Introduction

In today’s Beyond Earth Series episode, we will learn about our own galaxy, the Milky Way. We will start learning more about our own stars and other stars in our galaxy, and then we will go even further to talk about black holes and dark matter.

Audio Episode

Episode Transcript

0:03
Our planet as magnificent as it is, is just one planet circling an ordinary star in a rural section of our galaxy. The Milky Way isn’t just a static collection of stars, however, but a roiling dynamic place. Stars are born in the collapse of gigantic clouds of dust and debris. They keep themselves alive by consuming the primordial hydrogen of the universe. They use nuclear processes to create the heavier elements, including the carbon that makes up much of your body. Eventually, stars run out of fuel and die, returning their heavy elements to the interstellar clouds from which new stars and planets are made. In death, they leave behind a strange many jury of objects, including white dwarfs, pulsars, and even black holes. In recent decades, astronomers discovered that just as the inner planets are actually a small part of the solar system, the mighty pinwheel of the Milky Way is just a small part of the galaxy. In fact, the spiral arms of the Milky Way are enclosed in a mysterious substance known as Dark Matter puzzling out the nature of dark matter remains a major research project today, interested yet because that’s what we’re going to talk about. We’re going to talk about the Milky Way our own galaxy, our own hometown in the universe. Last time in our Beyond Earth series, we talked about our very own neighborhood, and that is the solar system, but this time we will talk about the Milky Way. So welcome to a new episode from our Beyond Earth series. This is your host, Danny and this is English plus podcast.

1:52
So let’s start our journey in the Milky Way by talking about the sun, the star next door. Every day on earth begins when one representative star of the Milky Way Galaxy, a very ordinary star pokes its nose above the eastern horizon. The sun plays such a central role in life on Earth, that it is easy for us to forget that it is, after all, just one more star in a galaxy full of them. everyday experience can lead you to one of the great scientific questions that occupied astronomers when they began thinking seriously about the sun. Stand outside on a summer day and feel its warmth on your face. Energy is coming to you from the sun, this energy has to come from some source inside the sun. But what it wasn’t until the early 1930s that the young German American physicist Hans Betha showed that the energy source of Stars was the process of nuclear fusion. And this means that every star must sooner or later run out of energy. Stars are not forever, but are born and die like everything else. So what is this power at the core of the Sun, the Sun in the solar system formed from the gravitational collapse of an interstellar dust cloud with more than 99% of that dust cloud being incorporated into the sun. One of the basic rules of nature is that as objects contract they heat up. So when the great gas cloud contracted, it got warmer, the particles and atoms that made up the cloud moved faster and faster, and the collisions between them became more and more violent. Eventually, they became so violent that electrons started to be torn loose from their atoms. The material in the sun became what physicists call a Plasma, a collection of negatively charged electrons and positively charged nuclei moving around independently of each other. And now let’s talk a little bit about the sun structure. For 4.5 billion years, the sun has been burning hydrogen at the rate of more than 400 million tons per second, and it will continue to do so for another 5.5 billion years. The core of the sun where it is hot enough for nuclear reactions to occur extends outward about a quarter of the way to the surface moving outward from the core to about 70% of the distance to the surface, we encounter what is called the radiative zone. In this region, the fast moving particles experienced a series of collisions beyond that the density of matter becomes too low for these kinds of collisions to impede the energy flow and the sun actually boils just like water on the stove. This convective zone extends almost all the way to the surface. Looking at the sun from the outside is a little light looking down into murky water. We can see only about 160 kilometers or about 100 miles deep into the sun through the thin outer layer called the photosphere above the

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photosphere are tenuous layers of atmosphere such as the corona, which is visible during the eclipses. And there’s the heliosphere, which actually extend out past the orbit of Pluto. And because the sun is not solid, different parts of it rotate at different speeds. This difference together with a constantly churning convection beneath the photosphere causes the magnetic field of the sun to be constantly twisted, distorted and pulled around giving rise to phenomena like sunspots and solar flares. Sunspots go through an 11 year cycle in which the number of observed spots increases and drops the solar cycle. And particularly solar flares can have an effect on things like satellite operations and radio transmissions on Earth. So that is in a nutshell about the sun, the star that we have next door, which is the source of life as we know it here on Earth. But that was just the beginning of our journey in the Milky Way. Of course, we started from something we think we know. But trust me, we still don’t know anything about or at least let’s not say anything. But we still have a lot to learn about our own sun this star next door. But for our journey today in Beyond Earth series, we’re not going to stop here, we’re gonna go further and next we’re going to talk about exoplanets. So that’s coming next, don’t go anywhere, I’ll be right back.

