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Dissertations / Theses on the topic 'Supernova 1987A'

Author: Grafiati

Published: 4 June 2021

Last updated: 21 February 2023

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1

Wheaton, Vivienne. "Investigation of radio emission from Supernova Remnant 1987A." Thesis, The University of Sydney, 2002. https://hdl.handle.net/2123/27884.

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This thesis investigates the recent radio emission from the remnant of Supernova 1987A in the Large Magellanic Cloud. Radio emission from this developing supernova remnant was detected in June 1990, just over three years after the initial outburst from the supernova explosion. Monitored with the Molonglo Observatory Synthesis Telescope and the Australia Telescope Compact Array, the SNR has been increasing in radio brightness to the present day. Observations from the Hubble Space Telescope, ROSAT and Chandra confirm that the remnant is also brightening in optical and X-ray wavelengths. T

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2

Fischera, Jörg. "Infrarotemission der SN 1987A nach 11 Jahren." [S.l. : s.n.], 2000. http://deposit.ddb.de/cgi-bin/dokserv?idn=961763183.

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3

Woo, Sui-chi. "Physical conditions in the circumstellar gas surrounding supernova 1987A." Click to view the E-thesis via HKUTO, 2005. http://sunzi.lib.hku.hk/hkuto/record/B30736365.

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4

Woo, Sui-chi, and 胡瑞慈. "Physical conditions in the circumstellar gas surrounding supernova 1987A." Thesis, The University of Hong Kong (Pokfulam, Hong Kong), 2005. http://hub.hku.hk/bib/B30736365.

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5

Larsson, J., C. Fransson, J. Spyromilio, et al. "THREE-DIMENSIONAL DISTRIBUTION OF EJECTA IN SUPERNOVA 1987A AT 10,000 DAYS." IOP PUBLISHING LTD, 2016. http://hdl.handle.net/10150/622678.

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Due to its proximity, SN. 1987A offers a unique opportunity to directly observe the geometry of a stellar explosion as it unfolds. Here we present spectral and imaging observations of SN. 1987A obtained similar to 10,000 days after the explosion with HST/STIS and VLT/SINFONI at optical and near-infrared wavelengths. These observations allow us to produce the most detailed 3D map of Ha to date, the first 3D maps for [Ca II] lambda lambda 7292, 7324, [O I] lambda lambda 6300, 6364, and Mg. II lambda lambda 9218, 9244, as well as new maps for [Si I]+[Fe II] 1.644 mu m and He I 2.058 mu m. A compa

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6

Leung, Wing-kit, and 梁榮傑. "Three dimensional structure and kinematics of the inner ejecta of supernova 1987A." Thesis, The University of Hong Kong (Pokfulam, Hong Kong), 2010. http://hub.hku.hk/bib/B45542077.

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7

Gröningsson, Per. "The rebirth of Supernova 1987A : a study of the ejecta-ring collision." Doctoral thesis, Stockholms universitet, Institutionen för astronomi, 2008. http://urn.kb.se/resolve?urn=urn:nbn:se:su:diva-8290.

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Supernovae are some of the most energetic phenomena in the Universe and they have throughout history fascinated people as they appeared as new stars in the sky. Supernova (SN) 1987A exploded in the nearby satellite galaxy, the Large Magellanic Cloud (LMC), at a distance of only 168,000 light years. The proximity of SN 1987A offers a unique opportunity to study the medium surrounding the supernova in great detail. Powered by the dynamical interaction of the ejecta with the inner circumstellar ring, SN 1987A is dramatically evolving at all wavelengths on time scales less than a year. This makes

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8

Cahen, Sébastien. "Deux enigmes de l'evolution stellaire : les neutrinos solaires et la supernova 1987a." Paris 7, 1987. http://www.theses.fr/1987PA077271.

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Les modeles solaires standards recents, bases sur les tables d'opacite de los alamos, sont compares. Les resultats, notamment l'abondance solaire solaire d'helium et le flux de neutrinos sont presentes et discutes. Un modele semi-analytique de courbe de lumiere de supernovae a ete developpe suivant le schema d'arnett. Les caracteristiques principales de l'emission lumineuse des supernovae, y compris celle des supernovae de type ib ainsi que celle de la supernova 1987a, sont correctement reproduites a l'aide de ce modele

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9

Gröningsson, Per. "The rebirth of supernova 1987A : a study of the ejecta-ring collision /." Stockholm : Department of Astronomy, Stockholm University, 2008. http://urn.kb.se/resolve?urn=urn:nbn:se:su:diva-8290.

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10

Cahen, Sébastien. "Deux énigmes de l'évolution stellaire les neutrinos solaires et la Supernova 1987a /." Grenoble 2 : ANRT, 1987. http://catalogue.bnf.fr/ark:/12148/cb37603554d.

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11

Lo, Man-kit. "Modelling and observations of the circumstellar ring system of supernova 1987A with the Hubble Space Telescope." Click to view the E-thesis via HKUTO, 2006. http://sunzi.lib.hku.hk/hkuto/record/B38909741.

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12

Kelly, P. L., G. Brammer, J. Selsing, et al. "SN REFSDAL: CLASSIFICATION AS A LUMINOUS AND BLUE SN 1987A-LIKE TYPE II SUPERNOVA." IOP PUBLISHING LTD, 2016. http://hdl.handle.net/10150/624069.

