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1 results in the observed narrowing of the EPR spectral line.
2  is accompanied by substantial broadening of spectral lines.
3 mal and nonthermal continuum models, with no spectral lines.
4 nts describing a continuum, with no detected spectral lines.
5 t outflows have been observed in ultraviolet spectral lines(7), with velocities of more than 3,500 ki
6 is by its emission in hydrogen recombination spectral lines(7,8).
7 A emits bright signals in the phosphorus (P) spectral line against a low-contrast background, showed
8  levels, the mechanisms of the broadening of spectral lines, and the selected parameters of the spect
9 concept laser beam synthesized of two narrow spectral lines at 3.99 um and 4.25 um wavelengths is dem
10 e unmodified mismatched G.A duplex exhibited spectral line broadening at neutral pH, suggesting a mix
11 as replaced by diamagnetic Zn(2+) to prevent spectral line broadening of the Q(A)(.-) due to magnetic
12 of clusters provide physical insight only if spectral lines can be assigned to pairs of quantum state
13  The number and wavelengths of the generated spectral lines can be dynamically reconfigured.
14                                 Because both spectral lines correspond to the same Floquet-engineered
15        In an argon ambient however, infrared spectral lines dominate the spectrum, while the plasma a
16          In contrast, at Q-band, most of the spectral lines due to the DMPO/.SG were separated from t
17                                  Narrow-band spectral lines enable researchers to investigate the mat
18 tion, we successfully obtained well-resolved spectral lines even without time-gated detection.
19 ition energy can be resolved into a separate spectral line for each photon number state of the microw
20  using the periodic Doppler shift of stellar spectral lines have recently achieved a precision of 60
21 cal frequency combs, featuring evenly spaced spectral lines, have been extensively studied and applie
22 nction using dimensionless intensity of Fe I spectral lines(I*), dimensionless velocity(v*) and dimen
23                                 Detection of spectral line in gamma-ray bursts (GRBs) is importance f
24                                    We detect spectral lines in 23 out of 26 sources and multiple line
25 duces both cells growth arrest and alter the spectral lines in a dose-dependent manner.
26                     In addition, doubling of spectral lines in all of the observed samples provides e
27  finding, coupled with the observation of Tc spectral lines in certain stars, shows that the majority
28                                 The observed spectral line is approximately four times narrower than
29                                Broadening of spectral lines is a signature of chemical exchange pheno
30       Probe deuteration resulted in a narrow spectral line of 1.2 G compared to a nondeuterated analo
31 f about two millikelvin in the 21-centimetre spectral line of atomic hydrogen associated with stars a
32 e upper limit on the strength of the Brgamma spectral line of hydrogen.
33 es, given its weak response to the brightest spectral line of Jovian lightning emission, the 656.3-na
34                                              Spectral lines of C, Ca, Fe, Mg, N and Na were selected
35 ned in situ by cross-calibration between the spectral lines of different charge states, and even diff
36 or the lowfield spectral line, the remaining spectral lines of DMPO/ .SG virtually over-lap with thos
37 n shown that in these objects the rotational spectral lines of molecular hydrogen observed at mid-inf
38 ectric quadrupole moment, which broadens the spectral lines, often over several megahertz.
39 ncies, each emitting a comb of evenly spaced spectral lines over a wide spectral span.
40     The synthesis of multiple narrow optical spectral lines, precisely and independently tuned across
41   We interpret this feature as a blueshifted spectral line produced by the annihilation of electron-p
42 s by measuring the gravitational redshift of spectral lines produced in the neutron star photosphere.
43                                     From the spectral line profiles, the molecules can be distinguish
44 y Gaussian fitting, and modifications in the spectral lines, respectively, also suggested complex for
45  quantitative concentration measurements and spectral line shape analysis.
