On Mars, the sky is pink during the day, shading to blue at sunset. What planet did you think I was talking about?
On Earth, the sky is blue during daytime, turning red at as the sun sinks toward night.
Well, it’s not quite as simple as that: if you ignore your dear sainted mother’s warning and look at the Sun, you’ll see that the sky immediately around the Sun is white, and the sky right at the horizon (if you live in a place where you can get an unobstructed view) is much paler. In between the Sun and the horizon, the sky gradually changes hue, as well as varying through the day. That’s a good clue to help us answer the question every child has asked: why is the sky blue? Or as a Martian child might ask: why is the sky pink? First of all, light isn’t being absorbed. If you wear a blue shirt, that means the dye in the cotton (or whatever it’s made of) absorbs other colors in light, so only blue is reflected back to your eye. That’s not what’s happening in the air! Instead, light is being bounced off air molecules, a process known as scattering. Air on Earth is about 80% nitrogen, with almost all of the rest being oxygen, so those are the main molecules for us to think about. As I discussed in my earlier article on fluorescent lights, atoms and molecules can only absorb light of certain colors, based on the laws of quantum mechanics. While oxygen and nitrogen do absorb some of the colors in sunlight, they turn right around and re-emit that light. (I’m oversimplifying slightly, but the main thing is that photons aren’t lost to the world!) However, other colors don’t just pass through atoms as though they aren’t there: they can still interact, and the way we determine how that happens is again the color. The color of light is determined by its wavelength: how far a wave travels before it repeats itself. Wavelength is also connected to energy: short wavelengths (blue and violet light) have high energy, while long wavelengths (red light) have lower energy. When a photon (a particle of light) hits a nitrogen or oxygen molecule, it might hit one of the electrons inside the molecule. Unless the wavelength is exactly right, the photon doesn’t get absorbed and the electron doesn’t move, so all the photon can do is bounce off, like a pool ball off the rail on a billiards table. Low-energy red photons don’t change direction much after bouncing–they hit the electron too gently for that. Higher-energy blue and violet photons, on the other hand, scatter by quite a bit: they end up moving in a very different direction after hitting an electron than they moving before. This whole process is known technically as Rayleigh scattering, for the physicist John Strutt, Lord Rayleigh.
The blue color of the sky
Not every photon will hit a molecule as it passes through the atmosphere, and light from the Sun contains all the colors mixed together into white light. That means if you look directly at the Sun or the sky right around the Sun during broad daylight, what you see is mostly unscattered light, the photons that pass through the air unmolested, making both Sun and sky look white. (By the way, your body is pretty good at making sure you won’t damage your vision: your reflexes will usually twitch your eyes away before any injury happens. I still don’t recommend looking at the Sun directly for any length of time, especially with sunglasses, which can fool your reflexes into thinking everything is safer than it really is.) In other parts of the sky away from the Sun, scattering is going to be more significant. The Sun is a long way away, so unlike a light bulb in a house, the light we get from it comes in parallel beams. If you look at a part of the sky away from the Sun, in other words, you’re seeing scattered light! Red light doesn’t get scattered much, so not much of that comes to you, but blue light does, meaning the sky appears blue to our eyes. Bingo! Since there is some green and other colors mixed in as well, the apparent color of the sky is more a blue-white than a pure blue.
(The Sun’s light doesn’t contain as much violet light as it does blue or red, so we won’t see a purple sky. It also helps that our eyes don’t respond strongly to violet light. The cone cells in our retinas are tuned to respond to blue, green, and red, so the other colors are perceived by triggering combinations of the primary cone cells.)
At sunset, light is traveling through a lot more air than it does at noon. That means every ray of light has more of a chance to scatter, removing the blue light before it reaches our eyes. What’s left is red light, making the sky at the horizon near the Sun appear red. In fact, you see more gradations of color too: moving your vision higher in the sky, you’ll note red shades into orange into yellow and so forth, but each color is less intense. So finally: why is the Martian sky pink? The answer is dust: the surface of Mars is covered in a fine powder, more like talcum than sand. During the frequent windstorms that sweep across the planet, this dust is blown high into the air, where light (yes) scatters off of it. Since the grains are larger than air molecules, the kind of scattering is different, and tends to make the light appear red. (Actually, the sky’s “true” color is very hard to determine, since there is a lot more variation than on Earth.) When there is less dust in the atmosphere, the Martian sky is a deep blue, when the Sun’s light scatters off the carbon dioxide molecules in the air. By DXS Physics Editor Matthew Francis
Perhaps the most important question to ask in science is “how do we know?” While it’s appropriate to ask this every day, today it feels even more so, as we prepare to witness a very rare astronomical event. This time, it’s happening on June 5, 2012; when this event occurred during the 18th century, it allowed astronomers to make the first precision measurements of the size of our Solar System. Captain James Cook, best known for his exploration of the Pacific (for Europe, that is—the natives already knew what was there), took a set of scientific instruments aboard his ship to Tahiti; other teams of researchers took measurements at those locations.
The rare event they observed was the transit of Venus: when Venus travels directly between Earth and the Sun, blocking a tiny amount of light. Astronomers in different locations timed the crossing of Venus across the Sun’s disc, and by comparing their numbers, were able to determine the distance between Earth and the Sun. With that distance in hand, they were able to calibrate the size of the entire Solar System. The 1769 observation was an international scientific effort (to use modern language), and while the results weren’t as good as the astronomers of the day had hoped, they still agreed with modern measurements.
Today we use a variety of techniques to measure distances, including radar ranging (bouncing radio waves off planets and timing the round trip), so we don’t have to wait for Venus transits anymore—which is good, since they aren’t common! The last Venus transit was in 2004, but the previous one before that was in 1882, and the next one will be in 2117. I got up very early in the morning on June 8, 2004, joining some fellow astronomy enthusiasts at the Rutgers observatory, where we took the photo you see at the top of the post.
The seemingly odd intervals between transits are because Earth’s and Venus’ orbits around the Sun don’t lie in the same plane. If you draw Earth’s orbit as an ellipse on a sheet of cardboard, and Venus’ orbit on another sheet of cardboard, they need to overlap in a small X pattern, as shown in the picture. The only times Venus will transit is when both Earth and Venus are on the same side of the Sun, and only when they are in the region where the cardboard pieces overlap. The angle (3.5°) in the picture is correct, but I’ve exaggerated the size of the Sun and the sizes of the “transit zones”; in truth, even though the Sun is huge compared to Earth, it’s not that big on the sky. If you do the real calculation, you find that Venus transits happen roughly twice per century, and those two events are separated by 8 years. It’s a rare and wonderful event!
