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given σ w . In Section 3.2, we will see that κ w and τ diss slightly change
the velocity profile through the cooling effect. In other words, thesetwo parameters change lr, syn and ηsyn (see also the discussion inSection 4.2). We also study dependence of the nebular flow profiles
on rTS in Section 3.3 as an interesting topic.
We take κ w = 104 and rTS = 0.1 pc as fiducial values from the paststudies (e.g. Kennel & Coroniti 1984a,b). We vary τ diss from 10 yr(fast dissipation) to ∞ (no dissipation). For the wind magnetization
parameter σ w , we study three representative cases of σ w = 0.1, 10,
and 103 and also σ w = 0.003, which corresponds to KC model. Notethat the cases of σ w = 1 do not show a special behaviour, and we
do not study the cases of σ w ≥ 104 for which the strong shock jumpcondition is not available (see equation A10). The values of τ conv
are derived for each combination of (σ w , κ w , rTS , τ diss ) in order toreproduce β(rPWN )c = 1500 km s−1 .

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*HDownloaded from http://ptep.oxfordjournals.org/ at Tohoku UFig. 3. Schematic picture of the poloidal currents Jp (openthe poloidal Poynting flux Sp (filled3.1arrows),
Flow dynamics
arrows), and the poloidal particle energy flux Fp near the equatorial plane (i.e., the inflow of the particle
Fig. 1 hemispherecompares theflow
dynamics fordissipation timenegative energies; striped arrow) in the steady state in the northernin theKS coordinates.
Thedifferent
BH. Allthree(seemagnetization
casesof σ w = 0.1 (red solid),τ disstheloses its rotational energy directly by Sp along the field linesscales
threadinghorizonSects. 4 and 5)
and byFp near the equatorial plane, which is associated with Sp along
fieldlines threading
the equatorialplaneindotted) areoverplotted.
The thin and
10 the(bluedashed),
103 (green
the ergosphere (see Sect. 3).
thick lines correspond to the fast (τ diss =10 yr) and no (τ diss = ∞)• Roi!cqY_HkQaZj
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dissipation models, respectively. r = 0.1 pc and κ = 10 are
commonin all theseplots.
we plot the profiles of6PbmSq!H+%N"CD:IA8For typical AGN jets,ℓ is expected to be ∼ 10 ordersof magnitude
smallerthan For
GM reference,/c •(cf. Ref.
KC model including the synchrotron cooling effect (σ = 0.003,TSgy

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• \qTi[qHw[47]), so that the distance that a particle travels until it achieves 4the asymptotic azimuthal velocity isκ w = 10 , rTS = 0.1 pc, and τ diss = τ conf = ∞). Note that thetiny compared to the size of the ergosphere. This justifies our calculations of the particle motion inhorizontal axes are not the distance from the pulsar r but from 

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脈動変光星の理論的研究

近年、MOST, CoRoT, Kepler衛星などを使った観測により極めて質の高いデータが大量に提供されるようになり、脈動変光星の研究はほとんど革命的な変革を受けた。当研究室では、恒星脈動を使ってその内部構造を探る。

SGR 1900+14: Giant γ FlareJPHLIGRFMS
Chaplin& Miglio (2013)
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