Global Climate Report. NOAA National Centers for Environmental Information (http://www.ncdc.noaa.gov). July 2019.

It’s summer, and it is hot out there; but if it feels like record-breaking temperatures are becoming more common globally, they are. The National Oceanic and Atmospheric Administration and European Copernicus Climate Change Service announced that July 2019 was the hottest month across the globe ever measured since measurements began, in 1880. Global temperatures averaged 16.73°C in July, which is 0.95 °C higher than the 20th-century average of 15.78°C . Average Antarctic sea-ice coverage was 8.5% below the 1981-2010 average. And sea ice coverage was 10.5% below the overall average, which is based on records beginning in 1979. The scientists also released geographical data, showing that the regions where temperatures varied furthest from averages, were Alaska, Central Europe, Northern and Southwestern parts of Asia, and certain regions in Africa and Australia. These findings corroborate scientific predictions regarding the effects of man-made climate change. Human activities, primarily from burning fossil fuels, emit carbon dioxide and other greenhouse gases that trap heat in the atmosphere. Increasing greenhouse gas emissions are associated with warmer global surface temperatures. The planet’s 10 hottest years on record have all fallen in the past two decades. Scientists and policymakers around the globe are also feeling this heat.

Unless significant measures to curb greenhouse gas emissions are adopted, scientists expect temperature records to keep falling. Scientists say global temperatures could increase by at least 3°C this century, which will create conditions on Earth that have not been seen in more than 2 million years. Given the notable trends in higher temperatures and natural disasters, we might be pushing the climate system toward states that we haven’t seen in our societal experience – and even in our species’ experience.

Manipulation of brain circuits using smartphone-controlled device

Qazi R et al. Wireless optofluidic brain probes for chronic neuropharmacology and photostimulation. Nature Biomedical Engineering, August 2019.

Scientists recently designed a device that can regulate brain circuits using a tiny brain implant controlled by a smartphone. This bluetooth-enabled device utilizes replaceable lego-like drug cartridges to target neurons with drugs and light. Existing methods to deliver drugs and light to the brain typically involve metal tubes and optical fibers. These tools are rigid and can substantially damage the brain’s soft tissue over time. Moreover, this bulky equipment often limits the patient’s movement because of the wired connections, making them unfit for long-term use. To achieve chronic remote-controlled drug delivery without exhaustion and evaporation of drugs, scientists invented a neural device with a replaceable drug cartridge, which could allow neuroscientists to study the same brain networks for several months without depleting the drug supply. These “plug-n-play” drug cartridges were integrated into a brain implant for mice with a soft and ultrathin probe (about the thickness of a human hair), which consisted of microfluidic channels and tiny LEDs (smaller than a grain of salt), for unlimited drug doses and light delivery. The implant is regulated via a smartphone, allowing researchers to trigger precise combinations and sequences of drug and light delivery. In animal models, these stimuli can be triggered with the target outside of the laboratory, allowing researchers to wirelessly instill changes in the animal’s brain while in its natural habitat. Using these neural devices, researchers are now able to perform fully automated animal studies where the behavior of one animal could positively or negatively affect behavior in other animals by conditional triggering of light and/or drug delivery. This device will allow researchers to better dissect the neural circuit basis of behavior and how specific neuromodulators in the brain tune behavior in various ways. In addition, the device can be utilized in complex pharmacological studies to develop potentially new therapeutics for pain, addiction, and emotional disorders.

The secret weapon of E.Coli 

Melson E. at al. The sRNA DicF integrates oxygen sensing to enhance enterohemorrhagic Escherichia colivirulence via distinctive RNA control mechanisms. Proceedings of the National Academy of Sciences, June 2019.