6:29
The idea that there are planetary systems circling other stars is an old one. Only in the last few decades, though, has the search for extrasolar planets or exoplanets became a major feature of galactic astronomy. The reason for the delay is simple. The technology was not yet up to the task. Planets shined by reflected light and are thus much dimmer than stars. Furthermore, they are located close to stars, so whatever light they sent out is swamped by light from their parents star. One astronomer likened the problem of seeing an exoplanet directly to detecting a birthday candle next to a search light in Boston by using a telescope in Washington DC. Consequently, the discovery of exoplanet had to wait for new kinds of detection techniques. So let’s talk about the very first detection. The first successful technique for detection of exoplanets is known as radial velocity measurement. To see how it works. Imagine that you are an observer looking at our own solar system from a distance of many light years. We are accustomed to thinking of the sun as being stationary while planets circled in their orbits, but in fact, the sun moves around a bit in response to the planet’s gravitational pull to for example, if Jupiter lay between you and the sun, when you were making your observation, the sun would be pulled slightly in your direction. Later, when Jupiter revolved behind the sun, the sun would be pulled slightly away from you over a 10 year period, then you would see the sun moving towards you for a while, then away from you. This motion can be detected by observing the Doppler shift in the light the sun emits bluer as it moves toward you render as it moves away. So although you couldn’t see Jupiter directly, you would know that it is there because of its effect on the sun. The first detection of an exoplanet in 1992 involves a rare case in which the planet must have formed after its parents star became a supernova. This was followed in 1995, however, by the discovery of a planet circling a more conventional star in the constellation Pegasus and with this ushering in the modern era of exoplanet detection. At first, the discoveries came in slowly at the rate of a few a year. But as the technique improved the pace picked up. We now know of several 1000 possible planetary system around other stars and astronomers predict that there will turn out to be billions of planets in our own galaxy and talking about that we need to talk about the Kepler mission. A Kepler is a spacecraft weighing in at a little over a ton. It is equipped to provide continuous monitoring of the brightness of more than 150,000 stars in our immediate galactic neighborhood because the satellites in low Earth orbit can have up to half the sky blocked by Earth’s disk. And because Kepler needs to watch the sky continuously, the spacecraft is actually maintained in an orbit around the sun, not the earth. You can think of it as trailing along behind earth like a miniature planet. The basic planet hunting technique used by Kepler is simple to describe but requires sophisticated equipment to make it work. The central idea is that if up