Viewing the Transit
If you want to view the Venus transit, the first thing you should do is see if it will be visible where you live. (Hopefully the weather will cooperate too! Such is the life of an astronomer.) In Richmond, Virginia (where I live), the transit begins around 6 PM. If you’re in the area, the Science Museum of Virginia is hosting a free viewing on the lawn; many other cities and towns have similar events.
A common sense warning: please don’t look directly at the Sun! However, you don’t need fancy equipment or a big observatory to witness the transit. Two weeks ago, I observed the solar eclipse using nothing but a microwave macaroni-and-cheese container. By piercing a hole in the bottom of the tub, I created a simple pinhole camera. A small and kind of fuzzy image of the eclipse appeared on a piece of paper, which I photographed. (Obviously you can do better if you have better equipment—I happened to be far from home during the eclipse and used what I had on hand.) A piece of cardboard covered in aluminum foil with a small hole works better, and you can project the image right onto the sidewalk, the side of a building, or another screen.
If you have a pair of binoculars that use glass lenses (since plastic will melt), point the larger lens toward the Sun and the smaller lens onto a flat surface. (Again, don’t look through the binoculars if you value your eyeballs!) If you have a telescope with a mirror or glass lenses, you can also project the image onto a flat surface, or create a sun funnel. There are a lot of ways to view the Sun if the ones I mention don’t appeal to you.
As a word of caution: the Venus transit won’t look as impressive as a solar eclipse, since Venus is a lot farther away than the Moon. It will appear to be a small round shadow on the Sun’s disc. The thrill (for me at least) lies in the knowledge: you are viewing a planet not much smaller than Earth as it crosses between us and our home star! If it isn’t enough these events are rare, think of how significant it is to catch a glimpse of the sheer size of our Solar System, in a way we don’t usually get to see. And always, always remember to ask the question: “how do we know?”
If you want to know more about transits and why they are still scientifically important today, try these links:
Tonight—August 31, 2012— is the second full Moon of August. The last time two full Moons occurred in the same month was in 2010, and the next will be in 2015, so while the events are rare, they aren’t terribly uncommon either. In fact, you’ve probably heard the second full Moon given a name: “blue moon”. (The Moon will not appear to be a blue color, though, cool as that would be. More on that in a bit.) What you may not know is that this term dates back only to 1946, and is actually a mistake.
According to Sky and Telescope, a premiere astronomy magazine (check your local library!), the writer James Hugh Pruett made an incorrect assumption about the use of the term “blue moon” in his March 1946 article. His source was the Maine Farmers’ Almanac, but he misinterpreted it. The almanac used “blue moon” to refer to the rare occasion when four full Moons happen in one season, when there are usually only three. By the almanac’s standards, tonight’s full moon is not a blue moon (though there will be one on August 21, 2013).
However, even that definition of “blue moon” apparently only dates to the early 19th century. In its colloquial, non-astronomical sense, a “blue moon” is something that rarely or never happens: like the Moon appearing blue. The Moon is white and gray when it’s high in the sky, and can appear very red, orange, or yellow near the horizon for the same reason the Sun does. As far as I can tell, the only time the Moon appears blue is when there’s a lot of volcanic ash in the air, also a rare event (thankfully) for most of the world. The popular song “Blue Moon” (written by everyone’s favorite gay misanthrope, Lorenz Hart) uses “blue” to mean sad, rather than rare.
I’m perfectly happy to keep the common mistaken usage of “blue moon” around, though, since it’s not really a big deal to me. Call tonight’s full Moon a blue moon, and I’ll back you up. However, because it’s me, let’s talk about the Moon and the Sun and why this stuff is kind of arbitrary.
The Moon and the Sun Don’t Get Along
The calendar used in much of the world is the Gregorian calendar, named for Pope Gregory XIII, who instituted it in 1582. The Gregorian calendar, in turn, was based on the older Roman calendar (known as the Julian calendar, for famous pinup girl Julie Callender Julius Caesar). The Romans’ calendar was based on the Sun: a year is the length of time for the Sun to return to the same spot in the sky. This length of time is approximate 365.25 days, which is why there’s a leap year every four years. (Experts know I’m simplifying; if you want more information, see this post at Galileo’s Pendulum.)
A problem arises when you try to break the year into smaller pieces. Traditionally, this has been done through reference to the Moon’s phases. The time to cycle through all the phases of the Moon is called a lunation, which is about 29 days, 12 hours, 44 minutes, and 3 seconds long. You don’t need to pull out a calculator to realize that a lunation doesn’t divide into a year evenly, but it’s still a reasonable way to mark the passage of time within a year, so it’s the foundation of the month (or moonth).
Many calendars—the traditional Chinese calendar, the Jewish calendar, and others—define the month based on a lunation, but don’t fix the number of months in a year. That means some years have 12 months, and others have 13: a leap month. It also means that holidays in these calendars move relative to the Gregorian calendar, such that Yom Kippur or the Chinese New Year don’t fall on the same date in 2012 that they did in 2011. (The Christian religious calendar combines aspects of the Jewish and the Gregorian calendars: Christmas is always December 25, but Easter and associated holidays are tied to Passover—which is coupled to the first full Moon after the spring equinox, and so can occur in a variety of dates in March and April.)
Another resolution to the problem of lunations vs. Sun is to ignore the Sun; this is what the Islamic calendar does. Months are defined by lunations, and the year is precisely 12 months, meaning the year in this calendar is 354 or 355 days long. This is why the holy month of Ramadan moves throughout the Gregorian year, happening sometimes in summer, and sometimes in winter.
The Gregorian calendar does things oppositely to the Islamic calendar: while months are defined, they are not based on a lunation at all. Months may be 30 days long (roughly one lunation), 31 days, or 28 days; the latter two options make no astronomical sense at all. Solar-only calendars have some advantages: since seasons are defined relative to the Sun, the equinoxes and solstices happen roughly on the same date every year, which doesn’t happen in lunation-based calendars. It’s all a matter of taste, culture, and convenience, however, since the cycles of Sun and the Moon don’t cooperate with the length of the day on Earth, or with each other.
