Excitation energies and oscillator strengths from the 1S0 ground state to the first 3P10 and 1P10 excited states of Mg-like ions are calculated using the multiconfiguration relativistic random-phase approximation including excitation channels from core electrons. The discrepancies between the relativistic random-phase approximation calculation and experimental results for the intercombination excitation energies and oscillator strengths are much reduced. The excitation energies and oscillator strengths for the resonance transition from the multiconfiguration relativistic random-phase approximation are in excellent agreement with experiment. A substantial part of the discrepancy in the 3P10-1P10 separations is resolved when core excitation channels are taken into account.
The electromagnetic properties of neutrinos, which are either trivial or
negligible in the context of the Standard Model, can probe new physics and have
significant implications in astrophysics and cosmology. The current best direct
limits on the neutrino millicharges and magnetic moments are both derived from
data taken with germanium detectors with low thresholds at keV levels. In this
paper, we discuss in detail a robust, ab initio method: the multiconfiguration
relativistic random phase approximation, that enables us to reliably understand
the germanium detector response at the sub-keV level, where atomic many-body
physics matters. Using existing data with sub-keV thresholds, limits on reactor
antineutrino's millicharge, magnetic moment, and charge radius squared are
derived. The projected sensitivities for next generation experiments are also
given and discussed
Excitation energies and oscillator strengths from the 'So ground state to the first 'P l and 'P & excited states of Zn-like ions are calculated by using the multiconfiguration relativistic random-phase approximation including excitation channels from core electrons. The disagreements among theories and experiments are much reduced but in general remain. PACS number(s): 31.20.d, 32.70.Cs
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