10:00
planet passes in front of a star, the brightness of that star will drop while the planet is making its transit then pick up again as the planet moves past in its orbit. Of course, this so called transit method of detection works only if the orbit of the planet takes it directly between the star and the observer. For example, if someone were observing our solar system, Jupiter could be detected by the transit method if the observer were located on the same plane as the planetary orbits, but not if he or she was above or below it. This means that only a tiny fraction of planetary systems can be detected by transit techniques. On the other hand, Kepler scientists are quick to point out that the transit method has one important advantage over the older radial velocity technique. In order for a planet to influence the star enough to produce a detectable Doppler shift, the planet has to exert a large gravitational attraction on the star. This means that the radial velocity method is most likely to detect large planets orbiting close to their stars. And these are the so called Hot Jupiters, and indeed, most of the planets detected before the Kepler launch or of this time. The transit method by contrast detects any planet that affects its stars brightness, regardless of its size, or distance from the star. In fact, one of Kepler’s most important results is the realization that the hot Jupiters are not all that common. They were just the first exoplanets to be seen this game as a great relief to scientists who study planet formation, because theory tells us that large planets should form far from their stars. So while the detection of exoplanets started slow, it really picked up speed until we reached a place where we have a treasure trove of exoplanets. By early 2013, the Kepler team had identified more than 3500 possible exoplanets, astronomers refer to these objects initially as candidates. This is not a case of excessive caution, but simply recognition of the fact that events other than planetary transits can cause a star’s brightness to flicker. A large collection of sunspots could do this for example, as good and eclipsing binary stars so close to the line of sight that the spacecraft can tell that it is a separate object. A minimum requirements then is that the transit repeat at the regular intervals appropriate for a planet in orbit. In fact, Kepler scientists describe two hurdles that a candidate must overcome before it is granted the rank of planet confirmation and validation. Confirmation requires that enough data be gathered to determine the object’s mass usually by having ground based telescopes measure the stars radial velocities after Kepler has identified a likely system. In some cases, monitoring the transits of several planets in a system allow scientists to work out the complex dynamics of motion and get the masses that way. Validation is the process of going through the data carefully and eliminating all the false positives that could fool you into thinking you had found a planetary system. Now unfortunately, in May 2013, the Kepler spacecraft lost functioning in the second of its four gyroscope like wheels, a loss that deprives engineers of the ability to point the spacecraft precisely. Although it can still carry out some studies. The spacecraft which completed its prime mission in 2012, will be of limited use in the future. The real Holy Grail of planetary science, an Earth like planet that could support life or perhaps already does will be found by spacecraft following the trail that Kepler blazed. Over the past 50 years, scientists have discovered life in unexpected places right here on Earth, newly discovered forms of life called extremophiles thrive in conditions such as highly acidic and highly salty environments that would have killed ordinary bacteria. The first ones were discovered in the 1960s in the hot springs of Yellowstone National Park with water temperatures well above the boiling point, these discoveries have had a profound effect on science suggesting new theories on how life developed here on Earth, and where life can be found on other planets. So this is what I wanted to tell you about exoplanets. I’m sure you heard of exoplanets before, but I hope that after I talked about them this way, you know exactly what we mean by them. And the methods we have to discover these exoplanets. Now, of course, nothing is for certain, but we all have theories, and we’re just trying, and by doing this, we will come to the very next topic in today’s episode, and that has to do with SETI and the question, are we really alone? That’s coming next. Don’t go anywhere. I’ll be right back.

