interstellar medium.
9 undly affects the growth of molecules in the interstellar medium.
10 monolayers in cold and dense regions of the interstellar medium.
11 n lengths than those observed in the diffuse interstellar medium.
12 formation of carbon-bearing molecules in the interstellar medium.
13 celerates to begin its merger into the local interstellar medium.
14 n of these isomers in the laboratory and the interstellar medium.
15 traviolet) spectral signature of dust in the interstellar medium.
16 licates that are abundant in IDPs and in the interstellar medium.
17 tion of sulfur between solids and gas of the interstellar medium.
18 ealing new insight into the chemistry of the interstellar medium.
19 st abundant nitrogen-bearing molecule in the interstellar medium.
20 ar objects and collides with the surrounding interstellar medium.
21 the physical and chemical conditions in the interstellar medium.
22 nlikely to survive in high abundances in the interstellar medium.
23 that the EUV flux cannot be an effect of the interstellar medium.
24 encounters to synthesize C3H radicals in the interstellar medium.
25 he complex molecular species observed in the interstellar medium.
26 ow they are formed in different areas of the interstellar medium.
27 e that is actively being searched for in the interstellar medium.
28 xyl radicals (OH) play a central role in the interstellar medium.
29 relevant complex organic molecules (COMs) in interstellar medium.
30 and the accelerated growth of grains in the interstellar medium.
31 ly due to low-resolution models of the local interstellar medium.
32 few specific PAHs have been detected in the interstellar medium.
33 core-collapse supernova explosions into the interstellar medium.
34 n the evolution of chemical diversity in the interstellar medium.
35 tride (PN) is a carrier of phosphorus in the interstellar medium.
36 bons (PAHs) contain 20% of the carbon in the interstellar medium.
37 chemistry of combustion, pyrolysis, and the interstellar medium.
38 d to be widespread in different areas of the interstellar medium.
39 onment, but consistent with formation in the interstellar medium.
40 nd in flames, comets, stars, and the diffuse interstellar medium.
41 cal shocks, stellar corona and wind, and the interstellar medium.
42 n their search for aromatic molecules in the interstellar medium.
43 ized PAHs, 1- and 2-cyanonaphthalene, in the interstellar medium.
44 nally excited OH(X) radicals observed in the interstellar medium.
45 s via pyridine to NPAH-type molecules in the interstellar medium.
46 distribution, and chemistry of anions in the interstellar medium.
47 enized, likely by repeated processing in the interstellar medium.
48 lar dust (ISD) is the condensed phase of the interstellar medium.
49 er mille, close to compositions in the local interstellar medium.
50 onments, from the atmosphere of Titan to the interstellar medium.
51 ydrodynamic interaction of the wind with the interstellar medium.
52 uter heliosphere, to about 0.1 cm(-3) in the interstellar medium.
53 rature ices relevant to the solar system and interstellar medium.
54 between the solar plasma and the much cooler interstellar medium.
55 s by twisting of field lines frozen into the interstellar medium.
56 ow-density environments of the Earth and the interstellar medium.
57 liosheath depletion region), rather than the interstellar medium.
58 organic matter, probably originating in the interstellar medium.
59 -3), very close to the value expected in the interstellar medium.
60 e the synthesis of the very first PAH in the interstellar medium.
61 iated formation of aromatic molecules in the interstellar medium.
62 ields than in stellar ejectae or the diffuse interstellar medium.
63 cently detected in the denser regions of the interstellar medium.
64 a new model of the formation of H(2) in the interstellar medium.
65 It governs the chemistry and physics of the interstellar medium.
67 2.3 x 10(-5) is consistent with that in the interstellar medium (after allowing for Galactic chemica
68 iamonds due to grain-grain collisions in the interstellar medium although a low-pressure mechanism of
69 d most easily studied sample of the Galactic interstellar medium, an understanding of which is essent
70 ction dominates at energies relevant for the interstellar medium and alone may explain observations i
71 mportance to form PAH-like structures in the interstellar medium and also in hydrocarbon-rich, low-te
72 rmation of PAHs and their derivatives in the interstellar medium and carbonaceous chondrites and coul
77 cies under low-temperature conditions in the interstellar medium and in hydrocarbon-rich atmospheres
79 Efforts to unveil the structure of the local interstellar medium and its recent star-formation histor
80 by photochemical reactions prevailing in the interstellar medium and later incorporated into asteroid
82 the bulk of their cosmogenic nuclides in the interstellar medium and not by exposure to an enhanced p
83 nt roles in extreme environments such as the interstellar medium and planetary atmospheres (CN, SiN a
89 5.8 inject large amounts of energy into the interstellar medium and suppress nuclear gas accretion,
91 atter in meteorites might have formed in the interstellar medium and/or the solar nebula, but was alm
92 produces cloud and intercloud phases in the interstellar medium, and disrupts molecular clouds (the
94 ned in conditions approximating those of the interstellar medium, and measured over the entire spectr
95 oduce heavy elements, inject energy into the interstellar medium, and possibly regulate the star form
98 are the best analogues to investigating the interstellar medium at a quasi-primitive environment in
100 generally thought to have originated in the interstellar medium, but it might have formed in the sol
101 agrees with the present value for the local interstellar medium, but seems to be incompatible with t
102 ecules in the astrochemical evolution of the interstellar medium, but the formation mechanism of even
103 y role in the astrochemical evolution of the interstellar medium, but the formation mechanism of even
104 es a change in the average properties of the interstellar medium, but the measurements are systematic
105 e molecules, H(2)S, are both detected in the interstellar medium, but the returned SH(X)/H(2)S abunda
106 sition of mass, momentum and energy into the interstellar medium by massive stars ('feedback') are th
109 massive stars(20,21), and released into the interstellar medium by Type II supernova explosions(2,22
110 osed that gas-phase organic chemistry in the interstellar medium can be initiated by the methyl catio
111 tents, and their ratio, are examined for the interstellar medium, comets, chondritic meteorites, and
112 otter than the 1,000,000 to 2,000,000 kelvin interstellar medium component in the Milky Way Galaxy.
