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What is the temperature called at which the second virial coefficient of a real gas is zero?
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∙ 14y ago
Boyle temperature
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∙ 14y ago
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Can you give a sentence using the word coefficient?
The 8 in 8x is the coefficient.They should be familiar with the series expressions for the virial coefficients for a lennard-jones potential.
Is aids caused by a virial infection?
Yes. The pathogen that causes AIDS is a virus called HIV.
Are virial infections contagious?
Virus infections are contagious - like the flu, the common cold, viral pneumonia, and so on.
What 5 physical properties that can be used when telling things apart?
Obviously there are lots more than five you could use, and it would depend on what kind of things they are, but maybe: 0. Temperature of any phase transitions (eg melting, boiling), but this might not be convenient to measure For comparing two solids: 1. Density 2. Heat capacity 3. Young's modulus 4. Electrical conductivity 5. Poisson's ratio For comparing two liquids: 1. Density 2. Heat capacity 3. Viscosity 4. Surface tension 5. Sound speed For comparing two gases: 1. Density (at some fixed pressure) 2. Heat capacity (not a great one if they're both close to ideal though) 3. Absorption spectrum 4. First virial coefficient 5. Breakdown electric field
Why temperature increases when a gas is compressed?
In a first attempt (please note that it is only an approximation) you can consider the law of ideal gases which sayspV = nRTwhere p is the pressure, V the volume, nthe number of moles, R is a constant and T the temperature.So you can see thatT = p · V/(nR)If V/(nR) is a constant, you can see immediately that the higher the pressure the higher the temperature (they are proportional magnitudes).If you want a deeper understand, you have to know that the kinetic theory of pressure establishes a direct relationship between pressure and speed (in an informal way, pressure is a consequence of collisions between gas particles and the walls in which they are confined). So the higher the speed the higher the pressure.In addition to this, the speed is related to the temperature across the virial theorem, which establishes that T is proportional to the speed squared.So, as we showed in the firsts lines, an increment in the pressure cause an increment in the speed and, consequently, an increment in the temperature.
Under what conditions do the gas laws deviate and give best results?
The ideal gas equation is derived for non-interacting, classical particles. Particles don't interact when they are far away, so it applies best to very low density gases. But it's a very good approximation in a wide range of circumstances, eg air at room temperature, the hydrogen in stars and nebulae etc. In general, we express classical deviations from ideal gas behaviour using the virial coefficients Bn: p/(k_B*T) = n + B1(T)*n^2 + B2(T)*n^3... where n is the particle density of the gas, p is the pressure, k_B is Boltzmann's constant and T is the temperature. Ideal gas behaviour is when all the terms on the right hand side apart from n are very small. If the density is still fairly low though, we only need to worry about B1. It turns out that at a certain temperature, called the Boyle temperature, B1=0 and so the gas behaves ideally at higher densities. If T is higher than this B1 is positive and if T is lower than B1 is negative. We might also need to worry about quantum mechanical effects. These become significant if the de Broglie wavlength of the particle approaches the inter-particle spacing. Basically this means light particles at very low temperature, for instance superfluid helium.
What has the author Trygve Braatoey written?
Trygg Engen has written: 'Odor sensation and memory' -- subject(s): Smell disorders, Psychophysics, Smell, Odors 'Feasibility of olfactory coding of noxious substances to assure aversive responses in young children' -- subject(s): Odors, Hazardous substances, Prevention, Home accidents
Are there hydrogen bonds between molecules in steam?
Water is a polar substance. In liquid water, this gives rise to hydrogen bonds between molecules, making it structurally more compact. However when water is heated up to steam, those hydrogen bonds break up and the molecules cannot be maintained globally as aggregates. The forces in play in steam are of collisional type and the polarity of the molecules does result in short-range attractive forces yielding negative second virial coefficients but in no way the molecules arrange themselves to conform to a hydrogen-bonded structure. The probability of simultaneous collision between several molecules though rare in steam may become important at high pressures below the critical point, but should not be confused with the structuration between neighbouring molecules in liquid water where hydrogen bonding takes place due to the closeness between water molecules. What is sure is that there is no hydrogen bonds above the critical point of steam. In steam hydrogen bonding is just not taking place for the molecules are too distant from each other. Collisional binary encounter does not generate hydrogen bonding!!!
