항성질량 블랙홀

3. X선 관측

쌍성계에서의 항성 블랙홀은 동반성의 물질이 블랙홀로 이동할 때 관측 가능하다. 밀집성이 되면서 방출되는 에너지는 물질의 온도를 수억 도까지 올리고 X선을 방출시킬 만큼 매우 크다. 그러므로 블랙홀은 X선으로 관측할 수 있다. 반면에 동반성은 광학 망원경으로 관측 가능하다. 블랙홀과 중성자별에서 방출된 에너지는 등급이 같다. 그래서 블랙홀과 중성자성은 종종 구분하기가 어렵다.^[62][63][64]

밀집된 X선 소스의 관측으로부터 질량을 유도한다. (X선 및 광학 데이터 결합) 확인된 모든 중성자성은 300만원 미만의 질량을 가지고 있으며, 300만원 이상의 질량을 갖는 밀집 체계가 없는 것은 중성자성의 성질이다. 이러한 요소들의 결합은 300만원 이상 되는 질량을 갖는 밀집성이 사실은 블랙홀이라는 것을 알려준다.^[62][63][64]

우리 은하에는 우리 은하 중심에 있는 초대질량 블랙홀보다는 우리에게 더 친숙한 수 개의 블랙홀 후보를 갖고 있다. 이들 후보들은 모두 밀집된 물체가 동반성의 강착원반을 통해 물질을 빨아들이는 X선 쌍성계이다. 이들 한 쌍에서 있음직한 블랙홀은 300만원에서 1200만원 이상까지 있을 수 있다.^[50][51][52]

6. 1. 우리 은하

6. 2. 은하 외부

X선 쌍성에서 나온 은하 외부의 후보는 다음과 같다.

NGC 6946에서 초신성 폭발 실패 이후 N6946-BH1의 소멸로 블랙홀이 형성되었을 수 있다.^[49]

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