#5–7: the Small Magellanic Cloud, NGC 3190 and NGC 6822. All between 0.1% and 0.6% of the Milky Way’s mass (it’s uncertain which one is largest), these three are substantial galaxies in their own right as well, with over a billion solar masses’ worth of material in each one.

Image credit: Kanál uživatele nastebni, still from video at https://www.youtube.com/watch?v=k99VdKmAVJU.

#8 & 9: Elliptical galaxies M32 and M110. These might “only” be satellites of Andromeda, but these ellipticals have over a billion stars inside each, and may yet be more massive than some of the galaxies numbered 5, 6 and 7 above.

And beyond that, there are at least 45 other known galaxies — smaller galaxies — making up our local group.

Despite their sheer numbers, their masses and their magnitudes, not one of them will exist the way they are right now another few billion years into the future.

Image credit: A. Gai-Yam / Weizmann Inst. of Science / ESA / NASA.

As time goes on, galaxies gravitationally interact. This not only pulls them together by the gravitational attraction you picture normally, but there are also tidal interactions. We normally think about tides as something the Moon creates by pulling on the Earth’s oceans, causing a bulge in one direction that gives us “high tide” when the Earth rotates through the bulge and “low tide” when we rotate through the trough, which is true enough.

But from a galaxy’s point of view, tides are a little more subtle. The portion of a small galaxy that’s closer to a larger one will be attracted with a greater gravitational force, while the portion that’s farther away will experience a lesser attractive force. As a result, small galaxies get stretched and eventually torn apart by their interactions with larger ones.

Illustration credit: Katherine Johnston, via https://www.ing.iac.es/PR/newsletter/news5/science1.html.

The small galaxies that are a part of our local group, including both Magellanic clouds and all the dwarf ellipticals, will be torn apart in exactly this fashion, and their matter will be incorporated into the larger galaxies they merge with.

“So what,” you say. That’s not a true death, because the big, Milky Way-like galaxies still survive. But even we won’t live forever in our current state. About 4 billion years in the future, the mutual gravitational attraction of the Milky Way and Andromeda will pull us into a gravitational dance with one another, leading to a major merger. Although the entire process will take billions of years to complete, the spiral structure of both galaxies will be destroyed, resulting in the creation of a single, giant elliptical galaxy at the core of our local group: Milkdromeda.

Eventually, the other galaxies within our local group will be sucked in as well, leaving just a single, giant galaxy made up of the cannibalized remains of all the others. This process will happen, eventually, in all the bound groups and clusters of galaxies throughout the Universe, while dark energy drives all the individual groups and clusters apart from one another.

But again, that’s not a true death, because there’s still a galaxy present. At least, for the time being, that’s the truth. But the galaxy is made up of stars, gas and dust, and there’s a finite amount of all of them.

Image credit: NASA, ESA, and The Hubble Heritage Team (STScI/AURA).

While the mergers will take tens of billions of years to complete, and dark energy will drive them apart and across the Universe towards invisibility and inaccessibility on timescales of hundreds of billions of years, the stars within will live on. The longest-lived stars in existence today will continue to burn their fuel for more than ten trillion years, and from the gas, dust and stellar corpses littering each galaxy, new stars will be born — albeit in smaller and smaller numbers and less frequently — throughout that time.

Image credit: the small star forming region NGC 346, from A. Nota (ESA/STScI) et al., ESA, NASA.

Even when the last star burns out, the stellar remnants — white dwarfs and neutron stars — will continue to shine for hundreds of trillions or even quadrillions of years before going dark. When that inevitability happens, we’ll still have brown dwarfs, or failed stars, merging together occasionally, reigniting nuclear fusion and creating starlight for tens of trillions of years at a time.

Image credit: NASA/JPL/Gemini Observatory/AURA/NSF. These are the two brown dwarfs that make up Luhman 16, and they will eventually merge together to create a star.

When that last star burns out, though, tens of quadrillions of years (some ~10^16 of them) in the future, the mass in the galaxy will still be present. Even that cannot be considered a “true death” in some senses.

Image credit: J. Walsh and Z. Levay, ESA/NASA.

Even without light, the galaxy itself will not last forever! All of these masses are gravitationally interacting with one another, and gravitational objects of different masses have a strange property when they interact:

The repeated “passes” and close encounters cause exchanges of velocity and momentum between them.

The lower-mass objects get kicked out of the galaxy, while the higher-mass objects sink towards the center, losing velocity in a process known as violent relaxation.

Over long enough timescales (~10^19 to 10^20 years), most of the mass of the galaxy will have been ejected, with only a small percentage of the remaining masses more tightly bound.

Image credit: ESA (Image by C. Carreau).

At the very center of this galactic remnant will be the supermassive black hole at the center of each one. This will, of course, be the last and final thing to go: it will get as large as it can from eating as many objects as it can get its hands on. At the center of Milkdromeda, we’ll likely find an object a hundred million times as massive as our Sun is today; larger groups and clusters might have black holes exceeding ten billion solar masses or even higher!

Yet even these won’t live forever.

Image credit: the EU’s Communicate Science, via http://www.communicatescience.eu/2010/11/black-hole-radiation-simulated-in-lab.html.

Thanks to the phenomenon of Hawking radiation, even these objects will decay away. It will take somewhere between 10^80 and 10^100 years, depending on how massive our supermassive black hole gets, but even this, too, will go away.

No matter how you define a galaxy or its remnants, all of them will most certainly die. As to when and how, the exact answer is up to you!