Nuclear Physics

A possible exponential decay function for this scenario would be P(t) = P0 * (0.5)^(t/50), where P(t) is the amount remaining after time t, P0 is the initial amount, and t is the time passed in years. This formula represents the decay of a substance with a half-life of 50 years.

gamma radiation!

The closest match in my (rather old) reference is K40, with a half life of 1.248x109 years. But precision was lacking in the question.

The decay of an unstable atom by absorbing a wandering positron into the nucleus, converting a neutron into a proton.

One example is how a radioactive form of iodine, 131I, can use positron capture to become xenon, 131Xe. This is a stable, so the conversion is a big help.

The "latest discovery" is, naturally, a moving target. Attempting to keep this space up to date would only duplicate the efforts of NASA and other space agencies around the world to post the latest news on their web sites. In other words, see nasa.gov[http://www.nasa.gov/].

Decay of organisms is primarily caused by the activity of decomposers such as bacteria, fungi, and other microorganisms. These decomposers break down organic matter into simpler substances, releasing nutrients back into the ecosystem. Physical factors such as temperature, moisture, and oxygen levels also play a role in the decay process.

In beta decay, we see one of two things happening. In one case, a proton in an atomic nucleus is converted into a neutron (beta minus decay) and a new element is formed with the ejection of an electron and an antineutrino. In the second case, a neutron in an atomic nucleus is converted into a proton (beta plus decay) and a new element is formed with the ejection of a positron and a nuetrino. If we were to write the formulae for these reactions we'd have to "generalize" them since we won't specify an element. But we can just pick two examples and post them. We see that carbon-14 undergoes beta minus decay to become nitrogen-14 in this equation: 614C => 714N + e- + ve The carbon-14 nucleus has a neutron within it change into a proton Then we see both a beta minus particle, an electron with high kinetic energy, and an antineutrino ejected from the nucleus. When sodium-22 undergoes beta plus decay to become neon-22, it looks like this equation: 1122Na => 1022Ne + e+ + ve The sodium-22 nucleus has a proton within it change into a neutron. We'll then see a beta plus particle, a positron (an antielectron) with high kinetic energy, and a neutrino ejected from the nucleus. That's the long and short of it. Use the link below to learn more about beta decay. It will lead you to, "What is beta decay?" here on WikiAnswers, and it has been answered.

Atomic number becomes two units less and atomic mass four units less.

Bismuth is the answer.

For the most part, yes the quantities of each are different. Light nucleii can have the same number of protons and neutrons and be stable enough to stay the same element (deuterium = 2H, 4He, 6Li , 10B, 12C, 14N, 16O, 20Ne, 24Mg, 28Si, 32S, 36Ar, 40Ca are stable), but a nucleus of a given element can sometimes have more or less neutrons, and be stable. Tin is the heaviest nucleus that has an isotope where #p = #n, and this isotope is very unstable

Yes they are.

Nearly all kinds of electromagnetic radiation are emitted during radioactive decay

Radioactivity is a property of certain elements or substances where they undergo spontaneous decay, emitting radiation in the form of particles or waves. This decay process can result in the release of energy and the transformation of the nucleus of the atom.

Mass deficit is the phenomenon wherein nucleons, the protons and neutrons that are being fused together to make up an atomic nucleus, each give up a little mass. This mass, the so-called mass deficit, is converted into binding energy or nuclear glue to hold the nucleus together. Really! If you guessed that the total mass of an atomic nucleus is less than the sum of the mass of the individual protons and neutrons that make up that nucleus, you'd be correct. Let's look just a bit further.

Remember that protons have a positive charge, and they don't like each other. Like charges repel, and that's a fundamental law of electrostatics. But when each nucleon gives up that aforementioned bit of mass for conversion into nuclear glue, the whole thing works and sticks together. Some say that it is the residual strong interaction (residual strong force) that is responsible for holding an atomic nucleus together, and you can look at it this way if you like. In any case, the situation is easy to see and get a handle on. The concept of mass deficit really is just that simple.

