The investigation of thermal emission parameters at radio wavelengths as a probe for gamma-ray energies in classical novae

Detalhes bibliográficos
Autor(a) principal: Coimbra, Teresa Flores
Data de Publicação: 2021
Tipo de documento: Dissertação
Idioma: eng
Título da fonte: Repositório Científico de Acesso Aberto de Portugal (Repositórios Cientìficos)
Texto Completo: http://hdl.handle.net/10773/33724
Resumo: The study of Classical Novae over the last two decades has fastly changed due to the upgrade of radio telescopes, such as the Karl Jansky Very Large Array, and the advent of space-based γ-ray telescopes, such as Fermi. Multi-frequency studies of these objects are able to provide us detailed information about the physical conditions after eruptions enabling us to study the contributions of novae to their interstellar medium. Some, if not all, classical novae are predicted to release GeV γ-rays, although the origin of these emissions is yet to be fully understood. However, there are significant indications that it is connected to internal shocks within the ejected material, which also causes the non-thermal emission and dust production. The radio light curves of 7 classical novae (V959 Mon, V1324 Sco, V5668 Sgr, V357 Mus, V906 Car, V5589 Sgr, and V1723 Aql) were fitted with a spherically symmetric thermal emission model in this study, of which 2 are from previously unpublished data (V5668 Sgr and V357 Mus). The model is based on the “Hubble Flow Model” and is coupled with the Markov Chain Monte Carlo (MCMC) code, emcee. This is the first time the emcee code was coupled to fit radio light curves of novae. Non-thermal emission was clearly evident in the results of the fit, as expected from previous studies of these novae. In 6 out of the 7 novae the model was capable to decouple the two components of the emission. Of the 7 novae, only 5 were detected with γ-ray emission. This dissertation aims to identify connections between the thermal emission input parameters (distance, filling factor, maximum expansion velocity, and mass of ejecta) and the γ-ray brightness or the limit of nondetection. To date, attempts to find correlations between parameters at different wavelengths and γ-ray emission, or lack of, were met with various successes. We find an inverse correlation between the ejecta mass and the γ-ray luminosity. This inverse correlation is reminiscent of the attenuation of γ-ray photons by an absorbing screen (most likely the ejecta itself). The inverse correlation found between the γ-ray emission and ejected mass may also help explain the origin of the 102 factor observed in the values of detected γ-ray luminosit.
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spelling The investigation of thermal emission parameters at radio wavelengths as a probe for gamma-ray energies in classical novaeClassical novaeRadio continuumGamma-rays continuumThe study of Classical Novae over the last two decades has fastly changed due to the upgrade of radio telescopes, such as the Karl Jansky Very Large Array, and the advent of space-based γ-ray telescopes, such as Fermi. Multi-frequency studies of these objects are able to provide us detailed information about the physical conditions after eruptions enabling us to study the contributions of novae to their interstellar medium. Some, if not all, classical novae are predicted to release GeV γ-rays, although the origin of these emissions is yet to be fully understood. However, there are significant indications that it is connected to internal shocks within the ejected material, which also causes the non-thermal emission and dust production. The radio light curves of 7 classical novae (V959 Mon, V1324 Sco, V5668 Sgr, V357 Mus, V906 Car, V5589 Sgr, and V1723 Aql) were fitted with a spherically symmetric thermal emission model in this study, of which 2 are from previously unpublished data (V5668 Sgr and V357 Mus). The model is based on the “Hubble Flow Model” and is coupled with the Markov Chain Monte Carlo (MCMC) code, emcee. This is the first time the emcee code was coupled to fit radio light curves of novae. Non-thermal emission was clearly evident in the results of the fit, as expected from previous studies of these novae. In 6 out of the 7 novae the model was capable to decouple the two components of the emission. Of the 7 novae, only 5 were detected with γ-ray emission. This dissertation aims to identify connections between the thermal emission input parameters (distance, filling factor, maximum expansion velocity, and mass of ejecta) and the γ-ray brightness or the limit of nondetection. To date, attempts to find correlations between parameters at different wavelengths and γ-ray emission, or lack of, were met with various successes. We find an inverse correlation between the ejecta mass and the γ-ray luminosity. This inverse correlation is reminiscent of the attenuation of γ-ray photons by an absorbing screen (most likely the ejecta itself). The inverse correlation found between the γ-ray emission and ejected mass may also help explain the origin of the 102 factor observed in the values of detected γ-ray luminosit.O estudo de novas clássicas nas últimas duas décadas tem mudado rapidamente devido à melhoria de telescópios rádio, como o Karl Janky Very Large Array e novos telescópios espaciais de raios γ, como o Fermi. Estudos de multifrequências destes objetos são capazes de fornecer informação detalhada sobre as condições físicas durante erupções, permitindo o estudo das contribuições de novas no meio interestelar. Prevê-se que algumas, senão todas, as novas clássicas emitam raios γ com energia na ordem dos GeV. No entanto, a origem destas emissões não está ainda totalmente compreendida. Contudo, existe indicações significativas de que estão relacionadas com choques internos dentro do material expelido, que também causa emissão não-térmica e produção de poeira. Neste estudo, curvas de luz nas bandas de rádio de 7 novas clássicas (V959 Mon, V1323 Sco, V5668 Sgr, V357 Mus, V906 ´ Car, V5589 Sgr e V1723 