14:58
The 1960

15:00
One conference at the National Radio Astronomy Observatory in Green Bank, West Virginia gathered 11 scientists to talk about the possibility of communicating with extraterrestrials. The conferees eventually summarize their estimates of the number of extraterrestrial civilization in a compact notation that has come to be called the Drake Equation, after Cornell astronomer Frank Drake, one of the organizers of the conference. So what is this Drake equation, the equation estimates that the number of extraterrestrial civilization trying to communicate with us and here of course, I’m not gonna tell you about the equation because honestly, I don’t really understand it myself. It’s kind of complicated, but it takes into account the rate at which suitable new stars are forming the probability that the star will have planets, the number of planets capable of supporting life, the probability that those planets will actually develop life and the probability that life will develop intelligence and also the probability that intelligent life will develop a technology capable of interstellar communication and finally, the length of time that communication one started will continue. So all these factors taken in and put in one equation, which is called the Drake Equation is a useful way to organize our knowledge and our ignorance of course, and it is the basis for search for extraterrestrial intelligence. And that is what we call SETI s. e. T. i The Search for Extraterrestrial Intelligence, you might have thought that we’re talking about a specific planet not not really, that is what SETI stands for Search for Extraterrestrial Intelligence. Now, the greenback attendees and based on the Drake equation came up with the most probable estimate for the number of civilizations possible that could possibly communicate with us of around a million civilizations. The idea of a vast intercommunicating galactic club made up of 1000s of intelligence species entered the public consciousness fueling countless science fiction scenarios. But although the Drake Equation started those possibilities, and started those ideas in science fiction and everything, but the main question remains, where is everybody? Okay, in the beginning, there was modest federal support for SETI programs. But when the searches failed to turn up anything interesting, that source of funding waned. Today the SETI program is being carried forward using private funding. What do you think about the problems involved in the search, you can see why it is taking so long, there are billions of stars out there, and a good proportion of them probably have planetary systems. With each star, you have to follow a slow process, you don’t know what frequency the aliens might be using for their broadcasts. So you slowly move, pausing long enough at each position to see if something interesting is coming through. Today’s SETI searches make use of modern fast electronics to monitor 1000s of stars in 1000s of frequencies at once, as they sort through a mountain of data. The point about SETI though, is that no matter how the search turns out, it’s worth doing. Are there ETS out there. That’s fantastic. Are we alone in the galaxy? Even more fantastic. There aren’t many other kinds of scientific activities with this kind of payoff. But until now, we still have this big question. That is, where is everybody? Now? Yeah, we have estimated according to the Drake equation, that there might be over 1 million possible civilizations trying to communicate with us. But where are they, as far as we know, there’s nobody or nobody tried to contact us, or at least maybe they tried to contact us. But we couldn’t pick up the signal or we didn’t understand that this was a signal, maybe they are not as intelligent as we are, or we are not as intelligent as they are. Or maybe there are some secrets. Maybe there were some interceptions, but they’re being kept in the dark until we figure out what to do with them. Now, of course, I’m not talking about conspiracy theories here. I really hate conspiracy theories. But the point is that it is possible and from a governmental point of view, you may not want to reveal everything, no matter how exciting it might be until you figure out what it means. But anyway, as far as we know, we still haven’t received a single alien message that we can understand at least. And this is all about SETI search for extraterrestrial intelligence. So we’re still talking about the Milky Way. We’re still talking about galaxy. What are we going to talk about next? Well, actually, we’re going to talk about stars in old age. Well, we know that our own star is kind of middle age, right? But what happens to stars in old age, that’s what we’re going to talk about next. So don’t go anywhere. I’ll be right back.

19:44
All stars begin life the same way our son did as a condensing cloud of interstellar dust. From then on, the star is using various means to ward off the eternal inward pull of gravity. We discussed the first of these strategies in the birth of our own Sun.

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It is the initiation of nuclear fusion reactions in the core, which sets up an outward pressure to stop the cloud from collapsing. Almost every star you see is in its hydrogen burning phase, astronomers called a main sequence stars, our Sun has been in this phase for roughly 4.5 billion years. Obviously, hydrogen burning can go on forever. Sooner or later, the hydrogen fuel in the STAR score will run out and the star will have to develop a new way of countering gravity. how long that takes depend on how big the star is, there are two competing effects here. On the one hand, bigger stars have more fuel to start with. On the other hand, bigger stars also generate a stronger gravitational force and have to burn fuel faster to overcome it. It turns out that the second effect winds and the bigger a story is, the shorter the time it can spend burning hydrogen. If you imagine the Milky Way galaxy being a year old, for example, a star like the Sun might have fuel enough for 10 months or so while very large stars might last as little as half an hour. So what will happen to a typical star like our own Sun when the hydrogen in its core runs out. As the nuclear fires start to fade, the pressure that has held off the forces of gravity for billions of years will grow weaker, gravity will take over again. But then the stars interior will heat up again. As it gets denser. Eventually, the temperature of the core will increase to the point where a new kind of nuclear fusion can take place with three helium nuclei coming together to produce a carbon nucleus. This sort of sequence in which the ashes of one nuclear fire becomes the fuel for the next is one of the major features of energy generation in aging stars. In the end four stars up to six times as massive as the Sun, the renewed fusion reactions will increase the stars energy output as well as cause its atmosphere to expand the edge of our Sun, for example, will eventually extend outside the current orbit of Earth because the stars energy is being sent out through a much larger surface. The color of that surface changes from white hot as in the sun today to a cooler read. A star like this is called a red giant stars nine or 10 times more massive than the Sun have enough mass to push the temperature high enough to repeat the process beyond the helium burning stage. When the collapse starts again, they’ll carbon nuclei in the innermost core combined with others to produce heavier elements. This fusion process can continue through the periodic table with the star developing an onion like shell structure as successively heavier elements are created by each collapse. Iron is the end of the line. You can get energy from iron by splitting it or by adding to it. It just builds up in the core of the star like ashes into great of a woodstove setting the stage for one of the most spectacular events in the universe, which is called a supernova. As iron accumulates in the heart of the star nuclear forces cannot keep it from collapsing under the influence of its own gravity. When the mass of the iron core gets to about 40%. More than the mass of the Sun. Gravity can force electrons and protons together to produce neutrons. As each electron disappears, the ability of the remaining electrons to counteract gravity decreases and in a very short time, the core turns into a mass of neutrons that collapses catastrophically as the core implodes the remnants of the onion like envelope of heavy elements that the nuclear reactions have built speed outward in a spectacular explosion. our home galaxy started off billions of years ago as a cloud made up primarily of hydrogen and helium. As large short lift stars were born and became supernovae, heavier elements began to appear. One way to think about the Milky Way then is to picture it as a giant machine constantly taking in primordial hydrogen and churning out the rest of the chemical elements. Our own solar system formed late in the history of the Milky Way, incorporating into its planets and even its life forms the heavy elements made by long dead stars. So what about the properties of a neutron star inside the exploding supernova, the collapsing core is simply a mass of neutrons. Because neutrons have no electrical charge and therefore do not repel each other. There is no radiative force to counter the force of gravity in the heart of the star and the core goes into freefall. This fall stops only when the neutrons are packed so tightly that the court cannot get any smaller. This is known as a neutron star. Because the mass of a neutron star is so concentrated, the force of gravity of the surface is huge. The collapse