46                       The changes in the EPR spectral line shape and the rotational correlation time
47 ate lifetime broadening contributions to the spectral line shape arising from electronic-vibrational
48                                      Similar spectral line shape changes of FR3 are caused by the Frd
49 b and MGPPIXMb show no temperature-dependent spectral line shape changes suggestive of Jahn-Teller dy
50                                      Through spectral line shape comparison between VSFG and IR spect
51 folded polypeptide ligand, showed changes in spectral line shape consistent with restricted motion of
52                                  Finally, 2D spectral line shape evolution reveals that it takes the
53 om the electron paramagnetic resonance (EPR) spectral line shape of the reduced [2Fe-2S] cluster, whi
54    In wild-type E. coli QFR, HQNO causes EPR spectral line shape perturbations of the iron-sulfur clu
55 ch of the residues on SecB showed changes in spectral line shape upon addition of SecA.
56 significant inhomogenous contribution to the spectral line shape, which is quantified by simulations.
57 e followed, appearing as evolution of the 2D spectral line-shape during the first 200 fs after excita
58   The typical asymmetrically broadened Raman spectral line-shape from sufficiently doped n- and p-typ
59                                          The spectral line-shape is well-described by one isotropic a
60                                      The EPR spectral line shapes and the influence of nonpolar O2 or
61 lysis of the electron paramagnetic resonance spectral line shapes and the influence of O2 on the satu
62                                          The spectral line shapes are accurately reproduced using a H
63 urface facing the aqueous phase, and the EPR spectral line shapes at these sites indicate considerabl
64 (II) zero field splitting and broadening the spectral line shapes but had no effect on oxidized enzym
65                   The dramatically different spectral line shapes for both aggregates are shown to ar
66                                  The complex spectral line shapes observed in the MAS NMR spectra are
67  Judging from the evolution of photoemission spectral line shapes of molecular energy states, we disc
68 Furthermore, electron paramagnetic resonance spectral line shapes of sites in the N-terminal domain a
69 O and (71)Ga MAS NMR spectra display complex spectral line shapes that could be accurately predicted
70               FSED experiments on C1 yielded spectral line shapes that could not be simulated as the
71                                          The spectral line shapes were analyzed as a function of side
72                                              Spectral line shapes were analyzed in terms of side-chai
73 able changes in appearance and variations in spectral line shapes, are among the most active research
74 des were analyzed on the basis of 31P and 2H spectral line shapes, order parameters, and T1 relaxatio
75  vast amount of information contained in the spectral line shapes, the problems with sensitivity and
76 none does not alter the [2Fe-2S] cluster EPR spectral line shapes, which remain indicative of one ubi
77 -PLB with CD3-Ala15 exhibit strong isotropic spectral line shapes.
78             Herein, we elucidate the sub-gap spectral line-shapes of organic semiconductors and their
79                    Our studies show that the spectral line splits into distinctive spinon and holon e
80 e this capability to simultaneously generate spectral lines that are resonant with two chosen spatial
81 ture of the very long electron beam produced spectral lines that were observed to have frequencies up
82 ons and as a result, except for the lowfield spectral line, the remaining spectral lines of DMPO/ .SG
83  secular state to detect one clean and sharp spectral line.This study demonstrates a top-down approac
84 ver more than 80 days, red colour and narrow spectral lines, which seem inconsistent with those obser
85                               Improvement of spectral line width from 4.8 Hz to 3.5 Hz was observed a
86  and experimental evidence suggests that the spectral line width is a result of multiple, discrete el
87 ibutions (sigma = 0.5-2%) are obtained whose spectral line widths are dominated (73-83%) by the intri
88 verse correlation was also found between the spectral line widths of coated SWCNTs and the efficiency
89 photoluminescence intensity and narrowing of spectral line widths with electrolyte addition, indicati
90 orporation of a capillary spinner to improve spectral line widths, and (3) facile sample changing via
91                To correlate the intensity of spectral line with the hardness of molten zone, the meth
92  from a very wide, inhomogeneously broadened spectral line with time-averaged single ensemble lumines
93  synthesis of multiple independently tunable spectral lines, with >1 muJ high pulse energies and a fe