Scientists have revealed how E. coli (Escherichia coli) bacteria seeks out the most oxygen-free parts of your colon to cause the worst infection possible. E. coli normally live in the intestines of healthy people and animals. Most varieties of E. coli are harmless or cause relatively brief diarrhea. But a few particularly nasty strains can cause cramps, diarrhea, vomiting – even kidney failure and death. Children are particularly at risk. A new study uncovers how this foodborne pathogen knows where and when to begin colonizing the colon on its way to making you sick. Bacterial pathogens typically colonize a specific tissue or organ in the host. Therefore, as part of their infection strategies, bacterial pathogens precisely time deployment of proteins and toxins to these specific colonization niches in the human host. This allows the pathogens to save energy and avoid detection by our immune systems and ultimately cause disease. The researchers in this study identified how E.Coli detects low oxygen levels in the large intestine and then produces proteins that allow it to attach to host cells and establish infection. Oxygen actually diffuses from the intestinal tissue into the gut, and there are comparably higher levels in the small intestine than the large. Remarkably, E. coli specifically waits until it has reached the-low oxygen large intestine before striking. E. coli controls this process via a small form of RNA that activates particular genes when oxygen levels are low. This is the point when the infection really gets established and the bacteria are able to begin to manufacture harmful Shiga toxins. The researchers predict that other bacterial pathogens, such as Shigella and Salmonella, likely utilize a similar control mechanism. Researchers suggest that if we can find a way to block oxygen sensing, we may be able to prevent the infection by allowing E. coli to pass harmlessly through the body.

Futile cycles are described as two opposing biological reactions that take place in a cell at the same time [1, 2]. As a result, futile cycles have seemingly zero net gain for the cell. Actually, because no process is 100 percent efficient, some energy is lost as heat. Thus, these cycles may even cost cells some energy. They were named “futile” cycles because scientists thought that it was wasteful for a cell to operate two exactly opposite processes simultaneously.

One such process occurs in the powerhouses of cells, the mitochondria. Mitochondria are the places where a process called “oxidative phosphorylation” takes place. Oxidative phosphorylation is an efficient way of producing ATP, the cellular energy currency [1]. In this process, high-energy electrons in nutrients are used to generate potential energy, which is in turn used to produce ATP.

Scientists who worked on mitochondrial function were flabbergasted to discover a family of proteins in the mitochondria that had a strange function. These proteins were dissipating the potential energy in the mitochondria before it could be used to produce ATP. They were named “uncoupling proteins” because they were uncoupling the potential energy buildup from ATP production [3]. Scientists couldn’t imagine what these wasteful proteins were doing in our mitochondria. Uncoupling proteins were decreasing the ATP production efficiency of mitochondria. Therefore, they named this process a futile cycle, where electrons from food were used for building up a potential, and an opposing action of uncoupling proteins were dissipating this potential before it could be stored as ATP [4]. This was similar to short-circuiting a battery by connecting two poles with a wire, and just discharging the energy—energy is lost but no work is done. The scientists took this process as a remnant of a random evolutionary process that was left unfinished—“futile,” with no function at all.

It took several years and the work of a different team of biologists to figure out the benefit of these uncoupling proteins [5]. The scientists were working on the differences between wasps and honey bees. One striking difference between these species was in their ability to adapt to colder temperatures: honey bees couldn’t fly and collect pollen when the outside temperature dropped below 10 C (50 F). They had to stay in their beehives to keep warm. On the other hand, wasps could fly around in colder temperatures. The researchers discovered that the main difference that accounted for this phenomenon was that honey bees didn’t have uncoupling proteins in their mitochondria, while wasps did. Therefore, it became apparent that the main function of uncoupling proteins was to generate heat for the body to stay warm during the times when outside temperatures fell. The uncoupling proteins, it seemed, were generating heat while dissipating the potential energy (just like the wire that heats up when you connect two poles of a battery in short circuit). Later on, it was discovered that these proteins had crucial functions in all warm-blooded animals, especially in ones that hibernate during winter.

In this case, an event that initially appeared to be meaningless or even stupid turned out to be indispensible for supporting life under certain circumstances. The fact that we cannot see wisdom behind certain events does not mean they are random or meaningless. Perhaps it is just a matter of time when, in some context, the seemingly futile thing will have a vital role. So the question remains: is there really any such thing as “random” or “futile”?

References

1. Alberts, B., J.H. Wilson, and T. Hunt. 2008. “Molecular Biology of the Cell.” 5th ed. New York: Garland Science. xxxiii, 1601, [90]

2. Available from: http://en.wikipedia.org/wiki/Futile_cycle#cite_note-0.

3. Nedergaard, J., D. Ricquier, and L.P. Kozak. 2005. “Uncoupling Proteins: Current Status and Therapeutic Prospects.” EMBO Rep. 6(10), p. 917–21.

4. Jezek, P. and J. Borecky. 1998. “Mitochondrial Uncoupling protein may participate in futile cycling of pyruvate and other monocarboxylates.” Am J Physiol, 1998. 275(2 Pt 1): p. C496–504.

