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Radio magnetic indicator

Fig. 10.4 Experimental scheme for the 2D [ N. HJ-TROSY using single transition to single transition polarization transfer (box labeled ST2-PT). On the lines marked H and 15N, narrow and wide bars stand for nonselective 90° and 180° radio-frequency pulses, respectively. The delay t=2.7 ms (see text). The line marked PFG indicates the pulsed magnetic field gradients applied along the z-axis G, amplitude 30 G/cm, duration 1 ms G2, 40 G/cm, 1 ms G3, 40 G/cm, 1 ms ... Fig. 10.4 Experimental scheme for the 2D [ N. HJ-TROSY using single transition to single transition polarization transfer (box labeled ST2-PT). On the lines marked H and 15N, narrow and wide bars stand for nonselective 90° and 180° radio-frequency pulses, respectively. The delay t=2.7 ms (see text). The line marked PFG indicates the pulsed magnetic field gradients applied along the z-axis G, amplitude 30 G/cm, duration 1 ms G2, 40 G/cm, 1 ms G3, 40 G/cm, 1 ms ...
There are precedents that indicate this is indeed likely to be the case. For example, around the middle of the nineteenth century, the Scottish physicist James Clerk Maxwell developed a theory that gave a unified explanation of the phenomena of electricity and magnetism. Not only did the theory suggest that light was made up of electromagnetic waves, it also led to the discovery of such new phenomena as radio transmission. [Pg.217]

Figure 6.3. Left. The overall observed spectrum of the Coma cluster from radio to gamma-ray frequencies (see labels). Right. The constraints to the spectrum of relativistic electrons in Coma as obtained from different observation (see labels) the radio halo data (blue dashed lines) for different values of the IC magnetic field the HXR data (red solid fine with arrows), the EUV data (green solid line with arrows) and the EGRET upper limit (magenta arrow). The arrows indicate that the spectra should be considered as upper limits, because we cannot exclude that a fraction of the HXR and EUV flux is provided by active galaxies or warm gas, respectively. Figure 6.3. Left. The overall observed spectrum of the Coma cluster from radio to gamma-ray frequencies (see labels). Right. The constraints to the spectrum of relativistic electrons in Coma as obtained from different observation (see labels) the radio halo data (blue dashed lines) for different values of the IC magnetic field the HXR data (red solid fine with arrows), the EUV data (green solid line with arrows) and the EGRET upper limit (magenta arrow). The arrows indicate that the spectra should be considered as upper limits, because we cannot exclude that a fraction of the HXR and EUV flux is provided by active galaxies or warm gas, respectively.
Figure 11.47. Magnetic hyperfine and spin-rotation splitting of the v = 17, N= 1 level of HD+. The infrared transitions indicated correspond to the lines observed in figure 11.43. The five radio frequency double resonance transitions observed were all between the G = 0 and 1 levels. Figure 11.47. Magnetic hyperfine and spin-rotation splitting of the v = 17, N= 1 level of HD+. The infrared transitions indicated correspond to the lines observed in figure 11.43. The five radio frequency double resonance transitions observed were all between the G = 0 and 1 levels.

See other pages where Radio magnetic indicator is mentioned: [Pg.1270]    [Pg.1270]    [Pg.85]    [Pg.214]    [Pg.35]    [Pg.238]    [Pg.7]    [Pg.339]    [Pg.71]    [Pg.405]    [Pg.295]    [Pg.23]    [Pg.531]    [Pg.976]    [Pg.179]    [Pg.164]    [Pg.81]    [Pg.86]    [Pg.87]    [Pg.33]    [Pg.11]    [Pg.389]    [Pg.178]    [Pg.177]    [Pg.177]    [Pg.42]    [Pg.844]    [Pg.133]    [Pg.169]    [Pg.418]    [Pg.460]    [Pg.203]    [Pg.40]    [Pg.392]    [Pg.195]    [Pg.993]    [Pg.2]    [Pg.501]    [Pg.315]    [Pg.470]    [Pg.531]    [Pg.207]    [Pg.250]    [Pg.214]    [Pg.1687]    [Pg.426]   
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