#TITLE_ALTERNATIVE#
Ultraluminous supersoft source (ULS) is class of X-ray emitters which have luminosities ~1039 erg/s, dominated by thermal X-ray radiation below 1 keV with little, or no, flux observed at higher energies. ULS was found at around year 2000 in ROSAT era, and since then have been observed with other X-r...
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| Format: | Final Project |
| Language: | Indonesia |
| Online Access: | https://digilib.itb.ac.id/gdl/view/30709 |
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| Institution: | Institut Teknologi Bandung |
| Language: | Indonesia |
| Summary: | Ultraluminous supersoft source (ULS) is class of X-ray emitters which have luminosities ~1039 erg/s, dominated by thermal X-ray radiation below 1 keV with little, or no, flux observed at higher energies. ULS was found at around year 2000 in ROSAT era, and since then have been observed with other X-ray missions with higher resolution, such as Chandra and XMM-Newton. This final project aims to study the X-ray properties of ULS, especially on its spectra. The method used in this final project is literature study and data processing. This final project also describes X-ray properties from two X-ray sources which have close relation with ULS, namely Black Hole Binary (BHB) and Ultraluminous X-ray Source (ULX). These sources have been extensively studied in the past few decades. Study about the properties of these sources are intended to provide some fundamental ideas in order to explain the physical model of ULS, in the context of acretion onto stellar-mass black hole. The most plausible physical model for ULS is an optically thick corona which blocked a super-Eddington disk. This physical model has a close resemble to the one used in ULX, which usually can be explained using super-Eddington accretion model. A unification model for ULX and ULS can be made based on that model. This final project used ULS data from XMM-Newton observations. The list of ULS is taken from Liu (2011) catalogue of ULX and ULS, which contains 70 ULSs. A data selection was done so that only 5 ULSs are used for analysis. There are a total of 27 observations. For those ULSs which have been observed more than once, variability study can be conducted, and a few ULSs do show variability in their intensity. Spectral fitting shows that most of the data can be fitted well with blackbody and disk blackbody model, where the resulted parameters are very similar to those of the earlier studies. |
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