Blue moons in the common post-1946 usage never happen in lunation-based calendar systems because by definition each phase of the Moon only occurs once in a month. On the other hand, the version from the Maine Farmers’ Almanac is relevant to any calendar system, because it’s defined by the seasons. As I wrote in my earlier DXS post, seasons are defined by the orbit of Earth around the Sun, and the relative orientation of Earth’s axis. Thus, summer is the same number of days whatever calendar system you use, even though it may not always be the same number of months. In a typical season, there will be three full Moons, but because of the mismatch between lunations and the time between equinoxes and solstices, some rare seasons may have four full Moons.
The Moon and Sun have provided patterns for human life and culture, metaphors for poetry and drama, and of course lots of superstition and pseudoscience. However, one thing most people can agree upon: the full Moon, blue or not, is a thing of beauty. If you can, go out tonight and have a look at it—and give it a wink in honor of the first human to set foot on it, Neil Armstrong.
Today – June 20 – is the northern Summer Solstice, sometimes known as the Northern Solstice, “first day of summer”, or Midsummer’s Day, depending on where you live. It’s the longest day and shortest night of the year in the northern hemisphere (where I live), though exactly howlong or short depends on how far north you live. And of course in the southern hemisphere, today is is the shortest day and longest night, since the seasons are reversed.
The secret to the solstice and to Earth’s seasons in general involves the tilt of Earth’s axis. Our planet orbits the Sun in an elliptical path, which you can draw on a flat piece of paper: it doesn’t move “up” or “down”, but stays in a single plane known as the ecliptic. (The name “ecliptic”, as you might guess, is related to the word “eclipse”, since ancient astronomers determined eclipses of the Moon and Sun could only occur at certain places in the sky.) Earth’s axis is tilted compared to the ecliptic, and the axis points more or less in the same direction, wherever the planet is in its orbit. The axis points almost directly at Polaris, the North Star, which is why that star is a good navigational guide for those in the northern hemisphere: no matter what time of year, it’s always in the same spot in the sky. Other stars rise and set as Earth rotates, but not Polaris. (Unfortunately, there isn’t a South Star.)
As you can see from the diagram above, during about half the year, the North Pole points more toward the Sun, while it points more away for the rest of the year. Where I live, the Sun will never be directly overhead, even at noon. The farthest north that will ever happen is a special latitude known as the Tropic of Cancer – and the northern Summer Solstice is the day that occurs. On the northern Winter Solstice, which happens on December 21 or 22, the Sun is directly overhead at noon at the latitude of the Tropic of Capricorn.
Now we can see why summers are hot! In summer, the Sun rises earlier, sets later, and reaches a higher point in the sky. Those things combined mean extra sunlight, heating up the air and the ground longer. We can also see why I put “first day of summer” in quotes: the Solstice is the apex of the process, but the increase in daylight and temperatures begins long before June 20 (at least every place I’ve lived). The Midsummer’s Day festival, celebrated throughout northern Europe, acknowledges that; Shakespeare’s play A Midsummer Night’s Dream may have been written for the English version of the festival (though from what I can tell, the historical evidence is scant).
Similarly, during winter the Sun’s light comes in at a steeper angle and days are shorter, so the time for the ground to warm is greatly reduced. The northern Winter Solstice (also known as the Southern Solstice, “first day of winter”, Midwinter’s Day, or Yule) is the shortest day and longest night of the year in the northern hemisphere. On that day, the North Pole points as far away from the Sun as it ever does. We also have the reason the tropics are warm all year around: they receive about the same amount of sunlight during both summer and winter.
Approximately halfway between the solstices, the Sun appears directly overhead at noon at the Equator. On those days, everywhere on Earth gets about 12 hours of daylight and 12 hours of night. These days are the equinoxes, meaning “equal night”. (The spell to extinguish light in the Harry Potter books is “nox”, for what it’s worth. Yes, I remember such things. I’m still waiting for my “accio!” summoning spell, though.) The two days are known as the Vernal(or spring) and the Autumnal (or autumn) Equinox, again based on the seasons in the northern hemisphere. From an astronomical point of view, Earth’s “solar year” is marked between successive vernal equinoxes. (A second measurement of the year, known as the sidereal year, is measured with respect to the stars. These two year measurements are almost, but not quite, the same length!)
Now let’s put all of this together in a movie! (For some reason, the Sun – which was a gently glowing lamp in my original simulation – came out looking flat and boring in the final movie. I guess I still have more to learn about creating three-dimensional animations.) For best results, please view this full-screen.
The four basic categories of molecules for building life are carbohydrates, lipids, proteins, and nucleic acids.
Carbohydrates serve many purposes, from energy to structure to chemical communication, as monomers or polymers.
Lipids, which are hydrophobic, also have different purposes, including energy storage, structure, and signaling.
Proteins, made of amino acids in up to four structural levels, are involved in just about every process of life.
The nucleic acids DNA and RNA consist of four nucleotide building blocks, and each has different purposes.
The longer version
Life is so diverse and unwieldy, it may surprise you to learn that we can break it down into four basic categories of molecules. Possibly even more implausible is the fact that two of these categories of large molecules themselves break down into a surprisingly small number of building blocks. The proteins that make up all of the living things on this planet and ensure their appropriate structure and smooth function consist of only 20 different kinds of building blocks. Nucleic acids, specifically DNA, are even more basic: only four different kinds of molecules provide the materials to build the countless different genetic codes that translate into all the different walking, swimming, crawling, oozing, and/or photosynthesizing organisms that populate the third rock from the Sun.
Big Molecules with Small Building Blocks
The functional groups, assembled into building blocks on backbones of carbon atoms, can be bonded together to yield large molecules that we classify into four basic categories. These molecules, in many different permutations, are the basis for the diversity that we see among living things. They can consist of thousands of atoms, but only a handful of different kinds of atoms form them. It’s like building apartment buildings using a small selection of different materials: bricks, mortar, iron, glass, and wood. Arranged in different ways, these few materials can yield a huge variety of structures.
We encountered functional groups and the SPHONC in Chapter 3. These components form the four categories of molecules of life. These Big Four biological molecules are carbohydrates, lipids, proteins, and nucleic acids. They can have many roles, from giving an organism structure to being involved in one of the millions of processes of living. Let’s meet each category individually and discover the basic roles of each in the structure and function of life.
You have met carbohydrates before, whether you know it or not. We refer to them casually as “sugars,” molecules made of carbon, hydrogen, and oxygen. A sugar molecule has a carbon backbone, usually five or six carbons in the ones we’ll discuss here, but it can be as few as three. Sugar molecules can link together in pairs or in chains or branching “trees,” either for structure or energy storage.
