Now, what we could imagine is a highly magnetic object acting as a particle accelerator and also banding the paths of released particles - not dissimilar to a mass spectrometer on earth.Tags: Professional Essay Writing UkGood Vs Evil EssaysBusiness Plan And StrategyManagement Topics For Research PaperUniversity Of Edinburgh Creative WritingPhoto Essay On PovertyHow To Write An Empathy Essay
Our new planet drifts out into the fluorine rich part of the disk and begins gathering it due to its gravity.
The planet has a surface rich in nickel and iron with much fewer silicates than earth.
The whole system falls into a disk around the supernova remnant.
Planets start forming during your standard process: accretion.
Firstly, fluorine is not particularly abundant in the universe so you need a large source in order to get an atmosphere of it.
Additionally, fluorine is easily consumed in stellar nucleosynthesis so it's hard to encounter a significant concentration for your planet forming. In a Red Giant star at the end of its life, it's inside is stratified with different layers of fusion occurring.The silicates burn and react and form their own layers or there is not enough silicate to react with the fluorine.As such the planet is able to keep a fluorine atmosphere for a geological period of time.The Star Dies in a core collapse supernova or Type II blasting its layers outward and releasing a ridiculous amount of neutrinos. Now the outflow of neutrino radiation is so great that it be enough to knock a proton off Neon or Neutron to make Neon-19 which decays into fluorine. The result is an expanding fluorine rich shell of gas.For the sake of argument, let's say there is a whole bunch of it.Our interpretation of the observations, with the use of radiative transfer calculations, indicates that both HF and HCl are formed in the inner regions of the envelope close to the AGB star.Thermochemical equilibrium calculations predict HF and HCl to be the major reservoirs of fluorine and chlorine in the atmospheres of AGB stars.We report the detection of emission in the J = 1−0 rotational transition of hydrogen fluoride (HF), together with observations of the J = 1−0 to J = 3−2 rotational lines of H35Cl and H37Cl, towards the envelope of the carbon star IRC 10216.High-sensitivity, high-spectral resolution observations have been carried out with the HIFI instrument on board Herschel, allowing us to resolve the line profiles and providing insights into the spatial distribution of the emission.As the planet begins to gather fluorine the surface burns.But the metal rich surface reacts with the fluorine and produces a nonreactive passive layer.