5. Staples, J.F., E.L. Koen, and T.M. Laverty. 2004. “Futile Cycle Enzymes in the Flight Muscles of North American Bumblebees.” J Exp Biol. 207(Pt 5): p. 749–54.

The sun radiates an enormous amount of energy-at a rate of 3.9×1026 Joule per second. This is roughly equivalent to the energy of a 10 billion megaton TNT bomb every second. This huge amount of energy has been maintained for several billion years and will continue for several more. The fusion reaction of the Sun is a process in which hydrogen burns, transforming into helium, which is then followed by thermonuclear explosions. Isotopes of hydrogen, such as deuterium and tritium, are fused to form heavier helium. During this process the released energy can be as high as 17.6 MeV. The energy released from a 17 lbs deuterium fusion is equal to 1,000 kilotons of TNT. Every second the Sun fuses 675,000,000 tons of hydrogen into 653,000,000 tons of helium.

Scientists have attempted to make fusion work on the earth to make larger amounts of energy, thus solving our energy problems for the future. The first nuclear fusion trials were carried out for nuclear weapons. The released energy from the fusion trials was 500 times higher than that from the fission reactions of nuclear weapons¹. The energy released was equal to that of approximately 12 million tons of TNT. The civilian applications for energy production began in the early 1950s, and we are still trying to solve how to control this amount of energy in reactors.

In nuclear fusion, the negative and positive ions of hydrogen, called plasma, reach temperatures of 100 million degrees. To achieve the plasma parameters of the Sun, for example, the same temperature and density, the plasma must be heated to 100 million degrees Celsius and be kept dense and confined for at least 1 second.

Plasmas are mostly heated by Ohmic (resistive) heating, beam injection, or radio frequency heating. Ohmic heating is the result of an induced current being passed through the plasmas. This mechanism is also used to make electric bulbs and heaters work. Ohmic heating cannot attain plasma temperatures; such heating does not rise above 20-30 million degrees Celsius. When the temperature increases, the resistivity of the plasma decreases. Natural beam injection is one of the mechanisms used to obtain higher energy temperatures. Injecting a high-energy beam of neutral atoms into the plasma causes more collisions and increases the plasma temperature by transferring the atoms’ energy to the plasma. Radio frequency heating is another collision mechanism that increases the plasma temperature. Radio waves generated by oscillators transfer their energy at appropriate frequencies to ions or electrons, thus increasing the plasma temperature. Scientists have managed to get to high enough temperatures; however, these plasmas cannot be contained by the reactor walls easily and the reactions cannot be sustained. To prevent a loss of reaction control and to make the plasmas denser, magnetic confinement mechanisms have been developed such as TOKAMAK, Z-PINCH and ICF.

The TOKAMAK (Toroidal Chamber) device was invented in the late 1950s by the Russian physicists Igor Tam and Andrei Sakharov. In this system, mixtures of deuterium and tritium plasmas, confined by doughnut-shaped magnetic fields, are produced by the toroidal coils, which are then heated to very high temperatures. The temperature achieved by the Princeton Labs is 510 million degrees-almost 30 times greater than the temperature of the Sun. One of the major problems in TOKAMAK is that superconducting magnetic coils are needed for the electricity demand, but the superconducting magnets only operate at cold temperatures. So, a space between the plasma and coils must be maintained to avoid the plasma reaching the coils and damaging them. This mechanism is still assumed to be the best for the confinement of plasmas².

Another confinement system is the Z-pinch (Zeta-Pinch) pulse power device. The current flow of experimental devices is in the Z-axis, so the device was called the Z-pinch by the British scientists in the late 1950s. In this mechanism, very tiny wires, thinner than a human hair, are positioned in different configurations, such as cylindrical or nested geometries, and are then placed in an anode cathode gap.

Applying high voltage on the system causes the energetic plasmas to compress and heat the deuterium or tritium fuel in small pellets. The current flows through these wires axially, generating magnetic fields that confine the plasma. The temperature achieved is about 1.6 billion degrees; this result, reported by the Sandia National Labs, is almost 250 times higher than the interior of the Sun. Z-pinches produce the most powerful plasmas, but the generated plasmas are very unstable³.

Lasers were invented in 1962, and have been applied in many areas. Lasers were used in infusion research to confine the plasma in the late 1960s by scientists at Lawrence Livermore. This laser-based process is called ICF (Inertial Confinement Fusion). In this mechanism, laser light is used to compress and heat the pellet. The temperature achieved is about 100 million degrees Celsius and the plasma is compressed almost 1,000 times its liquid density. However, this confinement occurs in less than in a microsecond, which is not enough time to allow the ions to build on the energy of their own inertia.