When you look on a nutrition label, you’ll see reference to “sugars.” That term includes carbohydrates that provide energy, which we get from breaking the chemical bonds in a sugar called glucose. The “sugars” on a nutrition label also include those that give structure to a plant, which we call fiber. Both are important nutrients for people.
Sugars serve many purposes. They give crunch to the cell walls of a plant or the exoskeleton of a beetle and chemical energy to the marathon runner. When attached to other molecules, like proteins or fats, they aid in communication between cells. But before we get any further into their uses, let’s talk structure.
The sugars we encounter most in basic biology have their five or six carbons linked together in a ring. There’s no need to dive deep into organic chemistry, but there are a couple of essential things to know to interpret the standard representations of these molecules.
Check out the sugars depicted in the figure. The top-left molecule, glucose, has six carbons, which have been numbered. The sugar to its right is the same glucose, with all but one “C” removed. The other five carbons are still there but are inferred using the conventions of organic chemistry: Anywhere there is a corner, there’s a carbon unless otherwise indicated. It might be a good exercise for you to add in a “C” over each corner so that you gain a good understanding of this convention. You should end up adding in five carbon symbols; the sixth is already given because that is conventionally included when it occurs outside of the ring.
On the left is a glucose with all of its carbons indicated. They’re also numbered, which is important to understand now for information that comes later. On the right is the same molecule, glucose, without the carbons indicated (except for the sixth one). Wherever there is a corner, there is a carbon, unless otherwise indicated (as with the oxygen). On the bottom left is ribose, the sugar found in RNA. The sugar on the bottom right is deoxyribose. Note that at carbon 2 (*), the ribose and deoxyribose differ by a single oxygen.
The lower left sugar in the figure is a ribose. In this depiction, the carbons, except the one outside of the ring, have not been drawn in, and they are not numbered. This is the standard way sugars are presented in texts. Can you tell how many carbons there are in this sugar? Count the corners and don’t forget the one that’s already indicated!
If you said “five,” you are right. Ribose is a pentose (pent = five) and happens to be the sugar present in ribonucleic acid, or RNA. Think to yourself what the sugar might be in deoxyribonucleic acid, or DNA. If you thought, deoxyribose, you’d be right.
The fourth sugar given in the figure is a deoxyribose. In organic chemistry, it’s not enough to know that corners indicate carbons. Each carbon also has a specific number, which becomes important in discussions of nucleic acids. Luckily, we get to keep our carbon counting pretty simple in basic biology. To count carbons, you start with the carbon to the right of the non-carbon corner of the molecule. The deoxyribose or ribose always looks to me like a little cupcake with a cherry on top. The “cherry” is an oxygen. To the right of that oxygen, we start counting carbons, so that corner to the right of the “cherry” is the first carbon. Now, keep counting. Here’s a little test: What is hanging down from carbon 2 of the deoxyribose?
If you said a hydrogen (H), you are right! Now, compare the deoxyribose to the ribose. Do you see the difference in what hangs off of the carbon 2 of each sugar? You’ll see that the carbon 2 of ribose has an –OH, rather than an H. The reason the deoxyribose is called that is because the O on the second carbon of the ribose has been removed, leaving a “deoxyed” ribose. This tiny distinction between the sugars used in DNA and RNA is significant enough in biology that we use it to distinguish the two nucleic acids.
In fact, these subtle differences in sugars mean big differences for many biological molecules. Below, you’ll find a couple of ways that apparently small changes in a sugar molecule can mean big changes in what it does. These little changes make the difference between a delicious sugar cookie and the crunchy exoskeleton of a dung beetle.
Sugar and Fuel
A marathon runner keeps fuel on hand in the form of “carbs,” or sugars. These fuels provide the marathoner’s straining body with the energy it needs to keep the muscles pumping. When we take in sugar like this, it often comes in the form of glucose molecules attached together in a polymer called starch. We are especially equipped to start breaking off individual glucose molecules the minute we start chewing on a starch.
Double X Extra: A monomer is a building block (mono = one) and a polymer is a chain of monomers. With a few dozen monomers or building blocks, we get millions of different polymers. That may sound nutty until you think of the infinity of values that can be built using only the numbers 0 through 9 as building blocks or the intricate programming that is done using only a binary code of zeros and ones in different combinations.
Our bodies then can rapidly take the single molecules, or monomers, into cells and crack open the chemical bonds to transform the energy for use. The bonds of a sugar are packed with chemical energy that we capture to build a different kind of energy-containing molecule that our muscles access easily. Most species rely on this process of capturing energy from sugars and transforming it for specific purposes.
Polysaccharides: Fuel and Form
Plants use the Sun’s energy to make their own glucose, and starch is actually a plant’s way of storing up that sugar. Potatoes, for example, are quite good at packing away tons of glucose molecules and are known to dieticians as a “starchy” vegetable. The glucose molecules in starch are packed fairly closely together. A string of sugar molecules bonded together through dehydration synthesis, as they are in starch, is a polymer called a polysaccharide (poly = many; saccharide = sugar). When the monomers of the polysaccharide are released, as when our bodies break them up, the reaction that releases them is called hydrolysis.
Double X Extra: The specific reaction that hooks one monomer to another in a covalent bond is called dehydration synthesis because in making the bond–synthesizing the larger molecule–a molecule of water is removed (dehydration). The reverse is hydrolysis (hydro = water; lysis = breaking), which breaks the covalent bond by the addition of a molecule of water.
Although plants make their own glucose and animals acquire it by eating the plants, animals can also package away the glucose they eat for later use. Animals, including humans, store glucose in a polysaccharide called glycogen, which is more branched than starch. In us, we build this energy reserve primarily in the liver and access it when our glucose levels drop.
Whether starch or glycogen, the glucose molecules that are stored are bonded together so that all of the molecules are oriented the same way. If you view the sixth carbon of the glucose to be a “carbon flag,” you’ll see in the figure that all of the glucose molecules in starch are oriented with their carbon flags on the upper left.
The orientation of monomers of glucose in polysaccharides can make a big difference in the use of the polymer. The glucoses in the molecule on the top are all oriented “up” and form starch. The glucoses in the molecule on the bottom alternate orientation to form cellulose, which is quite different in its function from starch.
Storing up sugars for fuel and using them as fuel isn’t the end of the uses of sugar. In fact, sugars serve as structural molecules in a huge variety of organisms, including fungi, bacteria, plants, and insects.
The primary structural role of a sugar is as a component of the cell wall, giving the organism support against gravity. In plants, the familiar old glucose molecule serves as one building block of the plant cell wall, but with a catch: The molecules are oriented in an alternating up-down fashion. The resulting structural sugar is called cellulose.
