This Is Why Venus Is The Brightest, Most Extreme Planet We Can See

And why, even at its faintest, it always outshines every other star and planet.

If you’ve been looking to the west after sunset recently, you may have noticed that there’s one point of light that outshines all the others not only around it, but across the entire night sky. That point is the planet Venus, a planet so bright and luminous that it outshines all other objects in the night sky except for the Moon. Every other star and planet pales in comparison to Venus as viewed from Earth, and that’s irrespective of whether Venus is at its closest to or farthest from Earth in its orbit.

Seen next to Mars — a bright planet in its own right — as it appeared during conjunction on July 12, 2021, Venus appeared about 200 times brighter than Mars, or almost six full astronomical magnitudes: equal to the brightness difference between the North Star and the planet Neptune. Although its continued brightness is perhaps Venus’s most notable feature, it isn’t just the brightest planet we can see from Earth, but rather an extreme, remarkable planet in a number of ways. Here’s what gives Venus its remarkable, unique status within the Solar System.

Venus’s cloud-rich atmosphere lies high above a dense, thick, extremely hot surface layer. The lower cloud decks don’t begin until you’re already tens of kilometers up, and persist in multiple layers until the highest hazes at ~90 kilometers in altitude. These clouds, composed largely of sulfuric acid, are perhaps the most striking feature of Venus’s atmosphere. (LIMAYE ET AL, DOI: 10.1089/AST.2017.1783)

1.) Venus’s atmosphere. Every planet within the Solar System is subject to a few different effects: the gravitational pull from the mass within the planet on one hand, and the particles and radiation emitted from the Sun on the other hand. These two phenomena oppose one another when it comes to the planet’s atmospheres, with the solar wind and radiation working to strip the planet’s atmosphere away while the gravitational pull of the planet works to grow the planet during the early, formative stages and hang onto as much of its atmosphere for as long as possible later on.

Although Mercury was close enough to the Sun and small enough that its atmosphere was fully stripped away long ago, Venus was more distant and more massive, and managed to hold onto its more massive molecular species, particularly its carbon dioxide. It’s speculated that a runaway greenhouse effect took place on Venus long ago, leading to its dense, thick, hot atmosphere, dominated by carbon dioxide and sulfuric acid clouds.

The upper layers of Venus’s atmosphere become ionized due to solar radiation, and this ionized layer, and the magnetic field resulting from the motion of the charged particles within it, protects the rest of Venus from the Sun’s stripping effects: similar to how Earth’s magnetic field protects our own planet’s atmosphere. This protection doesn’t cover everything, however; lighter species of gases — including water vapor — are constantly stripped away by the solar wind, and seen in Venus’s magnetotail.

An infrared view of Venus’ night side, by the Akatsuki spacecraft. Its brightness is greater than that of any other planet as seen from Earth, and it approaches our world closer than any other planet does. At its nearest, it appears the largest in the sky of all the planets; at its most distant, numerous other planets can appear larger. However, Venus is always the brightest. (ISAS, JAXA)

2.) Venus’s clouds. The multiple thick layers of sulfuric acid clouds play a tremendous role in pushing Venus to its extremes. Whereas on Earth, it’s primarily the greenhouse gases in our atmosphere that warm our planet — gases like water vapor, carbon dioxide, and methane, which are transparent at optical wavelengths but absorb and re-emit light in the infrared — Venus’s clouds are the primary heat-trapping agent on our sister planet. On Earth, clouds only account for about 25% of the trapped heat on our planet; on Venus, it’s well over 90%.

Additionally, the clouds on both Earth and Venus are highly reflective, but Earth is only ever partially covered in clouds, and many of Earth’s clouds are thin, high cirrus clouds that reflect only ~10% of the incoming sunlight, as opposed to the thick, low stratocumulus clouds that can reflect more like ~90% of the light. Venus, by contrast, has multiple layers of cloud-decks spanning something like 20 kilometers in altitude, such that 0% of the surface is visible at any time from space, as opposed to more like ~50% for planet Earth. This cloud cover winds up playing a vital role in the brightness of Venus as seen from Earth as well.

The Soviet Union’s series of Venera landers are the only spacecraft to ever land and transmit data from the surface of Venus. The longest-lived of all the landers exceeded the two-hour mark before the instruments overheated and contact was lost. To date, no spacecraft has survived for longer on the Venusian surface, where temperatures reach 900 degrees Fahrenheit (482 C). (VENERA LANDERS / USSR)

3.) Venus’s temperature. Although Venus is nearly twice the distance from the Sun as Mercury and receives only about 29% of the radiation-per-unit-area that Mercury receives, Venus, not Mercury, is the Solar System’s hottest planet. Whereas Mercury, a practically airless world, can get up to 427 °C (800 °F) in full Sun while its night side can plummet to as low as -180 °C (-290 °F), Venus consistently remains between 440–480 °C (820–900 °F): always hotter than Mercury at its absolute hottest.

