Kemijski sastav Sunca i njegove atmosfere

undergraduate thesis

• Title (english): Chemical composition of the Sun and Its atmosphere
• Author: Lukas Ištef
• Mentor: Vladimir Dananić (mentor)
• Committee member: Vladimir Dananić (predsjednik povjerenstva)
• Committee member: Igor Sutlović (član povjerenstva)
• Committee member: Veljko Filipan (član povjerenstva)
• Granter: University of Zagreb; Faculty of Chemical Engineering and Technology; Zagreb
• Defense date and country: 2021-09-20, Croatia
• Scientific / art field, discipline and subdiscipline: NATURAL SCIENCES; Physics

Abstract

Kemijski sastav Sunca predstavlja temelj astronomije. Njegovo poznavanje uvelike nam pomaže u shvaćanju Sunčeve unutrašnjosti, evolucije i općenito čitavog solarnog sustava jer su sva kozmička tijela u suštini jednakog kemijskog sastava. Metode koje se u ovu svrhu koriste i koje će u ovome radu biti opisane su solarna (apsorpcijska) spektroskopija te masena spektroskopija primitivnih meteorita. Apsorpcijskom spektroskopijom Sunčeve svjetlosti dobiva se određeni spektar prepun apsorpcijskih linija. Svaki pojedini element, odnosno njegov atom ima svoj karakterističan “otisak” u dobivenom spektru. Spektar atoma određenog elementa prikaz je njegove atomske građe, a sastavljen je od niza tamnih spektralnih linija upravo svojstvene za određeni atom. Na taj način može se zaključiti o kemijskom sastavu Sunca i njegove atmosfere te je upravo to temelj spektralne analize. Tradicionalno se solarna spektroskopija izvodila u 1D modelima atmosfere uz određena pojednostavljenja, međutim danas se koriste sve sofisticiraniji i realniji 3D modeli, čime se dobivaju bolji rezultati stoga je prethodne potrebno korigirati. Masena spektroskopija izvodi se u adekvatnim laboratorijima, u kojima se s vrlo visokom preciznošću određuje kemijski sastav određenog tijela, ovdje meteorita. Analiziraju se najprimitivniji meteoriti, a obilnosti elemenata koje se pritom dobiju poslužuju kao odlična komparacija sa obilnostima dobivenim solarnom spektroskopijom. Kemijski sastav Sunčeve atmosfere nije jednak solarnom. Naime, postoje značajna odstupanja i to je primarno uzrokovano veoma visokim temperaturnim skokom između donjeg i gornjeg dijela atmosfere. Obilnosti elemenata se pritom mijenjaju što ovisi o njihovom prvom ionizacijskom potencijalu (FIP), što će u daljnjem radu biti i prikazano.

Abstract (english)

The chemical composition of the Sun is the foundation of astronomy. Its knowledge greatly helps us to understand the solar interior, evolution and the entire solar system in general because all cosmic bodies are essentially made of the same chemical components. The methods used for this purpose, and which will be described in this paper, are solar (absorption) spectroscopy and mass spectroscopy of primitive meteorites. Absorption spectroscopy of sunlight gives a certain spectrum full of absorption lines. Each individual element, in other words its atom, has its characteristic "imprint" in the obtained spectrum. The spectrum of an atom of a certain element is a representation of its atomic structure and it is composed of a series of dark spectral lines specific to a particular atom. In this way, one can conclude about the chemical composition of the Sun and its atmosphere and this is precisely the basis of spectral analysis. Traditionally, solar spectroscopy was performed in 1D models of the atmosphere with some simplifications, but today more and more sophisticated and realistic 3D models are used, which gives better results, so the previous ones need to be corrected. Mass spectroscopy is performed in adequate laboratories, in which the chemical composition of a particular body, here a meteorite, is determined with very high precision. The most primitive meteorites are analyzed, and the abundances of the elements obtained serve as an excellent comparison with the abundances obtained by solar spectroscopy. The chemical composition of the solar atmosphere is not equal to that of the sun. Namely, there are significant deviations and this is primarily caused by a very high temperature jump between the lower and upper part of the atmosphere. The abundances of the elements change depending on their first ionization potential (FIP), which will be shown in further work.

• Keywords: kemijski sastav Sunca; solarna spektroskopija; apsorpcijski spektar; masena spektroskopija; primitivni meteoriti; model atmosfere; prvi ionizacijski potencijal
• Keywords (english): chemical composition of the Sun; solar spectroscopy; absorption spectrum; mass spectroscopy; primitive meteorites; atmospheric model; first ionization potential
• Language: croatian
• URN:NBN: urn:nbn:hr:149:383957
• Study programme: Title: Environmental Engineering - Undergraduate study; Study programme type: university; Study level: undergraduate; Academic / professional title: sveučilišni/a prvostupnik/ prvostupnica (baccalaureus/baccalaurea) inženjer/inženjerka ekoinženjerstva (sveučilišni/a prvostupnik/ prvostupnica (baccalaureus/baccalaurea) inženjer/inženjerka ekoinženjerstva)
• Type of resource: Text
• File origin: Born digital
• Access conditions: Open access
• Created on: 2023-04-03 08:54:04