114 the Sun through the dynamically active local interstellar medium creates an evolving heliosphere envi
115 r second(7), must 'sweep up' the surrounding interstellar medium, creating cavities in space around t
117 rticle density compared to the local average interstellar medium embedding our SS for the past few mi
119 tilted approximately 20-30 degrees from the interstellar medium flow direction (resulting from the p
121 enerated by cosmic-ray interactions with the interstellar medium, focusing primarily on the relevance
122 s indiscernible from Faraday rotation in the interstellar medium for typical GHz observations frequen
123 approximately 10(3) times that of the local interstellar medium (for example, owing to an O or B sta
124 and thereby prevents the metallicity of the interstellar medium from increasing steadily with time.
127 150 years, the prevailing view of the local interstellar medium has been based on a peculiarity know
129 ellar feedback (the momentum return into the interstellar medium) has been considered incapable of ra
130 which may themselves be very abundant in the interstellar medium, has led to the suggestion that ioni
131 udy interplanetary dust, Venus' tail and the interstellar medium.) Here we report the serendipitous d
132 ay, and the absorption of soft X-rays in the interstellar medium hinders the determination of the cau
134 l properties and elemental abundances of the interstellar medium in galaxies during cosmic reionizati
138 masses of highly excited, chemically evolved interstellar medium in this galaxy, which constitutes at
139 nization, cosmic rays also interact with the interstellar medium in ways that heat the ambient gas, p
140 eated by the supernovae swept up the ambient interstellar medium into an extended shell that has now
145 simulation experiments demonstrates that the interstellar medium is host to an unanticipated and coun
148 lative motion of the Sun with respect to the interstellar medium is slower and in a somewhat differen
149 redshifts of two to three, by which time the interstellar medium is sufficiently enriched with metals
150 f astronomical environments such as the cold interstellar medium (ISM) and (exo)planetary atmospheres
151 c hydrocarbons (PAHs) are omnipresent in the interstellar medium (ISM) and also in carbonaceous meteo
152 try has vital importance in the evolution of interstellar medium (ISM) and circumstellar regions, suc
153 y role in the astrochemical evolution of the interstellar medium (ISM) and in the chemistry of combus
154 largest noncyclic molecules detected in the interstellar medium (ISM) are organic with a straight-ch
158 large fraction of their original mass to the interstellar medium (ISM) through a processed, dusty, mo
159 ttribute this to the high Mach number in the interstellar medium (ISM), although the exact details of
160 arbons in ionizing environments, such as the interstellar medium (ISM), and some combustion condition
161 rimitive sugar-like molecule detected in the interstellar medium (ISM), is a potential precursor for
164 g our Galaxy is a crucial constituent of the interstellar medium: it mediates the dynamics of interst
166 of the heliosphere indicates that the local interstellar medium (LISM) magnetic field (B(LISM)) is t
170 ion pathways under extreme conditions of the interstellar medium (low temperature, radiation) have re
171 gnetic bubble, the heliosphere, in the local interstellar medium (mostly neutral gas) flowing by the
172 strength and orientation of the field in the interstellar medium near the heliosphere has been poorly
173 ecules (rather than from dust grains) in the interstellar medium, no consensus has been reached regar
174 ich the AGN drives an outflow, expelling the interstellar medium of its host and transforming the gal
177 cted if they had propagated only through the interstellar medium of the Milky Way-indicate extragalac
179 with only a moderate impact on the internal interstellar medium of W0410-0913, which is sustained by
181 nated in a very cold environment such as the interstellar medium or outer region of the solar nebula,
182 eorites are interpreted as a heritage of the interstellar medium or resulting from ion-molecule react
183 ) release huge quantities of energy into the interstellar medium, potentially clearing the surroundin
184 erved the icy grains originally found in the interstellar medium prior to solar system formation.
186 ombination with our current knowledge of the interstellar medium revealed that the EUV flux cannot be
188 mark of gas-phase chemical processing in the interstellar medium, suggesting that interstellar gases
189 H(3)), is the smallest amide detected in the interstellar medium that can exist as cis and trans isom
190 been formed from material inherited from the interstellar medium that suffered little processing in t
191 cular species that have been detected in the interstellar medium, the singlet carbene cyclopropenylid
192 lyzed grains were parts of aggregates in the interstellar medium: The large difference in nuclear rec
193 ingle-collision conditions as present in the interstellar medium, this core loses a hydrogen atom to
196 ploited to probe the exotic chemistry of the interstellar medium toward the discovery of this molecul
197 ecies have been definitively detected in the interstellar medium via their rotational, infrared, and/
199 butadiyne (MeC5N), a molecule present in the interstellar medium, was established in order to circumv
200 estimate that the irradiated objects in the interstellar medium were up to 30 times larger than the
201 c C(6) ring in hydrocarbon flames and in the interstellar medium where concentrations of dicarbon tra
202 actants, this reaction is viable in the cold interstellar medium where several methyl-substituted mol
203 inated by heated solar plasma, and the local interstellar medium, which is expected to contain cold n
206 ronomy, primarily because the opacity of the interstellar medium would prevent observations at these