FORMATION OF OVERHEATED REGIONS AND TRUNCATED DISKS AROUND BLACK HOLES: THREE-DIMENSIONAL GENERAL RELATIVISTIC RADIATION-MAGNETOHYDRODYNAMICS SIMULATIONS

作者：Takahashi Hiroyuki R; Ohsuga Ken; Kawashima Tomohisa; Sekiguchi Yuichiro

来源：Astrophysical Journal, 2016, 826(1): 23.

DOI：10.3847/0004-637X/826/1/23

<jats:title>ABSTRACT</jats:title>
<jats:p>Using three-dimensional general relativistic radiation-magnetohydrodynamics simulations of accretion flows around stellar mass black holes, we report that the relatively cold disk (<jats:inline-formula>
<jats:tex-math>
<?CDATA $\gtrsim {10}^{7}\;{\rm{K}}$?>
</jats:tex-math>
<jats:inline-graphic xmlns:xlink="http://www.w3.org/1999/xlink" xlink:href="apjaa2778ieqn1.gif" xlink:type="simple" />
</jats:inline-formula>) is truncated near the black hole. Hot and less dense regions, of which the gas temperature is <jats:inline-formula>
<jats:tex-math>
<?CDATA $\gtrsim {10}^{9}\;{\rm{K}}$?>
</jats:tex-math>
<jats:inline-graphic xmlns:xlink="http://www.w3.org/1999/xlink" xlink:href="apjaa2778ieqn2.gif" xlink:type="simple" />
</jats:inline-formula> and more than 10 times higher than the radiation temperature (overheated regions), appear within the truncation radius. The overheated regions also appear above as well as below the disk, sandwiching the cold disk, leading to the effective Compton upscattering. The truncation radius is <jats:inline-formula>
<jats:tex-math>
<?CDATA $\sim 30{r}_{{\rm{g}}}$?>
</jats:tex-math>
<jats:inline-graphic xmlns:xlink="http://www.w3.org/1999/xlink" xlink:href="apjaa2778ieqn3.gif" xlink:type="simple" />
</jats:inline-formula> for <jats:inline-formula>
<jats:tex-math>
<?CDATA $\dot{M}\sim {L}_{{\rm{Edd}}}/{c}^{2}$?>
</jats:tex-math>
<jats:inline-graphic xmlns:xlink="http://www.w3.org/1999/xlink" xlink:href="apjaa2778ieqn4.gif" xlink:type="simple" />
</jats:inline-formula>, where <jats:inline-formula>
<jats:tex-math>
<?CDATA ${r}_{{\rm{g}}},\dot{M},{L}_{\mathrm{Edd}},c$?>
</jats:tex-math>
<jats:inline-graphic xmlns:xlink="http://www.w3.org/1999/xlink" xlink:href="apjaa2778ieqn5.gif" xlink:type="simple" />
</jats:inline-formula> are the gravitational radius, mass accretion rate, Eddington luminosity, and light speed, respectively. Our results are consistent with observations of a very high state, whereby the truncated disk is thought to be embedded in the hot rarefied regions. The truncation radius shifts inward to <jats:inline-formula>
<jats:tex-math>
<?CDATA $\sim 10{r}_{{\rm{g}}}$?>
</jats:tex-math>
<jats:inline-graphic xmlns:xlink="http://www.w3.org/1999/xlink" xlink:href="apjaa2778ieqn6.gif" xlink:type="simple" />
</jats:inline-formula> with increasing mass accretion rate <jats:inline-formula>
<jats:tex-math>
<?CDATA $\dot{M}\sim 100{L}_{{\rm{Edd}}}/{c}^{2}$?>
</jats:tex-math>
<jats:inline-graphic xmlns:xlink="http://www.w3.org/1999/xlink" xlink:href="apjaa2778ieqn7.gif" xlink:type="simple" />
</jats:inline-formula>, which is very close to an innermost stable circular orbit. This model corresponds to the slim disk state observed in ultraluminous X-ray sources. Although the overheated regions shrink if the Compton cooling effectively reduces the gas temperature, the sandwich structure does not disappear at the range of <jats:inline-formula>
<jats:tex-math>
<?CDATA $\dot{M}\lesssim 100{L}_{{\rm{Edd}}}/{c}^{2}$?>
</jats:tex-math>
<jats:inline-graphic xmlns:xlink="http://www.w3.org/1999/xlink" xlink:href="apjaa2778ieqn8.gif" xlink:type="simple" />
</jats:inline-formula>. Our simulations also reveal that the gas temperature in the overheated regions depends on black hole spin, which would be due to efficient energy transport from black hole to disks through the Poynting flux, resulting in gas heating.</jats:p>

• 出版日期2016-7-20