<?php   /* Code © Charles Chandler http://qdl.scs-inc.us/?top=11566 */   /* Prialnik, D., 2000: An Introduction to the Theory of Stellar Structure and Evolution. Cambridge University Press Williams, J. P.; Blitz, L.; McKee, C. F., 1999: The Structure and Evolution of Molecular Clouds: from Clumps to Cores to the IMF. arXiv:astro-ph Richardson, J. D.: The Solar Wind: Probing the Heliosphere with Multiple Spacecraft   gmc = giant molecular cloud dp_ = dusty plasma */   // Some of the values are pulled from tables in QDL posts. The LU() // function retrieves values, given the post ID and the value name. $coDataPgID = 8906; $solarFacts = 4798;   // I'm getting two different densities here, depending on which numbers // I use. I "think" that the "100 particles per cm^3" is probably more // accurate, so I should go with that. Where they said that GMCs can be // up to 6 million solar masses, that was an upper limit, not an average. // But that produces much higher temperatures, and thus total energies. // Of course, that will relax the requirement for kinetic energy. $v['solarMass' ] = LU($solarFacts, 'solar mass'); // kg $v['solarRadius' ] = LU($solarFacts, 'solar radius'); $v['solarVolume' ] = VolumeOfSphere($v['solarRadius']); $v['deuteronMolarMass'] = LU($coDataPgID, 'deuteron molar mass'); // kg/mol $v['molarGasConstant' ] = LU($coDataPgID, 'molar gas constant'); //$v['gmcRadius' ] = (9.5 / 2) * pow(10, 14) * 1000; // radius of gmc, in m //$v['gmcVolume' ] = VolumeOfSphere($v['gmcRadius']); // volume of gmc, in m^3 $v['dp_density' ] = 100 * 1.672621777e-27 * 2 * 1e6; // 100 particles of diatomic hydrogen per cc $v['dp_volume' ] = $v['solarMass'] / $v['dp_density']; // volume, as mass / (mass/vol) if (0) { $v['gmcMass' ] = 6000000; // mass of gmc, in solar masses $v['dp_volume' ] = $v['gmcVolume'] / $v['gmcMass']; // volume to produce 1 Sun, in m^3 $v['dp_density' ] = $v['solarMass'] / $v['dp_volume']; } $v['dp_temperature' ] = 10;   // Find the pressure of the dusty plasma, // assuming that it is all diatomic hydrogen, // with the same molar mass as a deuteron. // P = (rho * R * T) / M $v['dp_pressure' ] = ($v['dp_density' ] * $v['molarGasConstant'] * $v['dp_temperature']) / $v['deuteronMolarMass'];   // From this we can get a constant. // PV^(7/5) $v['const PV^(7/5)' ] = $v['dp_pressure'] * pow($v['dp_volume'], 7/5);   // Now we find the expected pressure after compression into the volume of the Sun. // P = adiabatic constant / new volume $v['sun_pressure' ] = $v['const PV^(7/5)'] / pow($v['solarVolume'], 7/5);   // Then we can find the expected temperature in kelvins. // constant = PV / T $v['const PV/T' ] = ($v['dp_pressure'] * $v['dp_volume']) / $v['dp_temperature']; // Now the end T = PV / constant $v['sun_temperature' ] = ($v['sun_pressure'] * $v['solarVolume']) / $v['const PV/T'];   // Find the joules if the specific heat capacity // was that of a 75/25 mix of hydrogen and helium. $v['energy_heat_1' ] = $v['solarMass'] * $v['sun_temperature'] * 12026.25;   ?>