While Earth’s greenhouse effect only increases our planet’s temperature by about 33 °C (59 °F), Venus’s is tremendous, increasing its temperature by about 450 °C (810 °F) over the scenario where it’s a completely airless world. Down at the surface of Venus, it’s always hot enough to melt lead; our most long-lived landers operated for fewer than 3 hours upon touching down on the surface. While the surface of Venus might be the most hellish place in our Solar System — in many ways even more extreme than the volcanic surface of Jupiter’s moon Io — about ~60 kilometers up, it’s surprisingly Earth-like. With similar pressures and temperatures to those found at Earth’s surface, Venus, up above its cloud-tops, might already be home to simple but hardy microbial life forms.

The seven extraterrestrial planets of the solar system: Mercury, Venus, Mars, Jupiter, Saturn, Uranus, and Neptune, with sizes accurate to what’s visible from Earth, but with brightnesses adjusted. Saturn is many times fainter than Jupiter, despite being almost the same size and nearly the same reflectivity: a function of its much greater distance both from the Sun and from Earth. Venus, meanwhile, is 63,000 times brighter than the faintest planet, Neptune. (GETTY IMAGES)

4.) Venus’s reflectivity. This is where things start to get interesting. Every object in the Solar System has what’s known as an albedo: a measure of how reflective its surface is. There are two types of albedo that scientists talk about:

Bond albedo, which is the ratio of the total reflected radiation compared to the total incoming (solar) radiation, and

Geometric albedo, which is how much light actually gets reflected compared to a flat, ideally reflective surface.

By both measures, Venus is by far the most reflective planet in the Solar System, with albedos that are each more than double the next closest planet. Whereas airless worlds like Mercury or the Moon reflect only about 11–14% of the total incoming light, similar to what Earth would reflect if it were airless and free of icecaps, Venus reflects between 75–84% of the total light, dependent upon how it’s measured. This high level of reflectivity makes it appear intrinsically brighter than any other planet in the Solar System, with only a few ice-rich moons, like Saturn’s Enceladus, possessing a higher total albedo.

The phases of Venus, as viewed from Earth, can enable us to understand how Venus always appears from the perspective of Earth. Reaching a maximum elongation of 47 degrees away from the Sun, Venus is at its largest and brightest in the thin crescent phase, but when it’s more distant and smaller, it’s fuller, remaining the brightest object, other than the Moon, in Earth’s night sky. (WIKIMEDIA COMMONS USERS NICHALP AND SAGREDO)

5.) Venus’s appearance from Earth. There are a few different reasons, combined, for why Venus is always the brightest planet in Earth’s night sky. One is that Venus is relatively large (almost the same size as Earth) for a rocky planet as well as relatively close to the Sun; in terms of the total amount of solar radiation incident on its surface, only Jupiter receives more. Two is that Venus is the most reflective planet in the Solar System; the highest percentage of the incoming solar radiation is cast off back into space.

But three is Venus’s proximity to Earth. At its closest, Venus comes within 41 million km (25 million miles) of Earth, closer than any other planet. Even at its most distant, Venus is only 261 million km (162 million miles) from Earth: far closer than Jupiter ever gets to Earth. (The next closest approach of Jupiter to Earth will come in 2022, when it comes within 591 million km, or 367 million miles.)

Even though Venus exhibits the full suite of phases, its crescent phase near closest approach to Earth is when it’s at its brightest, but it’s only slightly fainter when it’s farthest away as it enters its full phase. Even at their brightest, the other bright planets — Jupiter and Mars — can’t compete with Venus, even when at its faintest.

The orbits of the planets in the inner solar system aren’t exactly circular, but they’re quite close, with Mercury and Mars having the biggest departures and the greatest ellipticities. The effects of the planets on Mercury’s precession, dominated by Venus, then Jupiter, and then Earth, cannot account for all of the observed precession, pointing the finger towards General Relativity. (NASA / JPL)

6.) Venus’s role in General Relativity. The first hint we had that something was “wrong” with Newtonian gravity within our Solar System came in the mid-19th century, by observing the orbit of Mercury. Over the past few centuries, we’d been observing Mercury in its elliptical orbit around the Sun, and we saw its perihelion — or its point of closest approach to the Sun — advance in its orbit. The total rate that the perihelion advanced by was 5600 arc-seconds per century, and that rate was a little bit too much for Newtonian gravity.

5025 of those arc-seconds per century was due to the precession of the equinoxes: an effect of Earth’s precessing orbit. The next key in understanding the problem was to calculate the effects of all the other planets on the orbit of Mercury. Although each planet makes a contribution, for a total of ~532 arc-seconds per century, the greatest contribution came from Venus: 277 arc-seconds per century, nearly double that of the next-largest contributor, Jupiter (at ~150), and more than triple the contribution of Earth (at ~90).

