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The preparation of a magnetic-tape finding list for the first 10 sections of the U.S. National Bureau of Standards Reference Data System (NSRDS-NBS3) tables of optical multiplets of astrophysical interest (Moore, 1965-1983) is reported. The format of the list is described, and a sample page is provided.
The cross section for the dissociative excitation of the O I 1172.6 A multiplet is measured by the bombardment of O2 by 100 eV electrons. A cross section value of about 1.56 x 10 to the -22nd sq cm + or - 30 percent and an O I 1173 A/O I 989 A branching ratio of about 0.00013 + or - 35 percent are obtained. The branching ratio values are compared to the data of Morrison (1985) and Garstang (1961). The data reveal that the 1173 A branch from the O I (3s prime 3D0) state is not large enough to account for the discrepancy between the predicted and observed O I 989 A intensity in the earth's upper atmosphere.
Electron impact on O2 has been employed to ascertain the absolute cross-section value and emission linewidths of the OI (3s 5S0-3p 5P; 7774 A) multiplet. The emission linewidths are highly Doppler-broadened in dissociative excitation, and display two distinct kinetic energy distributions: which indicate that both purely repulsive and discrete, bound, excited molecular states, which then predissociate, are involved in the dissociation process that leads to the excitation of OI 7774 A. The magnitude of the measured cross-section and the fragment kinetic energy distribution both indicate that the previous time-of-flight studies of the metastable OI (5S0) state require reinterpretation.
Sounding rocket measurements of the O-I 989-A dayglow obtained in 1978, 1980, and 1985 are discussed. The 989-A intensity and multiplet ratios are consistent with total branching losses (to atomic states other than the ground state) of 1.5-4 x 10 to the -4th. It is found that the 1173/989 intensity ratio is dependent only on the 1173/989 branching ratio and the atomic oxygen concentration when viewing upward from rocket altitudes.
A nine-level atomic model is presented for C I lines synthesis in the sun. All the atomic parameters are based on recent experimental and theoretical data. Profiles of the multiplets at 1561 and 1657 A are computed from a model of the solar chromosphere. The sensitivity of the results to changes in the atomic parameters is examined. Partial frequency redistribution must be included in these lines to obtain agreement between calculated and observed profiles.
We report on large-scale ab initio multiconfiguration Hartree-Fock calculations for the UV0.01 multiplet, 2s(sup 2)2p(sup 2)P(sub J) - 2s2p(sup 2 4)P(sub J prime), in N III. The resulting transition probabilities agree very well with recent semiempirical calculations, and the lifetimes for two of the three upper levels agree with experiments. The deviation for the third level is discussed. Comparisons made with the highest quality IUE echelle spectra available -- those of RR Tel and V1016 Cyg (both photoionized sources with electron densities below 10(exp 8)/cu cm) -- show that computed branching ratios of lines sharing a common upper level are in agreement with observations to within uncertainties of +/- 10%. High-quality solar limb data or stellar data from the Hubble Space Telescope (HST) could, in principle, be used to determine whether the theoretical or measured lifetimes for the discrepant level are in error. Unfortunately, stellar data for high-density plasmas (N(sub e) greater than 10(exp 11)/cu cm are needed) do not yet exist, and existing solar data lack the photometric precision to address this problem.
Comparison of experimental and calculated data for Stark broadening parameters for the Ar II 4726.87 Å, 4879.86 Å and 4965.08 Å spectral lines from multiplet (3P) 4s 2P – (3P) 4p 2Do is presented in this work.
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On February 17, 2016, the IceCube real-time neutrino search identified, for the first time, three muon neutrino candidates arriving within 100 s of one another, consistent with coming from the same point in the sky. Such a triplet is expected once every 13.7 years as a random coincidence of background events. However, considering the lifetime of the follow-up program the probability of detecting at least one triplet from atmospheric background is 32%. Additionally, follow-up observatories were notified in order to search for an electromagnetic counterpart. Observations were obtained by Swift's X-ray telescope, by ASAS-SN, LCO and MASTER at optical wavelengths, and by VERITAS in the very-high-energy gamma-ray regime. Moreover, the Swift BAT serendipitously observed the location 100 s after the first neutrino was detected, and data from the Fermi LAT and HAWC observatory were analyzed. We present details of the neutrino triplet and the follow-up observations. No likely electromagnetic counterpart was detected, and we discuss the implications of these constraints on candidate neutrino sources such as gamma-ray bursts, core-collapse supernovae and active galactic nucleus flares. Here, this study illustrates the potential of and challenges for future follow-up campaigns.
The solid solutions between ilmenite (FeTiO{sub 3}) and hematite (α-Fe{sub 2}O{sub 3}) have recently attracted considerable attention as a spintronic material due to their interesting magnetic and electrical properties. In this study, the electronic and magnetic structures of epitaxially grown 0.6FeTiO{sub 3}·0.4Fe{sub 2}O{sub 3} solid solution thin films were investigated by combining x-ray absorption near-edge structure (XANES), x-ray magnetic circular dichroism (XMCD) for two different crystallographic projections, and first-principles theoretical calculations. The Fe L-edge XANES and XMCD spectra reveal that Fe is in the mixed-valent Fe{sup 2+}–Fe{sup 3+} states while Fe{sup 2+} ions are mainly responsible for the magnetization. Moreover, the experimental Fe L-edge XANES and XMCD spectra change depending on the incident x-ray directions, and the theoretical spectra explain such spectral features. We also find a large orbital magnetic moment, which can originate the magnetic anisotropy of this system. On the other hand, although the valence state of Ti was interpreted to be 4+ from the Ti L-edge XANES, XMCD signals indicate that some electrons are present in the Ti-3d orbital, which are coupled antiparallel to the magnetic moment of Fe{sup 2+} ions.
Predicting the rates of spin-dependent processes characterized by nonradiative transitions between electronic states with different spin multiplicities is important for understanding the mechanisms of many photochemical and catalytic reactions. To calculate these rates, it is necessary to define the spin state representation and the couplings between these states that drives the interstate transitions. In this work, we describe three different approaches to calculating the spin-orbit coupling (SOC), transition probabilities, and rate constants between the MS components of the electronic states with different spin multiplicities. We implemented these approaches in our nonadiabatic statistical theory (NAST) software package, which predicts the transition probabilities and rate constants of spin-dependent processes using information obtained from electronic structure calculations. Here, we discuss the advantage and drawbacks of each approach and, as an example, calculate the rate constants for transitions between the spin states in the active site model of the protein rubredoxin.
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