Astronomical Glossary
Stark broadening is proportional to the ion and electron density in a plasma and is a good indicator of atmospheric pressure in a stellar atmosphere and hence of the star's luminosity. The simplest predictions of superstring theory concern processes at the Planck energy, and so far very little is known about the consequences of string theory at lower energies
This change in temperature happens in a large amount across the radiative zone, where the temperature falls from about 7 million degrees to 2 million degrees. With this outer layer, it has a chance to radiate away into space and so its not quite as hot, not quite as intense as the rest of the Sun? Pamela: The temperature structure of the Sun changes radically as you go from the centre to the outer layers
Solar System Introduction
These stars then spew this material out through various mechanisms such as stellar winds, planetary nebula phases, and the ultimate littering of the galaxy, supernova explosions. What is in the Solar System? - pretty much everything found around the Sun, which includes the Sun, planets, satellites (moons), asteroids, comets and anything else that is the area (dust and debris is pretty much all that remains)
It is possible to turn that last statement into a scientific principle: The fact of our being restricts the characteristics of the kind of environment in which we find ourselves. Planets of all sorts exist, and obviously, when the beings on a planet that supports life examine the world around them, they are bound to find that their environment satisfies the conditions they require to exist
The charged particles carried by solar winds also interfere with satellites, power lines, and other technology on Earth as well as causing the aurora borealis. However, the solar winds carry out the charged material to the edge of the Solar System where it forms a magnetic field that prevents other interplanetary material from getting in
Stellar Evolution
The slow squeezing process seems to have solved the energy problems of the Sun, right? A little more helium causes the energy production region to be slowly pushed out from the center - so everything is just fine, right? Not really, since the Sun (and stars like it) can only do this for so long. For these larger mass stars carbon would burn next, and then heavier elements after carbon, but only if the star is massive enough to raise the temperature and density to the high levels required for the fusion of these heavier elements
WebElements Periodic Table of the Elements
The evolution of chemistry's periodic table into the current form is an astonishing achievement with major contributions from many famous chemists and other eminent scientists
The evolution of high-mass stars on the HR diagram is quite different from that of low-mass stars: they always remain very luminous, but their outer layers can switch from hot to cool several times as the reactions in their interiors change. what is the apparent magnitude of Barnard's Star? what is the distance to Barnard's Star? what is the absolute magnitude of Barnard's Star? what is the luminosity of Barnard's Star? if Barnard's star were pure hydrogen at birth, and maintained its current luminosity, roughly how long could it remain on the main sequence? Use its initial mass, its luminosity, and the efficiency of hydrogen fusion to make your estimate
But you also make a lot of heavier elements, like Carbon, Oxygen, and Nitrogen, and sometimes Silicon, Neon, and sometimes even Iron, Cobalt, and Nickel. Fortunately that people who sadly are overweight and also suffering from various diseases can help to eliminate the severity of the illnesses by simply losing weight
Reply Cameron Reed Posted November 4, 2014 at 6:15 PM Well how do you know that the big bang theory is correct you can say you have proof but you do not have a reliable source if so. Reply Cameron Reed Posted November 4, 2014 at 6:21 PM Well how do you know that the big bang theory is correct you can say you have proof but you do not have a reliable source if so
StarsIntro
Brightness and distance In the second century BC, the Greek astronomer Hipparchus divided the stars into six brightness groups called magnitudes (now apparent visual magnitudes (m or V), first magnitude the brightest, sixth the faintest. In our part of the Galaxy there is on the average only about one atom of gas per cubic centimeter and one grain of dust per cubic meter, but volumes are so large that the ISM constitutes more than 10 percent of the Galaxy's mass
Case Study: The Natural Abundance of Elements - Chemwiki
Indeed, this process called the solar nebula theory has validity because we are able to see distantly forming solar systems with a dim central protostar surrounded by gas. Sign In Forgot Password Register username password If you like us, please share us on social media, tell your friends, tell your professor or consider building or adopting a Wikitext for your course
Most of the universe is hydrogen; the only reason hydrogen (and helium) are rare in the inner solar system is that these light gases were blown away in the early stages of the solar system via radiation pressure and the solar wind. If a planetesimal forms on one side of the solar nebula, and another planetesimal forms on the other, unless the bodies happen to be exactly the same distance from the Sun, the difference in rotation speeds will guarantee that eventually the bodies will catch up to each other
Helium has two protons and so is number 2, and so on all the way up to uranium, which, with 92 protons in its nucleus, is the heaviest of the "naturally occurring" elements. Everything else, every other chemical element, including carbon, oxygen, nitrogen, and all the other elements essential for your life, is thought to have been fabricated in stars
So - to summarize, your question has two parts: the abundance of iron and silicon is greater than the heavier elements in the universe in general, and the earth is at the right distance from the Sun so that when it condensed out of the solar nebula, the ligher elements were either bound up in compounds or blown away to the farther reaches of the solar system.Click Here to return to the search form. Back to the early solar nebula: In the center of this swirling gas cloud, or nebula, the density and temperature got high enough for a star to form and begin thermonuclear reactions in its core and shine
The Outer Planets: How Planets Form
This makes sense, since the outer planets all have many moons and rings that orbit in the same plane, just like the planets in our solar system orbit the Sun in the same plane. How did the terrestrial planets form? After the heavier elements and minerals condensed into solid bits of rock, they all orbited the Sun at about the same speed
These compounds arrived in the inner planets after their initial formation, most likely brought by impacts of planetesimals formed in the outskirts of the solar system (Q: What was Jupiter's role in bringing water to Earth?). Formation of moon systems As the early jovian planets captured large amounts of gas, the same process that formed the solar nebula -- contraction, spinning, flattening and heating -- formed similar but smaller disks of material around these planets
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