Here on Earth, the ingredients for life to survive, thrive, evolve, and sustain itself on our world have all coexisted without fail for billions of years. In addition to all the atoms and molecules our planet possesses, our world also has the right conditions for liquid water on its surface, owing to our atmosphere and being at just the right distance from our Sun.
Yet if the Sun were either significantly cooler or hotter, that habitability would come to an abrupt end. All the ingredients we could conceive of wouldn't change the simple fact: without the right energy input from our Sun, life would be an impossibility. Our Sun contains 99.8% of the Solar System's mass, but gets lighter every day. When enough time goes by, its changes will render Earth uninhabitable. Here's how it's changing.
When our Solar System first formed, a large clump of mass began gravitationally attracting more and more matter to it, forming a growing proto-star. Surrounding it, a protoplanetary disk formed, complete with the seeds of the Solar System's future planets. A race then ensued between two competing forces: gravitation, working to grow our proto-star and the planets within the disk, and radiation from external stars and our young, forming Sun.
Artist's impression of a young star surrounded by a protoplanetary disk. There are many unknown properties about protoplanetary disks around Sun-like stars, but the general picture of a dusty disk with heavy elements distributed through it is certainly what gave rise to our planets.ESO/L. CALÇADA
When radiation finally wins out, our Sun and the planets can no longer grow, and the matter that would continue to fall in gets blown away, eventually giving rise to our modern Solar System. This marks the point where our Solar System reaches peak mass: the most massive it will ever be. This also marks, not so coincidentally, the point where our Sun is at its least energetic.
As long as it fuses lighter elements into heavier ones, it will never give off so little energy again. Doesn't this seem paradoxical? The Sun, from this point on, will only get less massive, while the amount of energy it emits will only go up. If this flies in the face of what you think we know about stars, you're not alone. After all, more massive stars do burn hotter and brighter, all things being equal.
Asteroids in the early Solar System were more numerous, and cratering was catastrophic. Once the protoplanetary disk and the surrounding proto-stellar material has evaporated away, the growth of the Solar System's overall mass ceases, and it can only decrease from that point on.
NASA / GSFC, BENNU’S JOURNEY - HEAVY BOMBARDMENT
There's really only a couple of factors, all in combination with one another, that determine how hot a star is. Given that stars get their power from the nuclear fusion of lighter elements into heavier ones, we can actually enumerate what causes a star to give off energy. The factors are:
1. The temperature at the core of the star, since higher temperatures mean more energy-per-particle, yielding a greater likelihood of a fusion event when two particles collide.
2. The size of the fusion region, since bigger regions where fusion can occur leads to more fusion in the same amount of time.
If we look at and compare two different stars, the more massive one tends to reach higher core temperatures and have a larger fusion region. But if we look inside any individual star, we see something else.
The (modern) Morgan–Keenan spectral classification system, with the temperature range of each star class shown above it, in kelvin. The overwhelming majority of stars today are M-class stars, with only 1 known O- or B-class star within 25 parsecs. Our Sun is a G-class star.
WIKIMEDIA COMMONS USER LUCASVB, ADDITIONS BY E. SIEGEL
The Sun, as it burns through its fuel, gains its energy by fusing hydrogen, in a chain reaction, into helium. The proton-proton chain is how our Sun (and most stars) get their energy, since the end product (helium-4) is lighter and lower in mass than the initial reactants (4 protons). Nuclear fusion works on the principle of mass-energy equivalence, where a small fraction of about 0.7% of the total mass of whatever gets fused is converted into energy via Einstein's E = mc2.
As this occurs, the mass of the Sun slowly drops; the energy gets transported to the surface, and the "waste product" of helium sinks further down into the central region of the core. The helium at the very center cannot fuse at these temperatures, so there's less fusion-per-unit-volume occurring in the helium-rich regions.
Without fusion, there's less radiation, and the helium-rich inner part starts to contract under its own gravity. But gravitational contraction gives off energy, meaning that there's a lot of heat/thermal energy getting transported outward. As the star ages, therefore, the interior temperatures increase, and the region where fusion can occur (at temperatures of 4 million K and up) expands outward.