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We have acquired Hubble Space Telescope (HST) and Very Large Telescope near-infrared spectra and images of supernova (SN) Refsdal after its discovery as an Einstein cross in fall 2014. The HST light curve of SN Refsdal has a shape consistent with the distinctive, slowly rising light curves of SN. 1987A-like SNe, and we find strong evidence for a broad H alpha P-Cygni profile and Na I D absorption in the HST grism spectrum at the redshift (z = 1.49) of the spiral host galaxy. SNe. IIn, largely powered by circumstellar interaction, could provide a good match to the light curve of SN Refsdal, but

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13

Sawada, Ryo. "Nucleosynthesis Constraints on the Energy Growth Timescale of a Core-collapse Supernova Explosion." Kyoto University, 2020. http://hdl.handle.net/2433/253085.

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14

Lo, Man-kit, and 盧文傑. "Modelling and observations of the circumstellar ring system of supernova 1987A with the Hubble Space Telescope." Thesis, The University of Hong Kong (Pokfulam, Hong Kong), 2006. http://hub.hku.hk/bib/B38909741.

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15

Kihlström, Camilla. "The evolution of Supernova 1987A probed by Hubble Space Telescope observations in the narrow F502N Filter." Thesis, KTH, Fysik, 2016. http://urn.kb.se/resolve?urn=urn:nbn:se:kth:diva-183146.

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16

Souza, Carlos Alexandre Wuensche de. "Observações na faixa de raios X e gama da supernova SN 1987A usando detectores "phoswich" BGO-CsI (T1)." Instituto Nacional de Pesquisas Espaciais (INPE), 1988. http://urlib.net/sid.inpe.br/iris@1905/2005/07.26.22.52.33.

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O experimento SUGAR 87, lançado a bordo de balão estratosférico, foi inicialmente idealizado para verificar o desempenho dos detectares "phoswich" BGO-CsI(TI) na astronomia de raios gama, e, posteriormente, também para observar a supernova SN 1987A. Discute-se nesse trabalho as características dos detectares "phoswich" e da eletrônica associada, bem como o processo de redução dos dados e montagem dos arquivos. Apresenta-se o resultado da análise dos dados, e os limites superiores dos fluxos estimados em quatro bandas de energia. Os resultados obtidos são comparados com os de outros autores, mo

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17

BOUCHET, PATRICE. "Les mille et une nuits de la supernova sn 1987a. Contribution aux observations dans l'infrarouge entre 1 et 20 microns." Paris 7, 1990. http://www.theses.fr/1990PA077180.

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Depuis sa decouverte, la supernova sn 1987a est observee regulierement a la silla (eso) dans le domaine infrarouge du spectre. Les observations photometriques et spectrophotometriques obtenues entre 1 et 20 microns jusqu'au jour 1316 sont presentees. Ces observations permettent de calculer la luminosite bolometrique de la supernova et d'en etudier la variation en fonction du temps: il est montre que jusqu'au jour 900, la desintegration radioactive du cobalt peut, seule, rendre compte du budget energetique observe, mais que par la suite, la consideration d'une source d'energie supplementaire de

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18

Lehoucq, Roland. "Emission a haute energie de la supernova sn 1987a. Acceleration des rayons cosmiques dans les ondes de choc a deux fluides." Paris 6, 1992. http://www.theses.fr/1992PA066540.

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La premiere partie de cette these concerne l'emission a haute energie de la supernova sn 1987a. Ce travail est base sur une simulation monte-carlo du transfert des photons gamma emis lors de la desintegration des elements radioactifs (tels que le #5#6ni, #5#6co, #5#7co et #4#4ti) produits lors de l'explosion. Ces photons gamma interagissent avec l'enveloppe en expansion et y depose donc une partie de leur energie qui alimentera la courbe de lumiere bolometrique. L'un des problemes qui se pose concerne l'evolution tardive (au-dela de 1200 jours) de la courbe de lumiere, tres differente selon qu

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19

Jerkstrand, Anders. "Spectral modeling of nebular-phase supernovae." Doctoral thesis, Stockholms universitet, Institutionen för astronomi, 2011. http://urn.kb.se/resolve?urn=urn:nbn:se:su:diva-64130.

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Massive stars live fast and die young. They shine furiously for a few million years, during which time they synthesize most of the heavy elements in the universe in their cores. They end by blowing themselves up in a powerful explosion known as a supernova (SN). During this process, the core collapses to a neutron star or a black hole, while the outer layers are expelled with velocities of thousands of kilometers per second. The resulting fireworks often outshine the entire host galaxy for many weeks. The explosion energy is eventually radiated away, but powering of the newborn nebula continue

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20

Mattila, Seppo Kalevi. "Supernovae as probes of their host galaxies and circumstellar environments : search strategies in nuclear starbursts and spectroscopy of the SN 1987A CSM." Thesis, Imperial College London, 2002. http://ethos.bl.uk/OrderDetails.do?uin=uk.bl.ethos.396416.

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21

Palmer, David M. "Gamma-ray imaging observations of Supernova 1987A." Thesis, 1992. https://thesis.library.caltech.edu/6645/3/Palmer_dm_1992.pdf.

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The Caltech imaging γ-ray telescope has made four balloon flights from Alice Springs, Australia, to observe the hard X-ray and γ-ray emission from Supernova 1987 A as it evolved between 1987 May and 1989 April. We have detected γ-rays with the time behavior and spectral signature expected from freshly-synthesized radioisotopes embedded in a cloud of ejecta. In particular, we detect the 847 and 1238 keY γ-ray lines produced by the decay of ^(56)Co, and the continuum spectrum expected from Compton scattering of these γ-trays. The results of these observations are compared with other measurements

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