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EPS also produces an extremely strong magnetic field. In addition, the rate of rotation of the core increases during the collapse just as an ice skaters rate of spinning Greece’s when she pulls in her arms, some neutron stars rotate at nearly 1000 times a second eight can be that fast, and as the neutron star rotates, it intense magnetic field is swept around in a circle creating electromagnetic waves, the star emits a beam of radio waves that travels outward along the direction of the stars magnetic axis, like a lighthouse beam sweeping around in a circle, the rotating neutron star sends out a radio beam that sweeps through space. If you have a radio receiver in the path of the beam from a rotating neutron star, you will see a burst of radio waves when the magnetic axis points in our direction, followed by a period of no signal, and then another burst, and so on. In 1967, scientists at a radio telescope in England first observed these sorts of regular pulses. And the word pulsar was coined for these objects. Since that first discovery, a couple of 1000 pulsars have been discovered in the Milky Way. Amazing, isn’t it? I mean, you might not be that interested in astronomy, the universe, whatever, but to learn about these things, to learn about the great possibilities out there, and what is really happening. And again, I’m telling you that we know very little of our own planet before talking about the solar system, the Milky Way, or even the universe, which we will definitely talk about in our Beyond Earth series. Even some of these are theories, or even some of these are our own interpretations of what’s happening around us. Maybe they’re not exactly like that, maybe in the years to come, we will figure out that we were wrong in some of our own interpretations. And we will figure out some new ways to really discover life somewhere else in our galaxy, or even in the universe. But until this happens, I will always find this information or any information about the universe, so mind blowing, that I really have to share it with you. And that’s why I created beyond Earth series. And remember today’s episode, we were talking about the Milky Way, and we’re not done yet, we still have a couple of things to talk about. We’re going to talk about black holes, and dark matter. That’s coming next, don’t go anywhere, I’ll be right back.

