FRINK Linked Data Fragments server

Matches in SemOpenAlex for { <https://semopenalex.org/work/W2005556543> ?p ?o ?g. }

• W2005556543 endingPage "473" @default.
• W2005556543 startingPage "470" @default.
• W2005556543 abstract "Many uncertainties about the physics of Type Ia Supernovae have been revealed in the recent past, and numerous pieces are puzzled together to achieve a complete description of the phenomenon of thermonuclear explosions in the sky. However, very important parts are still missing. In particular, the concept lacks a proper connection between the various evolutionary steps, namely the progenitor scenario, explosion theory, nucleosynthesis from the burning, and the observations. Early time spectra of Type Ia Supernovae naturally contain information about all of these processes and are at the centre of the entire scenario. Appropriate models of that phase can provide the missing link and improve our understanding of this field enormously.The goal of this thesis is to advance new methods to calculate synthetic spectra in order to extract the information contained in the observations more efficiently. Based on a well established radiation transfer code, a new technique called Abundance Tomography is developed to derive the abundance distribution of Type Ia Supernovae ejecta. While previous approaches were limited to the determination of the abundances of specific species in restricted regions of the supernova envelope, here a complete stratified distribution of all major elements is obtained. This method is applied to the very well observed normal SN 2002bo. Combining the early spectra with those of the nebular phase leads to a coverage of the entire ejecta from the centre out to the highest velocities. The abundances derived are used to compute a synthetic bolometric light curve to test the radial distribution of Fe group and intermediate-mass elements.The sampling procedure of the incident radiation field at the lower boundary is modified to obtain a better description of the real situation in Type Ia Supernovae. This improves the overall flux distribution significantly, especially in the red part of the spectrum, where almost no real line opacity is found. Synthetic spectra with this new procedure reproduce the observations much more accurately, as is shown by models of SN 2002er.Hydrogen lines have never been detected convincingly in Type Ia Supernovae spectra. However, using spectra that were observed more than 10 days before maximum light, it is shown that small amounts of hydrogen in the outer parts of the ejecta can explain high velocity line absorptions, seen rather frequently in various objects, e.g. SN 2002dj, SN 2003du, and SN 1999ee. The hydrogen is not claimed to be primordial to the white dwarf but it is rather the effect of the supernova ejecta interacting with circumstellar material, namely the white dwarf's accretion disk build up prior to the explosion.Finally, UV spectra of Type Ia Supernovae are discussed. The ability of the Monte Carlo technique to deal naturally with this wavelength region is proven. Applications are presented by modelling spectra of SN 2001ep and SN 2001eh obtained with the Hubble Space Telescope.The results are discussed in the broader context of Type Ia Supernovae physics: What causes the diversity in the nearby sample? What are the progenitors and how does the explosion work? What is the influence on cosmological models?A detailed knowledge of the abundances, their distribution in the Supernova ejecta, and their ultimate causes delivers the key to these fundamental issues." @default.
• W2005556543 created "2016-06-24" @default.
• W2005556543 creator A5045263387 @default.
• W2005556543 creator A5063952009 @default.
• W2005556543 creator A5085076363 @default.
• W2005556543 date "2005-07-01" @default.
• W2005556543 modified "2023-09-30" @default.
• W2005556543 title "Abundance Tomography of Type Ia Supernovae" @default.
• W2005556543 cites W1580915579 @default.
• W2005556543 cites W1583674215 @default.
• W2005556543 cites W1641974191 @default.
• W2005556543 cites W1669035461 @default.
• W2005556543 cites W1672507132 @default.
• W2005556543 cites W1679908910 @default.
• W2005556543 cites W1812581782 @default.
• W2005556543 cites W1852489411 @default.
• W2005556543 cites W1924837178 @default.
• W2005556543 cites W1937555315 @default.
• W2005556543 cites W1972481559 @default.
• W2005556543 cites W1973120086 @default.
• W2005556543 cites W1973677647 @default.
• W2005556543 cites W1977758345 @default.
• W2005556543 cites W1981722972 @default.
• W2005556543 cites W1987861871 @default.
• W2005556543 cites W1988987494 @default.
• W2005556543 cites W1989204103 @default.
• W2005556543 cites W1989543776 @default.
• W2005556543 cites W1990102346 @default.
• W2005556543 cites W1990650561 @default.
• W2005556543 cites W1990905945 @default.
• W2005556543 cites W1992672178 @default.
• W2005556543 cites W1993985662 @default.
• W2005556543 cites W1995618220 @default.
• W2005556543 cites W2005421842 @default.
• W2005556543 cites W2012502562 @default.
• W2005556543 cites W2015524444 @default.
• W2005556543 cites W2020743846 @default.
• W2005556543 cites W2022558167 @default.
• W2005556543 cites W2034528967 @default.
• W2005556543 cites W2035212947 @default.
• W2005556543 cites W2035597315 @default.
• W2005556543 cites W2038347333 @default.
• W2005556543 cites W2039130581 @default.
• W2005556543 cites W2042607720 @default.
• W2005556543 cites W2044031897 @default.
• W2005556543 cites W2044199977 @default.
• W2005556543 cites W2053097648 @default.
• W2005556543 cites W2056284514 @default.
• W2005556543 cites W2059370568 @default.
• W2005556543 cites W2060993199 @default.
• W2005556543 cites W2062393562 @default.
• W2005556543 cites W2063610195 @default.
• W2005556543 cites W2067541961 @default.
• W2005556543 cites W2070751362 @default.
• W2005556543 cites W2072356130 @default.
• W2005556543 cites W2072851025 @default.
• W2005556543 cites W2073832139 @default.
• W2005556543 cites W2081511040 @default.
• W2005556543 cites W2086593645 @default.
• W2005556543 cites W2092229642 @default.
• W2005556543 cites W2095272324 @default.
• W2005556543 cites W2096911128 @default.
• W2005556543 cites W2101000578 @default.
• W2005556543 cites W2107835585 @default.
• W2005556543 cites W2114909577 @default.
• W2005556543 cites W2118344051 @default.
• W2005556543 cites W2122038210 @default.
• W2005556543 cites W2127392678 @default.
• W2005556543 cites W2135156375 @default.
• W2005556543 cites W2137342763 @default.
• W2005556543 cites W2139440433 @default.
• W2005556543 cites W2140767034 @default.
• W2005556543 cites W2153834943 @default.
• W2005556543 cites W2154213758 @default.
• W2005556543 cites W2154761413 @default.
• W2005556543 cites W2156856858 @default.
• W2005556543 cites W2161137739 @default.
• W2005556543 cites W2161844270 @default.
• W2005556543 cites W2401910189 @default.
• W2005556543 cites W2735454799 @default.
• W2005556543 cites W2949897354 @default.
• W2005556543 cites W2952535194 @default.
• W2005556543 cites W2963164330 @default.
• W2005556543 cites W2964222985 @default.
• W2005556543 cites W2987431865 @default.
• W2005556543 cites W2989614736 @default.
• W2005556543 cites W2990105695 @default.
• W2005556543 cites W2997687071 @default.
• W2005556543 cites W2999154694 @default.
• W2005556543 cites W3004459386 @default.
• W2005556543 cites W3009341580 @default.
• W2005556543 cites W3010899931 @default.
• W2005556543 cites W3013503367 @default.
• W2005556543 cites W3017545881 @default.
• W2005556543 cites W3027539418 @default.
• W2005556543 cites W3041106475 @default.
• W2005556543 cites W3049702659 @default.
• W2005556543 cites W3097313079 @default.

• next