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Understanding Gamma-Ray Bursts: Insights from CGRO, BeppoSAX, and HETE-2 Observations

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This overview explores the pivotal findings from various gamma-ray observatories, including the Compton Gamma-Ray Observatory (CGRO), BeppoSAX, and HETE-2. Key discoveries such as afterglow phenomena, redshift measurements of gamma-ray bursts (GRBs), and the correlation between GRBs and supernovae are highlighted. Notably, GRB020903 offers detailed characteristics like burst duration and spectral analysis across wide energy ranges. The advancements in gamma-ray detection technologies have significantly enhanced our understanding of these explosive cosmic events.

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Understanding Gamma-Ray Bursts: Insights from CGRO, BeppoSAX, and HETE-2 Observations

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  1. Compton Gamma-Ray Observatory (CGRO) Burst And Transient Source Experiment (BATSE) BeppoSAX (WFC / GRBM / NFI) BeppoSAX BATSE • 等方的な全天分布 • 暗いGRB の数が少ない • 残光の発見 • GRBの赤方偏移, z ~ 1 発見１９６７ ガンマ線バースト (GRBs) • ガンマ線で明るい (50-300 keV) • スパイク状の強度変動 • 継続時間の長いもの短いものclick

  2. High Energy Transient Explorer-2 (HETE-2) Soft X-ray Camera (SXC) MIT (USA) Attitude control optical camera MIT (USA) French Gamma-ray Telescope (FREGATE) CESR (France) Wide-field X-ray Monitor (WXM) 理研 (日本)/ LANL (USA) Satellite system MIT (USA) 重量 124 kg 大きさ 　89 cm (高さ) x 66 cm (幅) 軌道 高度 625 km, 赤道軌道 姿勢 　 反太陽方向 打ち上げ 2000年10月9日

  3. HETE-2 の特徴 • 地上観測者への GRB 発生位置の速報 • 広いエネルギー範囲 (2-400 keV) でのGRB 本体のスペクトルスコピー 15 副地上局 3 主地上局

  4. GRB020903 バースト発生時間: 2002年 9月3日 10:05:38 バーストの特徴: ・継続時間 (2-10 keV): 4.9 秒 (T50),9.8 秒(T90) ・ X-ray / g –ray fluence 比: S(2-30 keV) / S(30-400 keV) = 5.6 ・Peak flux (1s, 2-10 keV): (2.2 ±0.8) ph cm-2 s-1 ・Total fluence (2-10 keV): (5.9 ±1.4) x 10-8 erg cm-2 Afterglow: ・可視光天体(OT) (Palomar 200-inch, Soderberg et al.) ・母銀河の赤方偏移 z = 0.25±0.01 (Soderberg et al., Chornock & Filippenko) ・OT の位置に電波天体 (VLA, Berger et al.) ・母銀河は不規則銀河(HST, Levan et al.)

  5. OT WXM SXC GRB020903 バースト発生時間: 2002年 9月3日 10:05:38 バーストの特徴: ・継続時間 (2-10 keV): 4.9 秒 (T50),9.8 秒(T90) ・ X-ray / g –ray fluence 比: S(2-30 keV) / S(30-400 keV) = 5.6 ・Peak flux (1s, 2-10 keV): (2.2 ±0.8) ph cm-2 s-1 ・Total fluence (2-10 keV): (5.9 ±1.4) x 10-8 erg cm-2 Afterglow: ・可視光天体(OT) (Palomar 200-inch, Soderberg et al.) ・母銀河の赤方偏移 z = 0.25±0.01 (Soderberg et al., Chornock & Filippenko) ・OT の位置に電波天体 (VLA, Berger et al.) ・母銀河は不規則銀河(HST, Levan et al.)

  6. GRB と 超新星爆発の関連 (1)GRB030329 / SN2003dh WXM: 2-25 keV FREGATE: 7-400 keV 7-30 keV

  7. GRB と 超新星爆発の関連 (2)GRB030329 / SN2003dh 世界最速で残光発見 (理研 屋上望遠鏡) 残光から Ic 型超新星のスペクトル 24時間後 発生直後 （Torii et al. 2003) 東工大屋上望遠鏡 5時間後 2日後 67分後 (Sato et al. 2003)

  8. 終わり

  9. GRB の光度曲線 (HETEのバースト) スパイク状の強度変動 GRB020813 GRB030329 Counts / s GRB020531 継続時間の長いもの短いもの click Seconds since trigger

  10. GRB の全天分布 (http://cossc.gsfc.nasa.gov/batse/index.html) click

  11. BATSE-PVO logN-lopP (PVO: Pioneer Venus Orbiter, 1978-1992, 100 keV – 2 MeV, CsI scintillator) P-0.8 (z max = 1~2) log N yr -1 P-1.5 (z max = 0.2~0.3) (Fenimore et al. 1993, Mao and Paczynski 1992) click

  12. Optical (V band) 21 hours after the trigger ~ 9 days after the trigger (van Paradijs et al. 1997) GRB970228 X-ray 8 hours after the trigger ~ 3 days after the trigger One more click for optical, then http://bepposax.gsfc.nasa.gov/bepposax/first/grb970228.html click

  13. ガンマ線バースト からの放射 Vela (1970-1979) Apollo 16 (1972) GRB720427 (Metzger et al. 1974, Trombka et al. 1974) - Apollo 16 and Vela 6A - X線領域で同様の時間変動 10 E-1.36 (http://heasarc.gsfc.nasa.gov /docs/vela5b/vela5b.html) (http://heasarc.gsfc.nasa.gov /docs/heasarc/missions/images/apollo1516_images.html) 10-1 2.8-7.9 keV 6s X線観測の重要性 Photon cm-2 s-1 keV-1 break E-2.63 10-3 ぎんが衛星 GBD -PC: 2-25 keV -SC: 15-400 keV 67-5100 keV 10-5 10 100 1000 click HETE Energy (keV)

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