從大質量恆星爆發的伽瑪射線爆;Gamma-Ray Burst as Massive Star Explosion

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題名:	從大質量恆星爆發的伽瑪射線爆;Gamma-Ray Burst as Massive Star Explosion
作者:	浦田裕次
貢獻者:	天文學研究所
關鍵詞:	伽瑪射線爆;超新星;觀測;自動觀測儀器;研究領域：物理類
日期:	2011-08-01
上傳時間:	2012-01-17 18:57:04 (UTC+8)
出版者:	行政院國家科學委員會
摘要:	現今宇宙的重金屬元素大都來自超新星的爆發。而這些超新星也在星系演化中拌演重要地位，且同時和宇宙中另一種高能爆發--伽瑪射線爆有所關連。觀測資料顯示，伽瑪射線爆是某種大質量恆星死亡後，其中心產生黑洞以及造成高動能的超新星爆發，並透過相對論性噴流將能量釋放到星際中。此外，高紅移的伽瑪射線爆陸續被發現後，更將伽瑪射線爆與宇宙最初的第一代恆星連結一起。然而，產生伽瑪射線爆的原始星以及與超新星的關連至今尚未定案，天文學者正積極的從觀測資料以及理論模擬中找尋結合此兩種高能爆發的合理解釋。此計畫將致力於研究伽瑪射線爆原始星以及研究與其相關連的超新星。我們將執行(A)多波段伽瑪射線爆及時觀測研究伽瑪射線報的輻射機制。我們將建立廣角光學照相機（WIDGET)，捕捉伽瑪射線爆爆發時的瞬間光學特性，並結合衛星的觀測來限制目前伽瑪射線爆輻射理論（synchrotron self-Compton radiation)以及從原始星產生的黑體輻射（Blackbody radiation); (B) 從伽瑪射線爆餘暉晚期觀測來發現與其相關連的超新星，並與其他核塌縮超新星比較，藉以了解造成伽瑪射線爆的超新星其輻射機制。此外，我們將透過台灣所參與的光學巡天計畫(泛星計畫及日本昂星望遠鏡廣角巡天）所發現的核塌縮超新星當作樣本並與伽瑪射線爆相關的超新星比較，研究哪種超新星可造成伽瑪射線爆發。 Supernovae (SNe) have created the heavy chemical elements we now see in the Universe and their large kinetic energies mean they have been key components in the formation of galaxies. Gamma Ray Bursts (GRBs) is believed to arise when a very massive star dies in a highly energetic supernova producing a black hole and relativistic jet. Furthermore, GRBs are now well known as the powerful probe of the early Universe and the first star finding. However, recent discoveries of new ultra-luminous supernovae are testing our ideas of what types of stars can produce SNe/GRBs and even more fundamentally challenge the paradigm of core-collapse. We aim to reveal the GRB progenitor and conditions of GRB-SNe associations. We investigate the most different properties and the most resemble features between GRBs and SNe. First, we will perform (A) multi-frequency studies for the GRB prompt emission. Since SNe usually have no bright γ-ray or X-ray emissions, the prompt behavior is particularly different between GRB and SNe. The acceleration of the electron is directly related with how the massive star explodes. But recent detection of bright optical emission associated with γ-ray pose a challenge to the current understanding of the GRB radiation mechanism. In order to make break through, we will enhance our robotic instrument WIDGET to make multi-color simultaneous observations with γ-ray emission. This upgrade and its observations with GRB satellites allow us to constrain the synchrotronself- Compton radiation model of the prompt emission and existence of blackbody component from photosphere of progenitors. Second, we will perform (B) comparison studies on the SNe component associated with GRB. The late optical afterglows often show the bump that can be understood by the SNe component. This result is strongly suggested that GRBs link to core collapse supernova. However, the difference between them is unclear such as what are the progenitors of core-collapse SNe and GRBs and what are their explosion mechanisms and subsequent evolution? In fact, deep enough optical monitoring observations found the non-supernova associations for nearby GRB060614 and GRB060505. The key question is that what kind of SNe will make GRBs. In order to answer these questions, we will make the new core-collapse SNe template using unbiased optical imaging surveys (Pan-STARRS and SUBARU/HSC) and compare with the GRB-SNe component. 研究期間：10008 ~ 10107
關聯:	財團法人國家實驗研究院科技政策研究與資訊中心
顯示於類別:	[天文研究所] 研究計畫

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