Over the years, astronomers have become increasingly better at studying stars and determining their estimated ages.

This is done by looking at their size, brightness, and a number of other factors that change over millions of years as the star burns through its fuel source.

It was therefore surprising that when scientists studied the stars near the center of the Milky Way, they found that they appeared to be relatively young.

That’s nonsense, because experts know the environments where new stars are formed, and it’s not found in that part of space.

A group of scientists from Stanford and Stockholm University recently published a paper offering an explanation for why some stars in this region appear so young.

The paper explains that a computer model has determined that it is possible for the stars to remain ‘forever young’. This is because they are accreting large amounts of dark matter, which is believed to be located near the black hole at the centre of the Milky Way.

Of course, this is just a theory, which assumes that dark matter is real and that this has not yet been proven.

However, the mathematics seems to indicate that these stars can remain in a fairly constant state, without the normal signs of aging that scientists would expect.

At least that is the conclusion of the newspaper.

It is important to note that this article has not yet been peer reviewed. It will undoubtedly be reviewed by other scientists in the coming years.

Not surprisingly, there are also scientists who propose other explanations for why the stars appear so young.

One theory is that the stars are actually so young that they could develop in a region where new stars could grow as they were pulled toward the massive black hole.

Whatever the outcome, it is fascinating to discover that there are unusually young stars at the center of our galaxy.

Even though they still seem young.

If you found that interesting, you might also want to read about a second giant hole that has opened up on the surface of the sun. Here’s what it means.