© Charles Chandler
This page is for ongoing projects related to this model.
  • Synoptic Stellar Energy Budget
    • From Wikipedia:
      • In the dense nebulae where stars are produced, much of the hydrogen is in the molecular (H2) form, so these nebulae are called molecular clouds.1 The largest such formations, called giant molecular clouds, have typical densities of 100 particles per cm3, diameters of 100 light-years (9.50 × 1014 km), masses of up to 6 million solar masses,2 and an average interior temperature of 10 K.
      • I "think" that the density, as stated, is going to be more reliable than just going with the GMC volume and dividing it by 6 million (which sounds like a high-end number, not an average). Then see what that does to the rest of the calcs.
    • I need to subtract for the amount of thermal energy expelled into the heliosphere.
    • The following link has info on the interstellar medium. It might be outdated, but the numbers look like the ISM is more dense than the heliosphere.
    • I'm saying that all of the excess thermal energy has been converted into electrostatic potential. It sounds like there might be a way of quantifying that potential just from the energy budget. Then, is there a way of determining the strength of the E-fields, on the basis of the total electrostatic potential? And can that be compared to Stark Effect data, such as from IRIS?
    • Would it be possible to compare the hydrostatic pressure of the imploding dusty plasma to the electrostatic attraction once all of the matter becomes fully ionized?
  • Generate simulations for the various EM configurations that are central to this thesis.
  • The Task Report finds everything using the AstroTasks prototype.



1. Prialnik, D. (2000): An Introduction to the Theory of Stellar Structure and Evolution. Cambridge University Press

2. 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: 9902246

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