That simple difference in orientation means the difference between a polysaccharide as fuel for us and a polysaccharide as structure. Insects take it step further with the polysaccharide that makes up their exoskeleton, or outer shell. Once again, the building block is glucose, arranged as it is in cellulose, in an alternating conformation. But in insects, each glucose has a little extra added on, a chemical group called an N-acetyl group. This addition of a single functional group alters the use of cellulose and turns it into a structural molecule that gives bugs that special crunchy sound when you accidentally…ahem…step on them.
These variations on the simple theme of a basic carbon-ring-as-building-block occur again and again in biological systems. In addition to serving roles in structure and as fuel, sugars also play a role in function. The attachment of subtly different sugar molecules to a protein or a lipid is one way cells communicate chemically with one another in refined, regulated interactions. It’s as though the cells talk with each other using a specialized, sugar-based vocabulary. Typically, cells display these sugary messages to the outside world, making them available to other cells that can recognize the molecular language.
Lipids: The Fatty Trifecta
Starch makes for good, accessible fuel, something that we immediately attack chemically and break up for quick energy. But fats are energy that we are supposed to bank away for a good long time and break out in times of deprivation. Like sugars, fats serve several purposes, including as a dense source of energy and as a universal structural component of cell membranes everywhere.
Fats: the Good, the Bad, the Neutral
Turn again to a nutrition label, and you’ll see a few references to fats, also known as lipids. (Fats are slightly less confusing that sugars in that they have only two names.) The label may break down fats into categories, including trans fats, saturated fats, unsaturated fats, and cholesterol. You may have learned that trans fats are “bad” and that there is good cholesterol and bad cholesterol, but what does it all mean?
Let’s start with what we mean when we say saturated fat. The question is, saturated with what? There is a specific kind of dietary fat call the triglyceride. As its name implies, it has a structural motif in which something is repeated three times. That something is a chain of carbons and hydrogens, hanging off in triplicate from a head made of glycerol, as the figure shows. Those three carbon-hydrogen chains, or fatty acids, are the “tri” in a triglyceride. Chains like this can be many carbons long.
Double X Extra: We call a fatty acid a fatty acid because it’s got a carboxylic acid attached to a fatty tail. A triglyceride consists of three of these fatty acids attached to a molecule called glycerol. Our dietary fat primarily consists of these triglycerides.
Triglycerides come in several forms. You may recall that carbon can form several different kinds of bonds, including single bonds, as with hydrogen, and double bonds, as with itself. A chain of carbon and hydrogens can have every single available carbon bond taken by a hydrogen in single covalent bond. This scenario of hydrogen saturation yields a saturated fat. The fat is saturated to its fullest with every covalent bond taken by hydrogens single bonded to the carbons.
Saturated fats have predictable characteristics. They lie flat easily and stick to each other, meaning that at room temperature, they form a dense solid. You will realize this if you find a little bit of fat on you to pinch. Does it feel pretty solid? That’s because animal fat is saturated fat. The fat on a steak is also solid at room temperature, and in fact, it takes a pretty high heat to loosen it up enough to become liquid. Animals are not the only organisms that produce saturated fat–avocados and coconuts also are known for their saturated fat content.
The top graphic above depicts a triglyceride with the glycerol, acid, and three hydrocarbon tails. The tails of this saturated fat, with every possible hydrogen space occupied, lie comparatively flat on one another, and this kind of fat is solid at room temperature. The fat on the bottom, however, is unsaturated, with bends or kinks wherever two carbons have double bonded, booting a couple of hydrogens and making this fat unsaturated, or lacking some hydrogens. Because of the space between the bumps, this fat is probably not solid at room temperature, but liquid.
You can probably now guess what an unsaturated fat is–one that has one or more hydrogens missing. Instead of single bonding with hydrogens at every available space, two or more carbons in an unsaturated fat chain will form a double bond with carbon, leaving no space for a hydrogen. Because some carbons in the chain share two pairs of electrons, they physically draw closer to one another than they do in a single bond. This tighter bonding result in a “kink” in the fatty acid chain.
In a fat with these kinks, the three fatty acids don’t lie as densely packed with each other as they do in a saturated fat. The kinks leave spaces between them. Thus, unsaturated fats are less dense than saturated fats and often will be liquid at room temperature. A good example of a liquid unsaturated fat at room temperature is canola oil.
A few decades ago, food scientists discovered that unsaturated fats could be resaturated or hydrogenated to behave more like saturated fats and have a longer shelf life. The process of hydrogenation–adding in hydrogens–yields trans fat. This kind of processed fat is now frowned upon and is being removed from many foods because of its associations with adverse health effects. If you check a food label and it lists among the ingredients “partially hydrogenated” oils, that can mean that the food contains trans fat.
Double X Extra: A triglyceride can have up to three different fatty acids attached to it. Canola oil, for example, consists primarily of oleic acid, linoleic acid, and linolenic acid, all of which are unsaturated fatty acids with 18 carbons in their chains.
Why do we take in fat anyway? Fat is a necessary nutrient for everything from our nervous systems to our circulatory health. It also, under appropriate conditions, is an excellent way to store up densely packaged energy for the times when stores are running low. We really can’t live very well without it.
Phospholipids: An Abundant Fat
You may have heard that oil and water don’t mix, and indeed, it is something you can observe for yourself. Drop a pat of butter–pure saturated fat–into a bowl of water and watch it just sit there. Even if you try mixing it with a spoon, it will just sit there. Now, drop a spoon of salt into the water and stir it a bit. The salt seems to vanish. You’ve just illustrated the difference between a water-fearing (hydrophobic) and a water-loving (hydrophilic) substance.
Generally speaking, compounds that have an unequal sharing of electrons (like ions or anything with a covalent bond between oxygen and hydrogen or nitrogen and hydrogen) will be hydrophilic. The reason is that a charge or an unequal electron sharing gives the molecule polarity that allows it to interact with water through hydrogen bonds. A fat, however, consists largely of hydrogen and carbon in those long chains. Carbon and hydrogen have roughly equivalent electronegativities, and their electron-sharing relationship is relatively nonpolar. Fat, lacking in polarity, doesn’t interact with water. As the butter demonstrated, it just sits there.
There is one exception to that little maxim about fat and water, and that exception is the phospholipid. This lipid has a special structure that makes it just right for the job it does: forming the membranes of cells. A phospholipid consists of a polar phosphate head–P and O don’t share equally–and a couple of nonpolar hydrocarbon tails, as the figure shows. If you look at the figure, you’ll see that one of the two tails has a little kick in it, thanks to a double bond between the two carbons there.
