%0 Journal Article
%@holdercode {isadg {BR SPINPE} ibi 8JMKD3MGPCW/3DT298S}
%@nexthigherunit 8JMKD3MGPCW/3ETR8EH
%@archivingpolicy denypublisher denyfinaldraft
%@issn 0375-9687
%@usergroup administrator
%@usergroup marciana
%3 kawai-hete.pdf
%@dissemination WEBSCI; PORTALCAPES.
%X The High Energy Transient Explorer 2 (HETE-2), launched in October 2000, is currently localizing gamma-ray bursts (GRBs) at a rate of similar to20 yr(-1) many in real time. As of September 2003, HETE-2 had localized 47 GRBs; 16 localizations had led to the detection of an X-ray, optical, or radio afterglows. The prompt position notification of HETE-2 enabled probing the nature of so-called "dark bursts" for which no optical afterglows were found despite of accurate localizations. In some cases, the optical afterglow was found to be intrinsically faint, and its flux declined rapidly. In another case, the optical emission was likely to be extinguished by the dust in the vicinity of the GRB source. The bright afterglows of GRB021004 and GRB030329 were observed in unprecedented details by telescopes around the world. Strong evidence for the association of long GRBs with the core-collapse supernovae was found. HETE-2 has localized almost as many X-ray rich GRBs as classical GRBs. The nature of the X-ray rich GRBs a-rid X-ray flashes have been studied systematically with HETE-2, and they are found to have many properties in common with the classical GRBs, suggesting that they are a single phenomenon.
%T Hete-2 observations of gamma-ray bursts and their follow-ups
%K early optical-emission, afterglow, discovery, supernova, flashes.
%@secondarytype PRE PI
%@group DAS-INPE-MCT-BR
%@copyholder SID/SCD
%@secondarykey INPE-13773-PRE/8961
%2 sid.inpe.br/jeferson/2005/01.14.09.01.30
%@affiliation Tokyo Inst Technol, Dept Phys, Tokyo, Japan,
%@affiliation Inst Phys & Chem Res, Wako, Saitama  Japan,
%@affiliation Natl Space Dev Agcy Japan, Tsukuba, Ibaraki  Japan,
%@affiliation Aoyama Gakuin Univ, Sagamihara, Kanagawa  Japan,
%@affiliation Natl Astron Observ Japan, Mitaka, Tokyo  Japan,
%@affiliation MIT, Ctr Space Res, Cambridge, MA  USA,
%@affiliation Observ Midi Pyrenees, Toulouse,  France,
%@affiliation Los Alamos Natl Lab, Los Alamos, NM USA,
%@affiliation Univ Chicago, Ctr Astron & Astrophys, Chicago, IL  USA,
%@affiliation Univ Calif Berkeley, Space Sci Lab, Berkeley, CA  USA,
%@affiliation Univ Calif Santa Cruz, Santa Cruz, CA 95064 USA,
%@affiliation Ctr Etud Spatiale Rayonnements, Toulouse, France,
%@affiliation CNR, IASF, TESRE, Bologna,  Italy,
%@affiliation NASA, Goddard Space Flight Ctr, Greenbelt, MD  USA,
%@affiliation Tata Inst Fundamental Res, Bombay, Maharashtra 400005 India,
%@affiliation Univ Sci & Tech Masuku, Franceville, Gabon,
%@affiliation Inst Nacl Pesquisas Espaciais, Sao Jose Dos Campos,  Brazil,
%@affiliation Miyazaki Univ, Fac Engn, Miyazaki,  Japan,
%@affiliation
%@affiliation
%B Progress of Theoretical Physics Supplement
%P 279-286
%4 sid.inpe.br/jeferson/2005/01.14.09.01
%D 2004
%V 155
%A Kawai N,
%A Matsuoka M,
%A Yoshida A,
%A Shirasaki Y,
%A Ricker G,
%A Doty J,
%A Vanderspek R,
%A CrewG,
%A Villasenor J,
%A Atteia JL,
%A Fenimore EE,
%A Galassi M,
%A Lamb DQ,
%A Graziani C,
%A Hurley K,
%A JG, Jernigan,
%A Woosley S,
%A Martel F,
%A Monnelly G,
%A Prigozhin G,
%A Olive JF,
%A Dezalay JP,
%A Boer M,
%A Pizzichini G,
%A T, Cline,
%A Levine A,
%A Morgan E,
%A Tamagawa T,
%A Butler N,
%A Sakamoto T,
%A Torii K,
%A Barraud C,
%A Donaghy T,
%A M, Suzuki,
%A Nakagawa Y,
%A Takahashi D,
%A Tavenner T,
%A Sato R,
%A Urata Y,
%A Manchanda R,
%A Azzibrouck G,
%A Braga, João,
%A Takagishi K,
%A Yamauchi M,
%A I, Hatsukade,
%@area CEA