Lỗ đen sao

Một lỗ đen sao (hay lỗ đen khối lượng sao) là một lỗ đen hình thành bởi sự suy sụp hấp dẫn của một ngôi sao khối lượng lớn.[1] Chúng có khối lượng trải dài từ 5 đến vài chục lần khối lượng Mặt Trời.[2]

Ứng cử viên

Hầu hết các ứng cử viên đều là hệ sao đôi.

Tên Khối lượng lỗ đen
(lần khối lượng mặt trời)		 Khối lượng Đồng hành
(lần khối lượng mặt trời)		 Chu kỳ quỹ đạo (ngày) Khoảng cách từ Trái Đất (năm ánh sáng) Vị trí[3]
A0620-00/V616 Mon 11 ± 2 2.6–2.8 0.33 khoảng 3500 06:22:44 -00:20:45
GRO J1655-40/V1033 Sco 6.3 ± 0.3 2.6–2.8 2.8 5000−11000 16:54:00 -39:50:45
XTE J1118+480/KV UMa 6.8 ± 0.4 6−6.5 0.17 6200 11:18:11 +48:02:13
Cyg X-1 11 ± 2 ≥18 5.6 6000–8000 19:58:22 +35:12:06
GRO J0422+32/V518 Per 4 ± 1 1.1 0.21 khoảng 8500 04:21:43 +32:54:27
GRO J1719-24 ≥4.9 ~1.6 có thể 0.6[4] khoảng 8500 17:19:37 -25:01:03
GS 2000+25/QZ Vul 7.5 ± 0.3 4.9–5.1 0.35 khoảng 8800 20:02:50 +25:14:11
V404 Cyg 12 ± 2 6.0 6.5 7800±460[5] 20:24:04 +33:52:03
GX 339-4/V821 Ara 5–6 1.75 khoảng 15000 17:02:50 -48:47:23
GRS 1124-683/GU Mus 7.0 ± 0.6 0.43 khoảng 17000 11:26:27 -68:40:32
XTE J1550-564/V381 Nor 9.6 ± 1.2 6.0–7.5 1.5 khoảng 17000 15:50:59 -56:28:36
4U 1543-475/IL Lupi 9.4 ± 1.0 0.25 1.1 khoảng 24000 15:47:09 -47:40:10
XTE J1819-254/V4641 Sgr 7.1 ± 0.3 5–8 2.82 24000 – 40000[6] 18:19:22 -25:24:25
GRS 1915+105/V1487 Aql 14 ± 4.0 ~1 33.5 khoảng 40000 19:15;12 +10:56:44
XTE J1650-500 9.7 ± 1.6 [7] . 0.32[8] 16:50:01 -49:57:45
GW150914 (62 ± 4) M☉ 36 ± 4 29 ± 4 . 1.3 tỉ
GW151226 (21.8 ± 3.5) M☉ 14.2 ± 6 7.5 ± 2.3 . 2.9 tỉ
GW170104 (48.7 ± 5) M☉ 31.2 ± 7 19.4 ± 6 . 1.4 tỉ

Tham khảo

  1. ^ Celotti, A.; Miller, J.C.; Sciama, D.W. (1999). “Astrophysical evidence for the existence of black holes”. Classical and Quantum Gravity. 16 (12A): A3–A21. arXiv:astro-ph/9912186. doi:10.1088/0264-9381/16/12A/301.
  2. ^ Hughes, Scott A. (2005). "Trust but verify: The case for astrophysical black holes". arΧiv:hep-ph/0511217 [hep-ph]. 
  3. ^ Định vị theo ICRS lấy từ SIMBAD. Định dạng: xích kinh (hh:mm:ss) ±xích vĩ (dd:mm:ss).
  4. ^ Masetti, N.; Bianchini, A.; Bonibaker, J.; della Valle, M.; Vio, R. (1996), “The superhump phenomenon in GRS 1716-249 (=X-Ray Nova Ophiuchi 1993)”, Astronomy and Astrophysics, 314
  5. ^ Miller-Jones, J. A. C.; Jonker; Dhawan. “The first accurate parallax distance to a black hole”. The Astrophysical Journal Letters. 706 (2): L230. arXiv:0910.5253. Bibcode:2009ApJ...706L.230M. doi:10.1088/0004-637X/706/2/L230.
  6. ^ Orosz et al. A Black Hole in the Superluminal source SAX J1819.3-2525 (V4641 Sgr) Preprint
  7. ^ “Scientists Discovered the Smallest Black Hole” (PDF).
  8. ^ Orosz, J.A. et al. (2004) ApJ 616,376–382.[1], Volume 616, Issue 1, pp. 376–382.

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