Phospholipids form a double layer and are the major structural components of cell membranes. Their bend, or kick, in one of the hydrocarbon tails helps ensure fluidity of the cell membrane. The molecules are bipolar, with hydrophilic heads for interacting with the internal and external watery environments of the cell and hydrophobic tails that help cell membranes behave as general security guards.
The kick and the bipolar (hydrophobic and hydrophilic) nature of the phospholipid make it the perfect molecule for building a cell membrane. A cell needs a watery outside to survive. It also needs a watery inside to survive. Thus, it must face the inside and outside worlds with something that interacts well with water. But it also must protect itself against unwanted intruders, providing a barrier that keeps unwanted things out and keeps necessary molecules in.
Phospholipids achieve it all. They assemble into a double layer around a cell but orient to allow interaction with the watery external and internal environments. On the layer facing the inside of the cell, the phospholipids orient their polar, hydrophilic heads to the watery inner environment and their tails away from it. On the layer to the outside of the cell, they do the same.
As the figure shows, the result is a double layer of phospholipids with each layer facing a polar, hydrophilic head to the watery environments. The tails of each layer face one another. They form a hydrophobic, fatty moat around a cell that serves as a general gatekeeper, much in the way that your skin does for you. Charged particles cannot simply slip across this fatty moat because they can’t interact with it. And to keep the fat fluid, one tail of each phospholipid has that little kick, giving the cell membrane a fluid, liquidy flow and keeping it from being solid and unforgiving at temperatures in which cells thrive.
Steroids: Here to Pump You Up?
Our final molecule in the lipid fatty trifecta is cholesterol. As you may have heard, there are a few different kinds of cholesterol, some of which we consider to be “good” and some of which is “bad.” The good cholesterol, high-density lipoprotein, or HDL, in part helps us out because it removes the bad cholesterol, low-density lipoprotein or LDL, from our blood. The presence of LDL is associated with inflammation of the lining of the blood vessels, which can lead to a variety of health problems.
But cholesterol has some other reasons for existing. One of its roles is in the maintenance of cell membrane fluidity. Cholesterol is inserted throughout the lipid bilayer and serves as a block to the fatty tails that might otherwise stick together and become a bit too solid.
Cholesterol’s other starring role as a lipid is as the starting molecule for a class of hormones we called steroids or steroid hormones. With a few snips here and additions there, cholesterol can be changed into the steroid hormones progesterone, testosterone, or estrogen. These molecules look quite similar, but they play very different roles in organisms. Testosterone, for example, generally masculinizes vertebrates (animals with backbones), while progesterone and estrogen play a role in regulating the ovulatory cycle.
Double X Extra: A hormone is a blood-borne signaling molecule. It can be lipid based, like testosterone, or short protein, like insulin.
As you progress through learning biology, one thing will become more and more clear: Most cells function primarily as protein factories. It may surprise you to learn that proteins, which we often talk about in terms of food intake, are the fundamental molecule of many of life’s processes. Enzymes, for example, form a single broad category of proteins, but there are millions of them, each one governing a small step in the molecular pathways that are required for living.
Levels of Structure
Amino acids are the building blocks of proteins. A few amino acids strung together is called a peptide, while many many peptides linked together form a polypeptide. When many amino acids strung together interact with each other to form a properly folded molecule, we call that molecule a protein.
For a string of amino acids to ultimately fold up into an active protein, they must first be assembled in the correct order. The code for their assembly lies in the DNA, but once that code has been read and the amino acid chain built, we call that simple, unfolded chain the primary structure of the protein.
This chain can consist of hundreds of amino acids that interact all along the sequence. Some amino acids are hydrophobic and some are hydrophilic. In this context, like interacts best with like, so the hydrophobic amino acids will interact with one another, and the hydrophilic amino acids will interact together. As these contacts occur along the string of molecules, different conformations will arise in different parts of the chain. We call these different conformations along the amino acid chain the protein’s secondary structure.
Once those interactions have occurred, the protein can fold into its final, or tertiary structure and be ready to serve as an active participant in cellular processes. To achieve the tertiary structure, the amino acid chain’s secondary interactions must usually be ongoing, and the pH, temperature, and salt balance must be just right to facilitate the folding. This tertiary folding takes place through interactions of the secondary structures along the different parts of the amino acid chain.
The final product is a properly folded protein. If we could see it with the naked eye, it might look a lot like a wadded up string of pearls, but that “wadded up” look is misleading. Protein folding is a carefully regulated process that is determined at its core by the amino acids in the chain: their hydrophobicity and hydrophilicity and how they interact together.
In many instances, however, a complete protein consists of more than one amino acid chain, and the complete protein has two or more interacting strings of amino acids. A good example is hemoglobin in red blood cells. Its job is to grab oxygen and deliver it to the body’s tissues. A complete hemoglobin protein consists of four separate amino acid chains all properly folded into their tertiary structures and interacting as a single unit. In cases like this involving two or more interacting amino acid chains, we say that the final protein has a quaternary structure. Some proteins can consist of as many as a dozen interacting chains, behaving as a single protein unit.
A Plethora of Purposes
What does a protein do? Let us count the ways. Really, that’s almost impossible because proteins do just about everything. Some of them tag things. Some of them destroy things. Some of them protect. Some mark cells as “self.” Some serve as structural materials, while others are highways or motors. They aid in communication, they operate as signaling molecules, they transfer molecules and cut them up, they interact with each other in complex, interrelated pathways to build things up and break things down. They regulate genes and package DNA, and they regulate and package each other.
As described above, proteins are the final folded arrangement of a string of amino acids. One way we obtain these building blocks for the millions of proteins our bodies make is through our diet. You may hear about foods that are high in protein or people eating high-protein diets to build muscle. When we take in those proteins, we can break them apart and use the amino acids that make them up to build proteins of our own.
How does a cell know which proteins to make? It has a code for building them, one that is especially guarded in a cellular vault in our cells called the nucleus. This code is deoxyribonucleic acid, or DNA. The cell makes a copy of this code and send it out to specialized structures that read it and build proteins based on what they read. As with any code, a typo–a mutation–can result in a message that doesn’t make as much sense. When the code gets changed, sometimes, the protein that the cell builds using that code will be changed, too.
