New data!

Howdy! So this past week Dr. Hassel and I have been dealing with a little problem: The Siena High Performance Computing Cluster was down for a while! The cluster, which allows us to run complex calculations at times that would be impossible for a single computer or even for a few computers, was not working for a small amount of time but we just had to wait for it to get back up and running again! Once it started to work again, all was well and we were able to run some brand new simulations. In this blog post, I will show a few different graphs that we were able to produce and explain their importance! The first pair of graphs that I will show pertains to H2. Each of the molecules I will illustrate has two phases: the gas and ice phase. Since we are simulating the likelihood that these elements will form on a dust grain particle, we have to take into account that likelihood in both the gas and ice phases of its stellar evolution. I will be presenting 20 separate graphs in my presentation on April 1st! The molecules that are directly affected by the change in the binding energies are: O2, H2, N2, CH4, and CO. Then we have molecules that are only indirectly changed by the binding energy differences, which are H2O and NH3. Some of these molecules are affected greatly by the new binding energies and some are not affected in both the gas and solid phases, but each of these molecules are affected in at least one phase. HCOOH, NH2OH, and NH2CHO are the biomolecules that we also examined through our codes, which can provide more access into amino acid precursor formation in the earliest rungs of the space time continuum.

Thanks for reading this post and my next post (hopefully) will be all about the Rochester symposium!