Tag: Holes

One of the biggest challenges for modern astrophysics is to describe how the Universe went from a uniform place without planets, stars, or galaxies to the rich, structured, diverse cosmos we see today. Not just with a general story, mind you, but in gory detail, going not only as far back as we can ...

The mainstream used Newton’s formula (and its variations from Einstein and Schwarzschild) for gravitational acceleration a = G×M/R², circular velocity v = sqrt(G×M/R), and escape velocity ev = sqrt(2G×M/R), to say that for a massive and dense ste...

One of the biggest challenges for modern astrophysics is to describe how the Universe went from a uniform place without planets, stars, or galaxies to the rich, structured, diverse cosmos we see today. Not just with a general story, mind you, but in gory detail, going not only as far back as we can ...

Black holes are wondrous objects, but how many are out there? Made famous by the movie Interstellar, this depiction of a black hole seen edge-on with respect to its accretion disk in a highly-curved spacetime shows the substantial spacetime-bending power of a black hole. Close to the event ho...

Just like humans, black holes come in singles and pairs. And when a third black hole joins an existing pair, the three-body dynamics is often chaotic. Again, just as in human relationships. Most galaxies host a supermassive black hole at their center. This is the case for our Milky-Way galaxy and...

One of the biggest challenges for modern astrophysics is to describe how the Universe went from a uniform place without planets, stars, or galaxies to the rich, structured, diverse cosmos we see today. Not just with a general story, mind you, but in gory detail, going not only as far back as we can ...

The mainstream used Newton’s formula (and its variations from Einstein and Schwarzschild) for gravitational acceleration a = G×M/R², circular velocity v = sqrt(G×M/R), and escape velocity ev = sqrt(2G×M/R), to say that for a massive and dense ste...

When we go from R=4/3×G×M/c² in the left direction to R=0, the period of rotation significantly increases up to infinity, meaning the core of the Black Hole stops. Then friction inside the Black Hole will slow down and eventually stop the whole Black Hole. It turns ou...

Today, even the most massive of the known black holes represent only about 0.1% of the stellar mass of the galaxy: just one-thousandth of the amount of mass found by summing up all the stars in the galactic environment surrounding it. For a long time, astronomers have wondered just how these superma...