Today, many countries have invested millions of dollars in confinement and ignition systems to create fusion power. ITER is an International TOKAMAK fusion project that will be built in France (for more information: http://www.iter.org/). Its participants have agreed to provide funding of $13.1 billion. When it is completed, the ITER will be one of the most expensive scientific projects in the world. However, despite the high cost, there are good reasons why scientists insist on the use of fusion. One of these is that no CO2 is produced during the process. Everyone is aware that CO2 has negative effects; for example, it leads to increased pollution and global warming. Another reason is the abundance of hydrogen available for fusion in seawater and on the earth’s crust. Another important reason is that fusion is safer than fission or other energy sources: There are no nuclear accidents, and in case of malfunction, the plasma is absorbed and cooled by the reactor walls. Also, the generated amount of radioactive particles is fewer than those generated by fission.

If everything goes well, scientists expect that fusion will be used as a source of energy in a couple of decades. If fusion is successful, it can provide clean, safe, reliable, sustainable, and widely applicable energy.

M. Fatih Yilmaz is a graduate researcher at Physics Department, University of Nevada.

Notes

1. Frisch O. R.: “The Discovery of Fission – How It All Began.” Physics Today 20 (1967), 11, pp. 43-48; http://en.wikipedia.org/wiki/Nuclear_fission.

2. http://en.wikipedia.org/wiki/Tokamak; http://www.ppdl.gov.

3. James Glanz, Science 18 July 1997:Vol. 277. no. 5324, p. 306 DOI: 10.1126/science.277.5324.306.

…And We sent down Iron, in which is great might, as well as many benefits for mankind… (Hadid 57:25)

The above verse in the holy Qur’an uses the Arabic expression “anzalna”which means “sent down” for iron. But why? Early commentators understood this as having a metaphorical meaning to explain that iron has been sent to benefit people. But after understanding the nature of one of the most powerful explosions in the universe, you realize that the direct meaning “being physically sent down from the sky” miraculously points out to a very important scientific fact that was discovered only very recently. To understand and appreciate this miracle of the Qur’an, we will first talk about the life and death of stars and then come back to this verse to describe its relevance in detail.

Just like human beings, stars are also born, live, and die. One big difference is that they can live billions of years compared to the less than 100 years of human life. Also, for us, there is no way of knowing how long we will live or how we will die. But for a star, given its mass, you can predict its lifetime and the way it will die. Stars about the size of our sun live for a long time (a couple of billion years) and die gradually. Whereas massive stars with a mass of about 8 times the mass of our sun or more have short lifetimes (tens of million years) and die in a quick and incredibly violent explosion known as a supernova.

Supernova explosions are one of the most spectacular astronomical events observable by human beings. Normally, in a typical galaxy there are about 10 billion stars. A supernova happens to be one of these ordinary stars until it explodes. During the explosion, the amount of energy released by the supernova can exceed the energy of all the other stars combined in its galaxy! The power of this explosion is far too big even to imagine. The energy released is even greater than the total energy our sun will put out during its 10 billion year life!

The brightest supernova of modern times was an extragalactic supernova recorded in 1987. Since it was the first supernova in 1987, it was labeled as “1987A.” This is by far the best studied supernova of all times. In Fig. 1, the left panel shows the region of the sky two weeks after the supernova exploded. The supernova is still very bright. The right panel shows the same region before the explosion, with the arrow indicating the star undergoing the supernova explosion. This particular supernova was 160,000 light years away from us. This means that the actual explosion happened 160,000 years ago, but because it was so far from us, it took 160,000 years for the light rays from the explosion to reach us.

Fig 1. After and before images of the 1987A supernova. The left panel shows the region of the sky two weeks after the 1987A supernova exploded. The supernova is still very bright. The right panel shows the same region before the explosion and the arrow indicates the star undergoing the supernova explosion.

Since the supernova becomes extremely bright, it is even sometimes possible to see it with the naked eye in daytime. In fact, there are historical reports from ancient times concerning supernova explosions. On July 4th, 1054 A.D., Chinese astronomers noticed a “guest star,” which was visible in daylight to the naked eye for 23 days. Its remnant was discovered by the British amateur astronomer John Bevis in 1731. We now know that this bright “guest star” was a supernova. Its remnants, known as the Crab Nebula, are shown in the left panel of Fig. 2. This supernova is one of the very few that have been observed in our Milky Way galaxy. The last supernova to explode in our galaxy was in 1607 (see Fig. 2 right panel).

