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K. T(phase III-ii). We estimate flux of electromagnetic emission fromthe jet and discuss its detectability in Section 3. Section 4 is devoted
to summary and discussion.

KMIHLON

2 E VO L U T I O N O F A D I S C I N B B H S Y S T E M S
2.1 Initial evolution

We consider an equal-mass binary of initial separation Rini andmass of BHs MBH , where the separation should be small such thatthe binary can merge in the Hubble time. Some mechanisms areproposed to realize this situation, such as the common envelope
evolution (Kinugawa et al. 2014; Belczynski et al. 2016) and/or thefriction by dense gas (Bartos et al. 2016). We focus on an accretiondisc around one of the BHs. We do not discuss the origin of this disc,which might be fallback material of supernova explosion (e.g. Pernaet al. 2014) or a tidally disrupted object (e.g. Seto & Muto 2011).
Consider a gas ring around a BH. The ring expands both inward
and outward due to the viscous diffusion to become an accretion
disc (e.g. Pringle 1981). When the outer radius of the disc, rout ,becomes close to Rini , the tidal torque from the companion prevents the disc from expanding outward (Papaloizou & Pringle 1977;
Artymowicz & Lubow 1994; Ichikawa & Osaki 1994). The balance
between the viscous torque and the tidal torque determines the discradius, and it is expected that the outer radius of the disc is fixedat rout ∼ asep Rini , where we introduce a separation parameter asep .
We fix asep = 0.3 in this paper for simplicity (Paczynski 1977). Thethe viscoustime (e.g. Pringle1981)of the poloidal currents Jp (open arrows), the poloidal Po
disc expands to rout inFig.
3. Schematicpicture
1 ! rout "2 arrows), and the poloidal particle energy flux Fp near the equatorial plane (i.e., thetvis =α"K H
negative energies; striped arrow) in the steady state in the northern hemisphere in the KS"2!
3/2
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s,energy directly(1) by Sp along the field lines threading the horizon (seei,12 M1.5 α−1HFneartheequatorialplane, which is associated with Sp along the field lines threading tp#
where "K = GMBH/r 3ergosphereis the Keplerian
angular3).velocity,the(see Sect.
H = cs /"K is the scaleheight (cs is the sound speed),
M1.5 = MBH /30 M⊙ , α −1 = α/0.1, Ri, 12 = Rini /(1012 cm) and(>Downloaded from http://mnras.oxfordjournals.org/ at Tohoku UniverKMIHLON>KMIHLON=AC$)+

Figure 1. Schematic evolutionary tracks of the disc mass (red), the massaccretion rate (blue) and the binary separation (magenta). Note that this isa double logarithmic plot and that phase II is much longer than the other

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9. 李 宇珉 研究室：恒星物理学

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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。
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固有振動（脈動）の研究を行う。

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