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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 11.

Color-filled contour of the magnitude of the outgoing radial mass flux density (similar to Figure 7) for four different runs with different BH spins (from left to right: a = 0.5, 0.7, 0.9, and 0.99). The final snapshot (t/tg = 12,000) is displayed for each run with the whole computational domain r/rg ≤ 100 and 0 ≤ θ ≤ π. The navy solid line shows ﹩{u}^{r}=0﹩, while “whiteout” regions indicate the magnitude of the ingoing radial mass flux density. The jet stagnation is clearly displayed inside the PFD funnel (﹩{u}^{r}=0﹩), and it shifts toward the BH when a increases. −ut = 1 (Be ≈ 0) is shown with a magenta dashed line. Other components in the panels are identical to those in Figure 8.

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