This cutaway showcases the various regions of the surface and interior of the Sun, including the core, which is where nuclear fusion occurs. As time goes on, the helium-containing region in the core expands, causing the Sun's energy output to increase.WIKIMEDIA COMMONS USER KELVINSONG
Overall, the rate-of-fusion and the volume where fusion occurs increases over time. This results in the Sun — and all sun-like stars — increasing its energy output as it ages. At the same time, the energy that gets transported to the surface not only causes the emission of light, but some of the loosely-held particles at the limb of the Sun's photosphere.
Electrons, protons, and even heavier nuclei can gain enough kinetic energy to be ejected from the Sun, creating a stream of particles known as the solar wind. The charged particles spread throughout the Solar System and overwhelmingly leave the Solar System entirely, although a few of them will, by a chance alignment in geometry, wind up striking the atmospheres of one of the planets.
The evolution of the Sun's luminosity (red line) over time. The big increase is due to the core temperature and the volume where fusion occurs increasing as the Sun burns through its fuel.
WIKIMEDIA COMMONS USER RJHALL, BASED ON RIBAS, IGNASI (FEBRUARY 2010) SOLAR AND STELLAR VARIABILITY: IMPACT ON EARTH AND PLANETS, PROCEEDINGS OF THE INTERNATIONAL ASTRONOMICAL UNION, IAU SYMPOSIUM, VOLUME 264, PP. 3-18
When they do, they create the effect known as an aurora, which humanity has measured and observed throughout history. Over the past 4.5 billion years, the Sun has gotten hotter, but also less massive. The solar wind, as we measure it today, is roughly constant over time. There are the occasional flares and mass ejections, but they barely factor into the Sun's overall rate at which it loses mass.
This is a false-color image of ultraviolet Aurora Australis captured by NASA's IMAGE satellite and overlaid onto NASA's satellite-based Blue Marble image. The Earth is shown in false color; the aurora image, however, is absolutely real.NASA
Similarly, the Sun's fusion energy output has increased by about 20% over the course of its history, but this, too, is a small factor. If we measure the rate of mass loss today, due to both the solar wind and to nuclear fusion, we can figure out how much lighter the Sun is getting with each second that goes by. We can also extrapolate how much mass the Sun has lost over its entire history since it was born: a remarkable feat.
The solar wind carries away about 1.6 million tonnes of mass every second, or 1.6 × 109 kg/s. That's a lot of material, for sure, and it adds up over long periods of time. Every 150 million years, the Sun loses roughly the mass of Earth due to the solar wind, or about 30 Earth masses over the entire lifetime of the Sun so far.
A solar flare from our Sun, which ejects matter out away from our parent star and into the Solar System, is dwarfed in terms of 'mass loss' by nuclear fusion, which has reduced the Sun's mass by a total of 0.03% of its starting value: a loss equivalent to the mass of Saturn. Until we discovered nuclear fusion, however, we could not accurately estimate the Sun's age.
NASA’S SOLAR DYNAMICS OBSERVATORY / GSFC
From fusion, however, the Sun loses even more mass than that. The Sun's power output is a relatively consistent 4 × 1026 W, which means it converts approximately 4 million tonnes of mass into energy each second. From fusion, then, the Sun loses about 250% as much mass, each second, as gets carried away from the solar wind.
Over the course of its 4.5 billion year lifetime, the Sun has lost about 95 Earth masses due to fusion: approximately the mass of Saturn. As time goes on, the amount of mass lost by the Sun will increase, particularly as it enters the giant phase of its life. But even at this relatively steady rate, the growth of helium in the Sun's core means that we will heat up here on planet Earth.
The Sun, shown here, generates its energy by fusing hydrogen into helium in its core, losing small amounts of mass in the process. Over its lifetime, it's lost approximately the mass of Saturn by this process: about 2.5 times as much mass as it's lost due to the solar wind.
NASA / SOLAR DYNAMICS OBSERVATORY (SDO)
After about 1-to-2 billion years, the Sun will be burning hot enough that Earth's oceans will boil away entirely, making liquid water impossible on the surface of our planet. As the Sun gets lighter and lighter, it will counterintuitively get hotter and hotter. Our planet has already used up approximately three-quarters of the time we have where Earth is habitable. As the Sun continues to lose mass, humanity and all life on Earth approaches its inevitable fate. Let's make these last billion-or-so years count.