Can galaxies die?
We have not been around long enough to find out, but the only viable proposal to emerge so far is the Minkowski/Jackson/Whiffen model of recycling and evolution. This invokes active galactic nucleus (AGN) accretion (SMBH) and re-ionization of matter, which is re-emitted in quasar 'gas flows' or relativistic jets (Look up M87 or Centaurus A). Which then form new open spiral galaxies due to the intrinsic rotation of bodies in space to a virial radius. This is evidenced by the massive population peak of quasars at z= ~1.7, a few Billion years ago, coinciding closely with the age of the sun and older stars in the Milky Way, (and of course the lack of galaxies full of dead stars) and apparent correlation with the re-ionization of all below hydrogen. Such models are very unlikely to become part of mainstream science as irrefutable evidence is difficult to find and then change views with. no a galaxy cannot die rather it gets deteriorated bcoz of the expansion of the universe
What observation supports the Kinetic Molecular Theory of Heat?
Heat transfer is the process whereby heat is transferred from one medium to another. for example in a PWR power plant, heat is transferred from the primary circuit to the secondary circuit in a form of heat exchanger, which is basically a matrix of tubes. In this case heat is transferred from hot water at high pressure to water/steam at a lower pressure. In your car radiator heat is transferred from the engine coolant water to the ambient air. For design purposes engineers want to know how much heat can be transferred in a heat exchanger of a certain design, so they use a heat transfer coefficient which simply says how much heat will be transferred per second per degree temperature difference, for the physical arrangement involved. Kinetic energy is the energy possessed by a moving body. If its mass is M kg and speed V meters/sec, its kinetic energy is 1/2 x M x V2 Joules
Is a cloud an example of gas to liquid?
becaues they are a part of the atmospheFrom Wikipedia, the free encyclopediaJump to: navigation, searchSee also: Solar nebulait looks like its stiking its middle fingerWithin a few million years the light from bright stars will have boiled away this molecular cloud of gas and dust. The cloud has broken off from the Carina Nebula. Newly formed stars are visible nearby, their images reddened by blue light being preferentially scattered by the pervasive dust. This image spans about two light-years and was taken by the orbiting Hubble Space Telescope in 1999.A molecular cloud, sometimes called a stellar nursery if star formation is occurring within, is a type of interstellar cloud whose density and size permits the formation of molecules, most commonly molecular hydrogen (H2).Molecular hydrogen is difficult to detect by infrared and radio observations, so the molecule most often used to determine the presence of H2 is CO (carbon monoxide). The ratio between CO luminosity and H2 mass is thought to be constant, although there are reasons to doubt this assumption in observations of some other galaxies.[1]Contents1 Occurrence2 Types of molecular cloud 2.1 Giant molecular clouds (GMCs)2.2 Small molecular clouds2.3 High-latitude diffuse molecular clouds3 Processes 3.1 Star formation3.2 Physics4 References5 See alsoOccurrenceBarnard 68 Within our own galaxy, molecular gas accounts for less than one percent of the volume of the interstellar medium (ISM), yet it is also the densest part of the medium comprising roughly one-half of the total gas mass interior to the Sun's galactic orbit. The bulk of the molecular gas is contained in a molecular ring between 3.5 to 7.5 kiloparsecs from the center of the galaxy (the Sun is about 8.5 kiloparsecs from the center).[2] Large scale carbon monoxide maps of the galaxy show that the position of this gas correlates with the spiral arms of the galaxy.[3] That molecular gas occurs predominantly in the spiral arms argues that molecular clouds must form and dissociate on a timescale shorter than 10 million years-the time it takes for material to pass through the arm region.[4]Vertically, the molecular gas inhabits the narrow midplane of the Galactic disc with a characteristic scale height, Z, of approximately 50-75 parsec, much thinner than the warm atomic (Z=130-400 pc) and warm ionized (Z=1000 pc) gaseous components of the ISM.