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As a consequence, the baseband polluting term can be expressed as [13] s_{TxL}(n) = left[h_{text{Rx}}(t)star vert h_{text{TxL}}(t)star tilde{s}_{Tx}(t)vert^{2}right]_{t = n T_{Rx}} (2).
A star and T star for each superflare star were taken from Huber et al. (2014), and we assumed T spot=4,000 K (Berdyugina 2005).
The heat transfer across the windows is ∑ Q Window = ∑ A z U W T a - T star + I SHGF, Open image in new window (35).
From (2), the polluting term can be expressed as: begin{array}rcl@ U t) &=& h_{text{Rx}}(t) star vert tilde{s}_{Tx}(t) vert^{2} end{array} (3).
The heat transfer through external walls (and roof) for room zone and tower zone is predicted as ∑ Q external = ∑ ne A z T star - T z R, Open image in new window (33).
where A star is the apparent area of the star and T spot and T star are the temperatures of the starspot and photosphere of the star (Notsu et al. 2013b), respectively.
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Assuming a sudden expansion at time t (star-coalescence), per-gene mutation rate μ and no drift or migration since then, we would expect n = t· μ· N new mutations in a sample of N. From the network, we count 34 putative mutations among 198 White Sea group individuals in the cyt-b sequence, which, given μ = 0.75·10-8·1131 bp, would be expected in t = 34/(μ·198) ≈ 20 ky (a minimum estimate).
Besides these three major classes, there are also several miscellaneous variables: R Coronae Borealis stars, T Tauri stars, flare stars, pulsars (neutron stars), spectrum and magnetic variables, X-ray variable stars, and radio variable stars.
(3) Miscellaneous and special types of variables R Coronae Borealis stars, T Tauri stars, flare stars, pulsars (neutron stars), spectrum and magnetic variables, X-ray variable stars, and radio variable stars.
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