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There is probably no object in the sky that has been taken up so wholeheartedly in modern fiction and common usage as the black hole. The short definition of a black hole is that it is an object so massive, and so combat that nothing even light itself can escape the gravitational pole. At its surface, we expect that stars that begin life with 30 times the mass of the sun and go through the supernova process will wind up as black holes. The boundary in space that separates the interior of the black hole from the rest of the universe is called the event horizon. And it marks a point of no return. A distant observer watching an object falling into a black hole would see time on the object slow down and stop at the event horizon. An observer on the folding object, however, would see no change in a clock that was traveling with him. And you can see why black hole is actually the fuel of a lot of science fiction. I mean, this time problem is enough to fuel a lot of science fiction stories. So we talked about the black holes what they are, what about finding black holes? How do we find black holes? Astronomers think it likely that all or almost all galaxies have black holes at their centers. But how do you find something you can’t see. But one thing black holes exerts a gravitational force and that can be used to find them. Another way to spot black holes is through radiation from their vicinity. Matter of falling into a black hole tends to bunch up forming what is called an accretion disk collisions into disk heated up which emits energetic radiation. The star Cyrus x, which is a strong X ray source is one of our best candidates for a stellar black hole, we can have no direct knowledge of the interior of a black hole for the simple reason that there is no way for information to get out. Our mathematical models predict that there may be a singularity there a place where the curvature of space time becomes infinite, and the known laws of physics would break down at a singularity. So who knows? Maybe we will figure it out one day, and maybe we will never figure it out. Because until now, we have theories about black holes, but we don’t know exactly what’s in there, because obviously not even light can escape the gravitational pull of a black hole. And black holes, of course, are not the only mysterious phenomena in the universe. We also have dark matter the invisible galactic halo. One of the most startling discoveries of the late 20th century was that ordinary matter the stuff we are made of is just a small part of our universe. Most of the universe consists of something we’ve never seen.

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mean are detected. To understand how this discovery was made, we’ll have to think about how galaxies rotate. Our galaxy, for example, rotates like a giant pinwheel over periods of hundreds of millions of years with our son making a grand circuit every 220 million years or so. One way that astronomers study the structure of galaxies is to look at the details of galactic rotation. The main tool in this study is something called a rotation curve, in which astronomers plot how fast a star is moving as a function of how far away from the galactic circle it lies. stars in the densely populated galactic center locked together by gravity rotate together, this rotation is similar to what you would see on a merry go round. If you are standing near the inside of the platform, you will be moving fairly slowly, but as you move outward to the periphery, you will be whirling around faster and faster. The rotation curve for this situation shows the speed increasing steadily as you get farther away from the center. In the jargon of astronomers. This kind of rotation is called wheel flow, since it is characteristic of any solid rotating object. But as we move outside the galactic core, we find that all the stars are moving at the same speed regardless of how far they are from the center. This is a situation similar to what you see at a track meet where runners on an oval track have to stay in their lanes. Because the runners in the outer lanes have to travel farther, they usually start farther ahead than the runner in the inside lane. If this weren’t done, the runners in the outside lanes would gradually fall back. The same thing holds for the stars in a galaxy. The farther out they are, the more they fall back. Compared to stars closer to the center, you can see this situation manifested in the curved spiral arms of many galaxies. So what happens to the galactic rotation curve when we move still farther out. And here let’s have this little thought experiment. Imagine getting so far away from the galaxy that the whole pinwheel shrinks down to a single faint point of light in the distance. Even out there, the galaxy will exert a small gravitational force on you, so you will still be orbiting that distant point. You would expect though, to be moving very slowly, like the outer planets circling the sun in our solar system, just as Neptune moves much more slowly in its orbit than Earth. Once you are this far away from a galaxy, you would expect the speed of any material out there to get slower the farther away it is. This is called Kepler rotation after the famous astronomer Johann is Kepler who discovered the law for planets in the solar system, which is represented by the downward trending tail of the rotation curve. Yet even here, the stars move at the same rate as inside the galaxy. It was the failure to see this downward trend in Kepler flow that led scientists to the discovery of dark matter. As astronomers traced the rotation curve into the far outskirts of other galaxies, they didn’t see the downturn they expected in the early 1970s. Vera Rubin, who was then a young astronomer at the Carnegie Institution of Washington began using advanced imaging instruments to measure the rotation curves of galaxies. Starting with a nearby Andromeda Galaxy, she was amazed to observe that the curve stayed flat out to the limits of what she could measure, the stars kept moving at the same speed no matter how far they were from the galactic center. Galaxy after Galaxy gave the same result. In 1978, astronomers realized that their expectations about the rotation of galaxies were simply wrong, they determined that the only way to explain the observed rotation of the galaxies was to say that the visible part of a galaxy, the stars, and the dust cloud we’ve been exploring is enclosed in a giant sphere of matter that we cannot see, but whose effects we can observe. The term dark matter was quickly applied to this new material. And that was the story of the discovery of dark matter. But what are the properties of dark matter? No, I’m not saying that we know that for sure. But at least theoretically, whatever dark matter is, it does not emit or absorb light or other electromagnetic radiation, nor does it have any other kind of interaction with ordinary matter except for gravity. The usual tools of the astronomer, optical and radio telescopes, for example, are useless where Dark Matter is concerned. This means that while we can detect dark matter by observing its gravitational effect on luminous matter, for example, the effect it has on the rotation curve, we cannot see it directly. Once the idea of dark matter surfaced evidence for its existence in other venues showed up quickly. For example, there are stellar clusters in which individual stars are moving too fast to be held together by the gravitational attraction of the other

