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Parabolic Jets from the Spinning Black Hole in M87

  • Authors: Masanori Nakamura, Keiichi Asada, Kazuhiro Hada, Hung-Yi Pu, Scott Noble, Chihyin Tseng, Kenji Toma, Motoki Kino, Hiroshi Nagai, Kazuya Takahashi, Juan-Carlos Algaba, Monica Orienti, Kazunori Akiyama, Akihiro Doi, Gabriele Giovannini, Marcello Giroletti, Mareki Honma, Shoko Koyama, Rocco Lico, Kotaro Niinuma, and Fumie Tazaki

2018 The Astrophysical Journal 868 146.

  • Provider: AAS Journals

Caption: Figure 7.

Final snapshot of the fiducial run (a = 0.9375); t/tg = 9000. The magnitude of the outgoing radial mass flux density ﹩\sqrt{-g}\rho {u}^{r}(\gt 0)﹩, where ur is the radial component of the four-velocity, ﹩\sqrt{-g}={\rm{\Sigma }}\sin \theta ﹩ is the metric determinant, and ﹩{\rm{\Sigma }}\equiv {r}^{2}+{a}^{2}{\cos }^{2}\theta ﹩, is shown with a color-filled contour (the upper computational domain; 0 ≤ θ ≤ π/2). Contours with navy solid lines show ﹩{u}^{r}=0﹩, while “whiteout” regions indicate the magnitude of the ingoing radial mass flux density ﹩\sqrt{-g}\rho {u}^{r}(\lt 0)﹩. The jet stagnation surface is clearly displayed inside the PFD funnel (﹩{u}^{r}=0﹩). −ut = 1 (Be ≈ 0) is shown with a magenta dashed line. Other components are identical to those in Figure 2.

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