Biohazard!The names associated with nucleic acids can be confusing because they all start with nucle-. It may seem obvious or easy now, but a brain freeze on a test could mix you up. You need to fix in your mind that the shorter term (10 letters, four syllables), nucleotide, refers to the smaller molecule, the three-part building block. The longer term (12 characters, including the space, and five syllables), nucleic acid, which is inherent in the names DNA and RNA, designates the big, long molecule.
DNA vs. RNA: A Matter of Structure
DNA and its nucleic acid cousin, ribonucleic acid, or RNA, are both made of the same kinds of building blocks. These building blocks are called nucleotides. Each nucleotide consists of three parts: a sugar (ribose for RNA and deoxyribose for DNA), a phosphate, and a nitrogenous base. In DNA, every nucleotide has identical sugars and phosphates, and in RNA, the sugar and phosphate are also the same for every nucleotide.
So what’s different? The nitrogenous bases. DNA has a set of four to use as its coding alphabet. These are the purines, adenine and guanine, and the pyrimidines, thymine and cytosine. The nucleotides are abbreviated by their initial letters as A, G, T, and C. From variations in the arrangement and number of these four molecules, all of the diversity of life arises. Just four different types of the nucleotide building blocks, and we have you, bacteria, wombats, and blue whales.
RNA is also basic at its core, consisting of only four different nucleotides. In fact, it uses three of the same nitrogenous bases as DNA–A, G, and C–but it substitutes a base called uracil (U) where DNA uses thymine. Uracil is a pyrimidine.
DNA vs. RNA: Function Wars
An interesting thing about the nitrogenous bases of the nucleotides is that they pair with each other, using hydrogen bonds, in a predictable way. An adenine will almost always bond with a thymine in DNA or a uracil in RNA, and cytosine and guanine will almost always bond with each other. This pairing capacity allows the cell to use a sequence of DNA and build either a new DNA sequence, using the old one as a template, or build an RNA sequence to make a copy of the DNA.
These two different uses of A-T/U and C-G base pairing serve two different purposes. DNA is copied into DNA usually when a cell is preparing to divide and needs two complete sets of DNA for the new cells. DNA is copied into RNA when the cell needs to send the code out of the vault so proteins can be built. The DNA stays safely where it belongs.
RNA is really a nucleic acid jack-of-all-trades. It not only serves as the copy of the DNA but also is the main component of the two types of cellular workers that read that copy and build proteins from it. At one point in this process, the three types of RNA come together in protein assembly to make sure the job is done right.
The Sun will rise on the morning of December 22 and find most of humanity still living. I can say that with a great deal of confidence, though my scientist’s brain tells me I should say the world “probably” won’t end tomorrow. After all, there’s a tiny chance, a minuscule probability…but it’s so small we don’t have to worry about it, just like we don’t have to worry about being struck down by a meteorite while walking down the street. It could happen, but it almost certainly won’t.
My confidence comes from science. I know it sounds hokey, but it’s true. There’s no scientific reason—absolutely none—to think the world will end tomorrow. Yes, the world will end one day, and Earth has experienced some serious cataclysms in the past that wiped out a significant amount of life, but none of those things are going to happen tomorrow. (I’ll come back to those points in a bit.) We’re very good at science, after centuries of work, and the kinds of violent events that could seriously threaten us won’t take us by surprise.
Why the World Won’t End
So where does this stuff come from? Whose idea was it that “the end of the world will be on December 21, 2012″? The culprit, according to those who buy into the idea, is that the end of the world was predicted by the Mayas in their mythology, and codified in their calendar. However, it’s pretty safe to say that the Mayas didn’t really predict the end of the world, even though I don’t know much about the great Mayan civilization that existed on the Yucatan peninsula in what is now Mexico from antiquity until the Spanish conquest.
See this calendar? It’s being touted as a Mayan
calendar in articles about the “end of the world”,
but it ain’t Mayan. It’s an Aztec calendar. Please
don’t mix up civilizations.
The Mayas were the only people in the Americas known to have developed a complete written language, which is part of how we know a lot about them despite their destruction by the hand of European invaders. In particular, we know about their calendar, and the divisions they used. We use what’s called a decimal system for numbers, based on the 10 fingers of our hands. That’s why we break things up into decades (ten years) and centuries (ten decades), as well as a millennium (ten centuries). The Mayas liked different divisions of time: their b’ak’tun is approximately 394 years, and they placed a certain significance on a cycle of 13 b’ak’tuns. (I suspect the Klingon language in Star Trek borrowed some of its vocabulary from ancient Mayan.)
In the “Long Count,” one version of the Mayan calendar known to us, the present world came to be on August 11, 3114 BC. That world will end at the close of the 13th b’ak’tun from that creation day, which happens to be December 21, 2012. However, there’s good reason to think that the Mayas didn’t believe this would be the end of all things: other calendars exist that refer to an even longer span of years, stretching thousands of years into the future!
Even more importantly, though: the Mayan cosmology (their view of the universe) was cyclic, as in many other religions. This world was not the first in this cosmology, and it won’t be the last. In such a view, the true universe is eternal, and the cycles of time are a kind of divine rebooting, which don’t really end anything. The end of the 13th b’ak’tun might be a transformative event in the Maya cosmology, but it’s not the end of the world.
Frankly, I’m not sure why we should care even if the Mayas did believe this was the end of the world. As I said previously, there’s no scientific reason to think the world will end tomorrow. But maybe you might think there’s a non-scientific reason—divine intervention to wipe out the Earth, perhaps. However, I’d venture to guess that most of us don’t adhere to the Mayan religion. Their gods are not the gods most people worship. The prophesied arrival on Earth of Bolon Yookte’ K’Uh, the Nine-Footed God is not something central to my belief system, and probably not yours either.
In fact, millennial thinking is far more a Christian thing than it is a Mayan thing—or frankly most other religions. When people talk about the supposed end of the world tomorrow, they use the Christian terminology: Armageddon (referring to Megiddo, a place in northern Israel, named in the Book of Revelation as the site of the last battle) or the apocalypse (literally the “uncovering”, when all that was hidden becomes revealed). These weren’t concepts in the Mayan religion, and nothing in the Christian religion says the world will end on December 21, 2012.
The World Will End…Eventually
Some say the world will end in fire,
Some say in ice.
From what I’ve tasted of desire
I hold with those who favor fire.
Science tells us the world won’t end tomorrow. It also tells us the Mayan cosmology is wrong: time doesn’t go in cycles forever. Earth began 4.5 billion years ago, and will end in about 5 billion years more—at least as a livable world, which is what counts for us. In between its beginning and end, it is defined by cycles: the length of rotation (days) and the time to travel around the Sun (years), with its associated seasons. Other cycles are pretty arbitrary: centuries and b’ak’tuns don’t have any particular significance in terms of astronomical events.