When an atom is in an excited state, it means that its electrons have absorbed energy and moved to higher energy levels. This can happen through processes like absorbing light or collisions with other particles. The electrons do not stay in this state indefinitely and eventually return to their original, lower energy levels by releasing the absorbed energy in the form of photons.

Half-life is used to measure the rate of radioactive decay of a substance. It represents the time required for half of a quantity of a radioactive substance to decay. This information is important in various fields such as nuclear physics, medicine, and archaeology.

NO about 0.99 the speed of light howeaver they are electrons ( or positrons ) so exibit wave properties so there velocity cannot be mesured due to uncirtanty

(4,470 ± 0,020).109 years by alpha decay and (8,20 ± 0,10).1015 years by spontaneous fission.

Nuclear fusion can be either exothermic or endothermic. We're most familiar with the exothermic kind. Fusion in stars releases immense quantities of energy. A fusion nuclear weapon releases enormous energy. But there are situations where fusion is endothermic. We don't usually think of them because of the subtle way they occur. You're wondering what's up, and the answer is in the stars. When a star burns all its energy fusing atoms together, it "hits the wall" at iron. Iron making is the last of the exothermic nuclear fusion reactions. But in stars that have sufficent mass and makeup, those that go supernova, endothermic nuclear fusion is the mechanism by which all the elements heavier than iron are created. It's the only way that they can be created in nature. When the star collapses and that tipping point where the exothermic fusion reactions can't hold it up against its own massive gravity, then it's "go time" and endothermic fusion can occur. The "big squeeze" put on all the matter creates gigantic amounts of heat - enough to drive endothermic fusion. Then the blast distributes all that material across the universe. Including the trans-iron elements created in endothermic fusion reactions during collapse and the nova event.

This is one of those things where the answer depends on what you mean.

The fusion of a deuterium atom and a tritium atom into a helium atom produces about 14.1 million electron volts (MeV). By comparison, the fission of a uranium atom produces about 202 MeV, making a fission event over 14 times as powerful as a fusion event.

But we could looked at it another way. A uranium-238 atom as an atomic mass of about 238, and the 202 MeV come from that mass, providing a yield of about 0.82 MeV per unit mass. By contrast, the 14.1 MeV from one deuterium, with an atomic mass of about 2, and one tritium, with an atomic mass of about 3, so the yield is about 2.8 MeV per unit mass, which makes fusion over 3 times as powerful as fission per mass per event.

If an electron is released from the nucleus (and not from an electron shell) then it would have been emitted by a neutron in beta decay. In beta-minus decay, a neutral neutron emits an electron and an anti-neutrino and becomes a proton; in beta-plus decay, a proton emits a positron and a neutrino and becomes a neutron.

The Terbium isotope found in nature (159Tb) is stable.

Like all elements, Terbium has radioisotopes, of which 33 have been created to date. 158Tb is the most stable of these, with a half-life of 180 years, 157Tb has a 71 year half-life. 160Tb has a half-life of 72.3 days.

Most of the remaining radioisotopes have half-lives that are less measured in seconds, although some have half lives that are measured in days.

After 133.5 days, there will be 0.125 mg of the 2 mg sample of iron-59 remaining. This can be calculated by taking into account each half-life period (44.5 days) and calculating the remaining amount after 3 half-lives (133.5 days).

absorption peak for CO is at ~2142 cm-1...therefore the force constant would be

k=4*pi2*c2*v2*(m1*m2/(m1+m2))

where c is the speed of light in cm/s (2.99792458 x 1010 cm/s)

v is the vibrational frequency in cm-1 (2142 cm-1) and m1 and m2 are the masses of the atoms (m1=0.0120 kg/mol/6.0221415 x1023 1/mol, m2=0.01601 kg/mol/6.0221415 x1023 1/mol)

entering all of this yields k~1854 N/m