Supernova explosions are one of the most violent events that happen in the universe. They release an unbelievable amount of energy. But why would a star explode anyway? If it has so much energy still, why does it not remain shining peacefully as it does for most of its lifetime? To answer these questions, we need to remember how stars work.

Figure 2 Supernovae remnants. The left panel shows remnant of the supernova that exploded in 1054. It is about 6,500 light years from earth. It consists of diffuse interstellar gas and dust (nebula) spread in a circular region of a diameter of 6 light years.(Image Credit: FORS Team, 8.2-meter VLT, ESO ). The right panel shows remnants of the last supernova, which exploded in our galaxy in 1604. This combined image — from NASA’s Spitzer Space Telescope, Hubble Space Telescope, and e Chandra X-ray Observatory — unveils a bubble-shaped shroud of gas and dust that is 14 light-years wide and is expanding at 4 million miles per hour (2,000 kilometers per second). It is about 20,000 light years away from us.(Image and caption credit: NASA )/

Let us start by answering a more basic question: What is the energy source of stars? Stars produce their energy through a process called nuclear fusion. The idea is very simple; you fuse together light nuclei, like hydrogen, to produce heavier nuclei, like helium. In this process, the combined mass of low-mass nuclei is more than the resulting fused massive nucleus. This difference in the masses is converted to energy through the Einstein’s famous E=mc2 equation, where E is the energy released, m is the mass difference that is released in the reaction, and c is the speed of light.

But since the nuclei are positively charged, they repel each other, so there must be extremely high densities and temperatures to overcome this barrier. The most common form of fusion that takes place in stars is the fusion of four hydrogen nuclei to produce one helium nucleus. The temperature needs to be about 8 million C0 for this reaction to occur. It requires higher temperatures to fuse nuclei that are heavier than hydrogen. For example, fusing helium requires temperatures higher than 100 million C0.

During most of their lifetime, stars produce energy by fusing hydrogen into helium. After they run out of hydrogen, if the temperatures in their cores are high enough, they start to fuse helium nuclei into carbon and oxygen. And when they run out of helium, they then start to fuse carbon and oxygen. As mentioned above, fusing heavier elements requires extremely high temperatures and high pressures, so it can only happen for massive stars in the late stages of their lives where such conditions are met. For lighter stars like our sun, temperatures are not enough for this.

Even for the massive stars, fusion reactions cannot continue forever. The game of building heavier and heavier elements stops when iron is produced in the core. Iron is a very special element. It has the highest binding energy per nucleon. This makes it the most stable element. You actually lose energy when you fuse iron nuclei together rather than gain energy, so elements heavier than iron cannot be made during these cycles. At this stage of its life, the star looks like an onion, in the sense that it has a layered structure. At the core there is iron, surrounding this core there are layers of lighter elements in the order of their atomic weights, with hydrogen being at the outermost layer (see Fig. 3).

At this point in time, a very delicate balance that holds the star steady becomes unstable. Normally, the gravitational attraction tries to compress everything together. Therefore, the star has a tendency to collapse onto itself due to gravity. This is balanced by the outward radiation and thermal pressure that are generated by intense fusion reactions that are occurring in the core. But when the core turns into iron, fusion can no longer take place. That means there is no longer a supporting outward force that prevents the star from collapsing.

Figure 3 The onion skin model of a supernova. As it gets close to its death, a pre-supernova star has a layered structure that resembles an onion. Heavy elements produced by nuclear fusion inside the star are concentrated toward the center of the star. Iron, being the most stable element, sits at the core.

After the iron core gets to a certain size, this iron core suddenly collapses onto itself. This collapse happens so fast that it takes only a fraction of a second for the initially earth-sized core to shrink to a radius of 60 km. As the core collapses, the outer layers of the star start to collapse and rush in to fill the gap created by the collapsing core. At this point, another drastic event occurs. The iron core cannot compress forever. When the density in the core reaches the nuclear density, it rebounds. This time the core starts to move outward. But wait, the outer layers are still collapsing! When the collapsing envelope of the star meets with the rebounding core, one of the most powerful explosions in the universe occurs. This is known as a supernova explosion, which can be seen millions of light years away!