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Stars. In these cases, some extra gravitational omph is needed. And that of course, is what dark matter supplies. Today, astronomers believe that dark matter makes up 23% of the mass of the universe compared to a bit less than 5%. For luminous matter like stars, the rest is another even more elusive category called dark energy that we will talk about in the next episode. But now let’s stick to dark matter. calculations show that for a galaxy like the Milky Way, more than 90% of the galaxies total mass has to be in the same new and unexpected form. So if there is so much of this stuff around what is it theorists have not been slow in producing hypothetical answers to this question. The most popular candidates for the missing matter are as yet undetected objects known as weakly interacting massive particles, or wimps for short. Another class of theories involves something called supersymmetry, these theories predict that they are so called supersymmetric partners for all of the known elementary particles particles that will presumably be seen in accelerator experiments. The theories are interesting, but of course, the only way we’ll know for certain what dark matter is made of is to have someone identify the stuff in a laboratory. Many processes, particularly collisions with cosmic rays can jostle atoms and mass the very faint Dark Matter signal. For this reason, Dark Matter searches tend to be located deep underground in mines or tunnels where the overlying rock provides a shield against this sort of interference. A typical Dark Matter search experiment is located in an abandoned iron mine in northern Minnesota, the mind in the town of Sudan is in the middle of the famous Mesabi range that supplied much of the eye in that built early 20th century America, the mind is now a state park. In a chamber more than 600 meters or 2000 feet beneath the surface, a stack of ultra pure Geranium and silicon wafers is cooled to within a fraction of a degree of absolute zero, scientists hope that a few of the particles in the dark matter wind sweeping through the mind will interact with atoms in the stacks producing vibrations that can be detected by instruments on the crystalline surface. Today, no generally accepted Dark Matter discovery has been made. Although some groups have tantalizing results. This means we are in a position of knowing that 90% of our galaxy is made of some new material, but we don’t know exactly what it is. So my friends, that was what I wanted to share with you about the black hole and dark matter. Now, of course, in today’s episode, we talked about the Milky Way our own galaxy, and our discussion of the dark matter will be the end of today’s episode. Next time we’re going to talk about the universe. So we’re going even bigger, we’re reaching even farther into the universe before we continue our series with a series of interesting questions that are still mysteries of the universe. Or maybe we kind of sold a couple of them, but definitely not all. I hope you enjoyed today’s episode and you learn some new things. Don’t forget that you can find the transcript of this episode on my website English plus podcast.com. And while you’re there, you can explore the many learning opportunities you have on the website. And don’t forget that you can become a Patron if you want not only to support this podcast, but also to get a lot of benefits, including the premium episodes that you can listen to on Patreon, you will have all the links you need in the description of the episode, you can go to the website or you can go to my Patreon page and support me there and support my show. I would like to thank you very much for listening to another episode from English plus podcast and another episode from our series beyond Earth. Don’t forget to learn a new thing every day with English plus podcast and that’ll be everything for today. This is your host Danny, thank you very much for listening. I will see you next time.

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