Thermal spectrum

Zane, S. et al. (2001), Proton cyclotron features in thermal spectra of ultramagnetized neutron stars , ApJ 560, 384. 

Thermoanalytical methods essentially encompass such techniques that are based entirely on the concept of heating a sample followed by well-defned modified procedures, such as gravimetric analysis, differential analysis and titrimetric analysis. In usual practice, data are generated as a result of continuously recorded curves that may be considered as thermal spectra . These thermal spectra also termed as thermograms, often characterize a single or multicomponent system in terms of ... 

The model spectra contain two component of thin thermal spectra with different Te and r. The 90% confidence level contour in logr-Te plane are shown in fig. 3. 

The Fermi-energy pie = ll.l(pioi )1/3 MeV. The difference in chemical potentials /t, and the relative fraction of free protons are obtained from a low density analytic equation of state similar to that in [90] with modifications noted in [88], Shown in Fig. 15 is a typical snapshot spectrum of neutrinos from a 15 Mq star s core collapse within a narrow range of stellar core density around 1011 gm cm-3. Note the two separate peaks from captures on free protons and heavy nuclei which have non-thermal spectra. 

At zero stress, a moderate temperature rise of samples containing the >(H,0) centres results in the observation of two thermalized spectra >2(14,0) and >3(H,0) with 2p i lines at 8.224 and 7.76meV, respectively [185], If it is assumed that the final states of the lines of these spectra are the same as those of >i(H,0), one deduces (H, O) - >2 (H, O) and >1 (H, O) - >3 (H, O) energy separations of 2.512 and 2.98 meV, respectively. Thus, the thermal population of the Is ( >2) and Is ( >3) states corresponding to these energy differences should result in intensity ratios between the >2 and >3 spectra on the one hand and the >1 spectrum on the other hand, smaller than those actually measured. A fit of the measured intensity ratios to the splitting deduced from the realistic Boltzmann factors gives only 1.57 and 1.94 meV for... 

Typical thermal spectra (see Figures 2.3 and 2.4) may contain one or more exothermic peaks due to crystallization of different phases, but only the lowest temperature peak is considered in discussing glass stability. Once a significant number of crystals are formed, subsequent events at higher temperatures are not considered important in glass stability discussions. 

Calculated reactor neub measured value of 6.94 adjacent to fuel clusters and 5.48 in the moderator, halfway between tubes. The neutron spectral index was calculated at (Afferent positions in the unit cell and the Core using thermal spectra obtained with ffie SLOP-1 code. Measurements d this quantity were done with Lu foils. 

In preparation for the experiment, extensive calculations and selected critical facility measurements were made. The basic analytical approach is the multigroup method in the Sn and diffusion theory approximations to the transport equation. The fast and epithermal spectra used in computing the multigroup cross sections are calculated using HRO. The thermal spectra are calculated using Battelle Revised THERMOS. ) The NeUdn kernel is used to describe the thermal-neutron scattering in water. 

Extensive criticality calculations have been done for this rack to ensure that it meets the applicable criteria under all conditions. The calculations were performed using a four-energy-group, X-Y representation of the racks in the PDQ-07 (Ref. 4) program. Cross sections fo>r the POQ-07 model were obtained from LEOPARD (Ref. 5) super cell calculations, which also yielded fast and thermal spectra for use in RODWORTH (Ref. 6), a blackness theory code which was modified to account for boron particle self-shielding. The resulting cross sections were then - used in a PDQ-07 calculation which explicitly modeled the system geometry. 

Westcott C E. Effective Cross Section Values for Well-Moderated Thermal Spectra., CBRP-96d ED3 Rev. November 1 I960. 

The spectral selectivity of a solar absorber can be judged by comparing its solar absorptance and thermal emittance with the ideal values. Because of the overlap of the solar and thermal spectra, as seen in Fig. 1, the solar absorptance of the ideal surface is limited to a maximum of about 0.99 and the total emittance (600 K) is limited to a minimum of about 0.01. 

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