This gigantic collision ejects the outer layers of the star into the interstellar medium. As a result of the extreme conditions generated by this, the fusion of heavier elements (heavier even than iron) occurs. As the material from the exploding star collides with the interstellar gas and dust, a whole range of light emissions (from visible to X-ray) occurs. Colorful nebulae (as seen in Fig 2.) that will glow for thousands of years are thus generated.

One of the most important outcomes of supernova explosions is that heavy elements, including iron, are ejected into the interstellar medium. In fact, the only source of heavy elements is such events. All the heavy elements that are found in our solar system are made in one of these violent explosions. They cannot be made in our solar system, as they require extremely high temperatures. That means, the carbon that makes our cells, the hemoglobin that carries oxygen in our blood, and basically almost everything in our body are all made of elements produced in these explosions. We are, in the most literate sense, stardust. It is estimated that on average each carbon atom in our body went through four of these cycles in the past.

It is very clear that these explosions are important for the existence of life on earth. But, understanding the mechanism of these events was only possible in recent years.

It is extremely surprising to hear that iron and almost every other element in our body were made during one of these explosions. Even more astonishing is when we look at what the Holy Qur’an says about iron.

In the Holy Qur’an, there is a special chapter about iron, known as “Hadid” or “Iron”. The first thing that surprises you about this chapter is its chapter number: 57. The interesting thing about this is that it matches the atomic weight of one of the isotopes of iron. Iron can have stable isotopes with atomic weights of 54, 56, 57, and 58. The most common form of iron is the one with atomic weight 56 (56Fe).

The reason why this chapter is called “Iron” is the fact that in one verse of this chapter, the Holy Qur’an talks about iron. The second thing that is surprising is the verse number of this particular verse: 25 (or if you count the basmala, it becomes 26). This number (26) is the number of protons in an iron nucleus. And the third numerical code is the total number of verses in this chapter and that is equal to 30. This is equal to the number of neutrons in the most common form of iron nuclei (56Fe). Additional numerical codes can be found through a more detailed inspection of this Qur’anic chapter. No one knew anything about the iron nuclei in the 7th century when the Qur’an was revealed in its present form. And the chance of these numbers being purely coincidental is less than one in a thousand.

After studying these numerical codes, the content of the verse is even more interesting and closely related to our topic. In this verse, the Almighty says: …And We sent down Iron, in which is great might, as well as many benefits for mankind … (57:25). The expression “sent down” used for iron in this verse is the English translation of the Arabic word “anzalna”. This can either be understood as having a metaphorical meaning to explain that iron was given for the benefit of people. But, if the literal meaning, “being physically sent down from the sky,” is considered, we realize that this verse miraculously indicates the scientific fact that all the iron in our solar system came from the sky from supernova explosions.

Another interesting aspect is the fact that the verse says “…in which is great might …” The Arabic word “shaded” used to describe this can also be translated as “in which is great power” or as “in which is great violence”. If you assume this phrase is referring to iron, you can understand it to mean that iron has a great strength. Or a deeper meaning would be to consider the fact that iron nuclei is the most stable nuclei, i.e. the fact that it has the highest binding energy per nucleon. If you consider this phrase as referring to the act of sending down, in that case it reminds you of the great violence in supernova explosions.

In summary, supernova explosions are the violent deaths of massive stars. The course of events that leads to these gigantic explosions, as well as their far reaching consequences, is very interesting. They are the only source of iron and other heavy metals found in our solar system. They show the mercy of God, as life on earth without them would not be possible. At the same time, they can be thought of as an incredible show of divine power. As the Holy Qur’an says at the end of the verse that mentions iron:

Surely God is the All-Strong, the All-Glorious with irresistible might. (Hadid 57:25)

The Anglo-Australian Observatory (http://www.aao.gov.au/)

http://antwrp.gsfc.nasa.gov/apod/ap030914.html

http://www.nasa.gov/multimedia/imagegallery/image_feature_219.html

For more detailed discussion, see for example: Adam Burrows, Nature 403 (6771), 727 (2000).

http://chandra.harvard.edu/resources/illustrations/superPre.html

For example, according to numerological (abjad) calculations, the abjad of the word “Al-Hadeed” in Arabic, when the numerological values of its letters are added up is also 57 and numerological value of the word “Hadid” alone is 26. ( http://www.miraclesofthequran.com/scientific_30.html )