[5] The exception to the ionized gas distribution are HII regions which are bubbles of hot ionized gas created in molecular clouds by the intense radiation given off by young massive stars and as such they have approximately the same vertical distribution as the molecular gas.This smooth distribution of molecular gas is averaged out over large distances; however, the small scale distribution of the gas is highly irregular with most of it concentrated in discrete clouds and cloud complexes.[2]Types of molecular cloudGiant molecular clouds (GMCs)Vast assemblages of molecular gas with masses of 104-106 times the mass of the Sun are called giant molecular clouds (GMC). The clouds can reach tens of parsecs in diameter and have an average density of 102-103 particles per cubic centimetre (the average density in the solar vicinity is one particle per cubic centimetre). Substructure within these clouds is a complex pattern of filaments, sheets, bubbles, and irregular clumps.[4] A GMC contains 100,000 to 10,000,000 times as much mass as the Sun by virtue of its size: 50 to 300 light-years across.[citation needed] The densest parts of the filaments and clumps are called "molecular cores", whilst the densest molecular cores are, unsurprisingly, called "dense molecular cores" and have densities in excess of 104-106 particles per cubic centimeter. Observationally molecular cores are traced with carbon monoxide and dense cores are traced with ammonia. The concentration of dust within molecular cores is normally sufficient to block light from background stars so that they appear in silhouette as dark nebulae.[6]GMCs are so large that "local" ones can cover a significant fraction of a constellation; thus they are often referred to by the name of that constellation, e.g. the Orion Molecular Cloud (OMC) or the Taurus Molecular Cloud (TMC). These local GMCs are arrayed in a ring in the neighborhood of the Sun coinciding with the Gould Belt.[7] The most massive collection of molecular clouds in the galaxy forms an asymmetrical ring around the galactic center at a radius of 120 parsecs; the largest component of this ring is the Sagittarius B2 complex. The Sagittarius region is chemically rich and is often used as an exemplar by astronomers searching for new molecules in interstellar space.[8]Small molecular cloudsMain article: Bok globule Isolated gravitationally bound small molecular clouds with masses less than a few hundred times the mass of the Sun are called Bok globules. The densest parts of small molecular clouds are equivalent to the molecular cores found in GMCs and are often included in the same studies.High-latitude diffuse molecular cloudsMain article: Infrared cirrus In 1984 IRAS identified a new type of diffuse molecular cloud.[9] These were diffuse filamentary clouds that are visible at high galactic latitudes (looking out of the plane of the galactic disc). These clouds would have a typical density of 30 particles per cubic centimeter.[10]ProcessesStar formationMain article: Star formation Composite image showing young stars in and around molecular cloud Cepheus B.The general hypothesis is that the creation of newborn stars occurs exclusively within molecular clouds. This is a natural consequence of their low temperatures and high densities, since the gravitational force acting to collapse the cloud may exceed the internal pressures that are acting "outward" to prevent a collapse. Also there is observed evidence that the large, star-forming clouds are confined to a large degree by their own gravity (like stars, planets, and galaxies) rather than external pressure (like clouds in the sky). The evidence comes from the fact that the "turbulent" velocities inferred from CO linewidth scale in the same manner as the orbital velocity (a virial relation).PhysicsThe physics of molecular clouds are poorly understood and much debated. Their internal motions are governed by turbulence in a cold, magnetized gas, for which the turbulent motions are highly supersonic but comparable to the speeds of magnetic disturbances. This state is thought to lose energy rapidly, requiring either an overall collapse or a steady reinjection of energy. At the same time, the clouds are known to be disrupted by some process-most likely the effects of massive stars-before a significant fraction of their mass has become stars. Molecular clouds, and especially "giant" molecular clouds (GMCs), are often the home of astronomical masers