The end of the world as we know it will happen in about 5 billion years, when the Sun ceases fusing hydrogen into helium in its core. When that happens, the Sun will grow into a red giant star, swallowing up Mercury and Venus. Earth probably won’t be devoured, but with the Sun’s surface so much closer, things will become distinctly unpleasant. It’s unlikely the atmosphere or oceans could survive, meaning the end of most life. (Some microbes could probably continue to live underground. That kind of thing is a story for another day.) However, 5 billion years is a long time from now.
Could another cataclysm overtake us before that time? Yes. As you may know, about 65 million years ago, a large asteroid smashed into Earth, an event that at least helped end the reign of dinosaurs, and ushering the extinction of many other species.
Unfortunately, we can’t rule out the possibility that could happen again. There are enough asteroids and comets in our Solar System that could eventually cross orbital paths with Earth; if a large specimen collided with us, it would be devastating.
However, we’re talking about tomorrow. No asteroid will strike Earth on December 21: astronomers keep careful track of everything near our planet, and nothing we know of is on a collision course with Earth for the near future. Asteroids and comets are really the only things we have to worry about doing serious damage for life on Earth, but you can sleep easy tonight and tomorrow night: we’re safe.
If you could somehow see the planets during
daylight hours, here’s how they would
appear tomorrow at noon. There’s no
alignment. (You can see this for yourself
using the free planetarium program Stellarium.)
Some people have talked about fairly far-fetched ideas: alignments of planets, or lining up Earth, the Sun, and the center of the galaxy. The planets of the Solar System aren’t aligned tomorrow—the image shows where several of them are in relation to the Sun at noon. Jupiter isn’t anywhere close to the planets you see. You’d need a pretty strong imagination to say they’re lined up in any way: while they do lie along a line, that’s the way they always are, since they all orbit the Sun more or less in the same plane. Alignment with the galactic center is even more simple to dismiss: about once a year, the Sun appears aligned with the galactic center in the sky. And nothing happens.
Another explanation I’ve seen involves a mysterious planet called “Nibiru” or “Planet X,” which either will collide with Earth or otherwise generate a baleful influence. Phil Plait, the Bad Astronomer, has a lot about the Nibiru nonsense, so I won’t repeat what he says. Suffice to say Nibiru doesn’t exist: there’s no evidence for it, and (surprise!) it’s not anything that came from Mayan mythology to begin with, so there’s no reason to associate it with a December 21 apocalypse.
A Positive Conclusion
Science, I think, is reassuring in the midst of panic. Why people like to scare themselves and others with misguided ideas of the world’s end, I am not qualified to say. I don’t know how many people are convinced the world will end tomorrow, compared with the number of people who are either wholly skeptical or those who might be a little worried. However, let me reassure you again: the world will not end tomorrow. We can take comfort in the knowledge that December 22 will come, 2012 will end, and a new year—a new cycle—will begin. Any remaking of the world is up to us, so rather than worrying about imaginary apocalypses, let’s commit to improving the lives of those who live on our magnificent planet.
I arrived at my building’s outpatient unit at 1:38 pm (I work in a hospital). Although my appointment was at 1:40 pm, I still gave myself a huge pat on the back for being “early,” which, technically, I was. A few signatures later, I was handed a paper gown of fairly decent quality and was instructed to wear it, opening to the back, after removing everything except my skivvies. There I was, sitting on the examination table, feeling quite vulnerable. And then I looked down. Crap! My legs were still in hibernation state. Even though doctors aren’t supposed to judge, I just didn’t see how this could fly under the radar. My only hope was that someone much more hairy had already been examined, setting some arbitrary threshold that would place me under “I’ve seen worse” category. Before my mind drifted into a state where I imagined every possible uncomfortable doctor-patient exchange, the doctor entered the room. It was a dude. I was a bit disappointed but there was nothing I could do about that. It was apparent that I was slightly embarrassed, and his attempt at making small talk did not help to dispel the awkwardness of having to let him scan every inch of my skin, including my you-know-what areas, for abnormalities. But I knew that this exam could save my life.
Skin cancer is the most common cancer in humans and comes in several varieties, including basal cell carcinoma (BCC), squamous cell carcinoma (SCC), and melanoma. BCC is the most commonly acquired skin cancer, accounting for nearly 80% of skin cancers reported. As its name implies, BCC develops in the basal layer of the epidermis and often presents as a pearly, flesh colored nodule, usually on areas that get sun exposures (head, neck, arms). SCC, which arises in the squamous cell population of the epidermis, is the second most common type of skin cancer, affecting approximately 200,000 people each year, and often resembles a scaly patch surrounded by a red halo of inflamed skin. While sun exposed areas are more vulnerable, SCC can occur anywhere on the body (including genitalia) and, if not detected in a timely fashion, can spread to other areas in the body. The nastiest version of skin cancer is the potentially (and often) fatal melanoma. Either developing in a pre-existing mole or spontaneously appearing as a new dark spot on the skin, melanoma claims the life of one person per hour in the United States alone (including the life of my great uncle, Hank).
There are a number of misconceptionswhen it comes to skin cancers, such as the notion that people of color are less vulnerable. While an increase in the amount of the skin pigment called melanindoes provide more protection from the sun, the skin cancer survival rate for people of color is considerably lower than that of Caucasian people.This has mainly been attributed to a delay in detection, highlighting that everyoneneeds to undergo regular skin cancer screening procedures.Also, it is commonly thought that early signs of skin cancer should be painful.However, there are no symptoms associated with the development of most skin cancers and, other than visual signs, early skin cancer lesions can feel like normal skin.
The best bet is to be aware of the skin cancer risk factors, including sun exposure, family history, medical history, and number of moles, so that you can better protect yourself. Also, using water-resistant sunscreen containing both UVA and UVB protection (SPF 30 or greater), seeking shade whenever possible, and avoiding tanning beds, are great tactics for skin cancer prevention. Even if you follow all the rules, be sure to give yourself a periodic self-examination. Furthermore, get screened by a professional on an annual basis. Visit the American Academy of Dermatology to locate the free skin cancer screenings in your area.
Remember, even though you might have to bare your body to some random dude (with credentials), early detection is the key for survival. Plus, it’s all over in 5 minutes or less. I’d trade that for a healthy lifetime any day.