The “missing” 43 arc-seconds per century was precisely what Einstein’s General Relativity was able to account for, but without quantifying the contributions from other planets so precisely, particularly from Venus, understanding the role that General Relativity played would have been impossible.

When Mercury (upper) first begins transiting across the Sun, there is no hint of an atmospheric ‘arc’ that would reveal the presence of sunlight filtering through its atmosphere. By contrast, Venus’ atmosphere (lower) displays a clearly defined arc during transits, and did as far back as the 18th century, (NASA/TRACE (TOP); JAXA/NASA/HINODE (BOTTOM))

7.) Venus and the birth of transit spectroscopy. Being the second planet from our Sun, Venus is one of two planets (along with Mercury) that’s observed to transit in front of the Sun’s disk from our perspective here on Earth. Unlike transits of Mercury, however, where Mercury simply appears as an opaque disk silhouetted against the Sun, sunlight appears to “curve” around the edge of Venus as the transit both begins and ends. Observations of transits of Venus, which only occur twice per century, on average, were humanity’s first indication that Venus possessed — whereas Mercury lacked — a substantial atmosphere.

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But we can do so much more than just detect the existence of an atmosphere during transits: we can actually measure what its atmospheric contents are, molecule-by-molecule. First demonstrated during the 2004 transit of Venus, this technique is now a vital part of exoplanet sciences as we attempt to use transit spectroscopy to discern the atmospheric constitutents of planets around other stars. Although, in principle, this was a possibility long before, it’s only here in the 21st century that instrumentation technology has caught up to our scientific dreams.

This infographic displays some illustrations and planetary parameters of the seven planets orbiting TRAPPIST-1. They are shown alongside the rocky planets in our Solar System for comparison. These seven known worlds only go out to approximately the orbit of Venus; it is possible and perhaps even likely that many more worlds exist beyond the outermost one yet discovered. Which worlds are Mercury-like, Venus-like, Earth-like, or Mars-like have not yet been determined. (NASA)

8.) Venus’s lessons for exoplanets. Today, we look at Venus and we see it as it is now: hot, bright, and shrouded in a thick, dense, heavy-element-rich atmosphere. But it provides us with one of the four main potential fates for a rocky planet interior to a star’s frost line.

Get too close to your parent star, and you’ll become tidally locked and/or have your entire atmosphere stripped away, like Mercury on both counts.
Get too far from your parent star, especially if you’re too small, and you’ll become cold, frozen, and inhospitable to life, like Mars.
If things work out just right in terms of your atmosphere, your size, and your distance from the Sun, you might have liquid water on your surface and a sustained, long-term shot at life.
But you could still possess a thin atmosphere, avoid tidal locking, and transition from a world with Earth-like potential to becoming a Venus-like hellhole: if your planet experiences a runaway greenhouse effect.

If things had gone differently on Venus, perhaps it, too, could have become a world with a wet, life-rich, self-sustaining biosphere over the long term. Perhaps, in the distant past, things once were very different on Venus, and perhaps there’s a rich history of ancient, early life on that planet. When we’re considering what could be out there on planets beyond our own Solar System, we need to look not just for “other Earths” that may be out there, but for other Venuses as well, as well as any evolutionary steps that it may have underwent along the way.

Earth, at left, and Venus, as seen in infrared at right, have nearly identical radii, with Venus being approximately ~90–95% the physical size of Earth. However, due to its close proximity to the Sun, Venus suffered a tremendously different fate earlier on. It’s possible that, about a billion years from now, Earth will finally follow suit. (ARIE WILSON PASSWATERS/RICE UNIVERSITY)

All told, Venus is a planet full of extremes. It possesses the thickest atmosphere of any rocky, terrestrial world known. It achieves the hottest surface temperatures of any planet in the Solar System. It’s the most reflective planet in the Solar System, outclassing even the gas giants. And — of particular interest to observers on Earth — it’s always the brightest point of light visible in the night sky. Whenever it’s not directly behind the Sun, either in the post-sunset or the pre-dawn skies, no other star or planet ever outshines it.

So, with everything we now know, why is it that Venus is the brightest planet in the Solar System?

It’s due to the combination of its large, Earth-like surface area, its relatively close proximity to the Sun, its very reflective, cloud-rich atmosphere, and the fact that even at its most distant, it’s never more than about 1.75 astronomical units from planet Earth. Even when Jupiter and Mars, the next brightest planets, are at their absolute brightest, they still can’t compete with Venus at its faintest. The next time you look up and see an unparalleled bright point of light fixed in the post-sunset or pre-dawn skies, you’ll know precisely why Venus, compared to all the other stars and planets visible from Earth, always appears to outshine them all.

Starts With A Bang is written by Ethan Siegel, Ph.D., author of Beyond The Galaxy, and Treknology: The Science of Star Trek from Tricorders to Warp Drive.