Aql) foram ajustadas com um modelo de emissão térmica com simetria esférica, dos quais 2 são de dados não publicados (V5590 Sgr e V357 Mus). O modelo e baseado no “Hubble Flow Model” e está acoplado ao código de Monte Carlo de Cadeias de Markov, emcee. Esta e a primeira vez que o código emcee foi acoplado para fazer ajustes de curvas de luz nas bandas de rádio de novas. Emissão não-térmica estava claramente evidente nos resultados dos ajustes, como era de esperar tendo em conta resultados de estudos prévios. Em 6 de 7 novas, o modelo foi capaz de dissociar as duas ´ componentes de emissão. De 7 novas, apenas 5 foram detetadas em emissão de raios γ. Nesta dissertação pretende-se identificar conexões entre os parâmetros de entrada da radiação térmica (distância, fator de preenchimento, velocidade máxima de expansão e massa expelida) e o brilho de raios γ, ou o limite de não deteção. Até à data, tentativas para encontrar correlações entre parâmetros a diferentes comprimentos de onda e emissão de raios γ, ou falta dela, tiveram diversos graus de sucesso. Nós encontrámos uma correlação inversa entre a massa ejetada e a luminosidade de raios γ. Esta correlação inversa e remanescente da atenuação de fotões γ, por uma barreira absorvente (muito provavelmente o próprio material ejetado). A correlação inversa encontrada entre a emissão de raios γ e a massa expelida pode também ajudar a explicar o fator de 102 observado nos valores de luminosidade de raios γ.2022-04-22T08:47:04Z2021-12-17T00:00:00Z2021-12-17info:eu-repo/semantics/publishedVersioninfo:eu-repo/semantics/masterThesisapplication/pdfhttp://hdl.handle.net/10773/33724engCoimbra, Teresa Floresinfo:eu-repo/semantics/openAccessreponame:Repositório Científico de Acesso Aberto de Portugal (Repositórios Cientìficos)instname:Agência para a Sociedade do Conhecimento (UMIC) - FCT - Sociedade da Informaçãoinstacron:RCAAP2024-02-22T12:04:53Zoai:ria.ua.pt:10773/33724Portal AgregadorONGhttps://www.rcaap.pt/oai/openaireopendoar:71602024-03-20T03:05:05.059946Repositório Científico de Acesso Aberto de Portugal (Repositórios Cientìficos) - Agência para a Sociedade do Conhecimento (UMIC) - FCT - Sociedade da Informaçãofalse
dc.title.none.fl_str_mv The investigation of thermal emission parameters at radio wavelengths as a probe for gamma-ray energies in classical novae
title The investigation of thermal emission parameters at radio wavelengths as a probe for gamma-ray energies in classical novae
spellingShingle The investigation of thermal emission parameters at radio wavelengths as a probe for gamma-ray energies in classical novae
Coimbra, Teresa Flores
Classical novae
Radio continuum
Gamma-rays continuum
title_short The investigation of thermal emission parameters at radio wavelengths as a probe for gamma-ray energies in classical novae
title_full The investigation of thermal emission parameters at radio wavelengths as a probe for gamma-ray energies in classical novae
title_fullStr The investigation of thermal emission parameters at radio wavelengths as a probe for gamma-ray energies in classical novae
title_full_unstemmed The investigation of thermal emission parameters at radio wavelengths as a probe for gamma-ray energies in classical novae
title_sort The investigation of thermal emission parameters at radio wavelengths as a probe for gamma-ray energies in classical novae
author Coimbra, Teresa Flores
author_facet Coimbra, Teresa Flores
author_role author
dc.contributor.author.fl_str_mv Coimbra, Teresa Flores
dc.subject.por.fl_str_mv Classical novae
Radio continuum
Gamma-rays continuum
topic Classical novae
Radio continuum
Gamma-rays continuum
description The study of Classical Novae over the last two decades has fastly changed due to the upgrade of radio telescopes, such as the Karl Jansky Very Large Array, and the advent of space-based γ-ray telescopes, such as Fermi. Multi-frequency studies of these objects are able to provide us detailed information about the physical conditions after eruptions enabling us to study the contributions of novae to their interstellar medium. Some, if not all, classical novae are predicted to release GeV γ-rays, although the origin of these emissions is yet to be fully understood. However, there are significant indications that it is connected to internal shocks within the ejected material, which also causes the non-thermal emission and dust production. The radio light curves of 7 classical novae (V959 Mon, V1324 Sco, V5668 Sgr, V357 Mus, V906 Car, V5589 Sgr, and V1723 Aql) were fitted with a spherically symmetric thermal emission model in this study, of which 2 are from previously unpublished data (V5668 Sgr and V357 Mus). The model is based on the “Hubble Flow Model” and is coupled with the Markov Chain Monte Carlo (MCMC) code, emcee. This is the first time the emcee code was coupled to fit radio light curves of novae. Non-thermal emission was clearly evident in the results of the fit, as expected from previous studies of these novae. In 6 out of the 7 novae the model was capable to decouple the two components of the emission. Of the 7 novae, only 5 were detected with γ-ray emission. This dissertation aims to identify connections between the thermal emission input parameters (distance, filling factor, maximum expansion velocity, and mass of ejecta) and the γ-ray brightness or the limit of nondetection. To date, attempts to find correlations between parameters at different wavelengths and γ-ray emission, or lack of, were met with various successes. We find an inverse correlation between the ejecta mass and the γ-ray luminosity. This inverse correlation is reminiscent of the attenuation of γ-ray photons by an absorbing screen (most likely the ejecta itself). The inverse correlation found between the γ-ray emission and ejected mass may also help explain the origin of the 102 factor observed in the values of detected γ-ray luminosit.
publishDate 2021
dc.date.none.fl_str_mv 2021-12-17T00:00:00Z
2021-12-17
2022-04-22T08:47:04Z
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