Notes & Considerations on Proposal for Astrosphere Catalog and Baseline Model for Comparison and Reference over Time
The proposition of a catalog for comparing diverse astropause and astrosphere modeling equations and methods is outlined and examined. Sound method is found possible, and good reason is found for the generation for such a catalog.
Throughout the field of astrophysics, there lacks a consistency on estimating astropause and astrosphere distances (for brevity’s sake both will be referred to as astrosphere for the remainder of this paper). The equations for the estimates themselves differ, and even when the equations are sympathetic, the values assumed and applied differ. As an example, the solar system had been given a range of estimates from at least 74 AU to 150 AU until Voyager 1 reported 121.7 AU. With other systems, we are in absence of Voyager records and we cannot simply await similar probes for validation. Presently, there are many factors that cause these differences. A few examples to convey the concept of difference are: one equation working off of mass-loss rate and negating wind speed, another equation factoring in ISM cloud considerations differently, or another factoring in electromagnetic considerations where others do not. There is no simple solution to these problems as the current period of exploration will naturally generate dissimilar approaches and solutions. Further, there is currently no convenient means to find and compare multiple approaches against each other to attempt to discern definition and pattern. What could be created is a catalog which has a steady and predictable line which estimates could be compared against and kept on file. This would allow estimates to be made and plotted against a predicted model which does not suppose itself to be dependent upon real factors and variables within the equation, but instead works inversely from sample to produce an “ideal” model by which estimates can be lined up against. The reason for doing so would allow for estimates to be examined in long view against a trend and pattern with a known skeleton model from which they deviate, as opposed to now where estimates are aligned and compared against nothing and we have a lack of direction or focus as to the culmination of these estimates being generated.
The Hunt catalog is comprised of the baseline, sample estimates, and profiles of those estimates defined by the differences between the estimates and the baseline. What follows are the components to assembling and then employing the Hunt line catalog for an example.
In this paper a variable is created for application as outlined. This value is given a name of “Hunt” variable, and al subsequently derived productions from the employment of the Hunt variable adopt the name “Hunt” (e.g. “Hunt line”). The Hunt variable is considered adjustable as this value is a result of the data’s average being applied as a value for approximation in equations outlined later. For clarity, the Hunt variable is given a symbol H. It is referred to as “Hunt” since it is employed to approximate a finding of an unknown radius given the related radius opposite of the one approximated. The Hunt variable implies a direct correlation between the two radii proportionately. The results of employing the Hunt variable are only considered an approximation because the Hunt variable is only a value from an average from the data collected so far and as such is not specific to a particular object’s constituency or definition. No application of the Hunt variable should ever be found to be applied in place of typical models and methods. The purpose and application of the Hunt variable are confined to the operations and functions defined within this paper.
Due to the limited quantity of verifiable star astrospheres, the initial Hunt baseline is built from atoms and a few stars. This was done because the atomic data is more readily available in high quantity and good record. Atoms divide the radius of their nucle