© 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 It might be outdated, but the numbers look like the ISM is more dense than the heliosphere.
  • http://web.mit.edu/space/www/helio.review/axford.suess.html
• 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.

 

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