@Article{BragaM:2005:GlChXr,
               author = "{Sakamoto T} and {Lamb DQ} and {Kawai N} and {Yoshida A} and 
                         {Graziani C} and {Fenimore EE} and {Donaghy TQ} and {Matsuoka M} 
                         and {Suzuki M} and {Ricker G} and {Atteia JL} and {Shirasaki Y} 
                         and {Tamagawa T} and {Torii K} and {Galassi M} and {Doty J} and 
                         {Vanderspek R} and {Crew GB} and {Villasenor J} and {Butler N} and 
                         {Prigozhin G} and {Jernigan JG} and {Barraud C} and {Boer M} and 
                         {Dezalay JP} and {Olive JF} and {Hurley K} and {Levine A} and 
                         {Monnelly G} and {Martel F} and {Morgan E} and {Woosley SE} and 
                         {Cline T} and Braga, Jo{\~a}o and {Manchanda R} and {Pizzichini 
                         G} and {Takagishi K} and M, Yamauchi",
          affiliation = "Tokyo Inst Technol, Dept Phys, Meguro Ku, Tokyo, 1528551 Japan and 
                         RIKEN, Inst Phys \& Chem Res, Wako, Saitama 3510198 Japan and 
                         NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA and Univ 
                         Chicago, Dept Astron \& Astrophys, Chicago, IL 60637 USA and 
                         Aoyama Gakuin Univ, Dept Phys, Setagaya Ku, Tokyo, 1578572 Japan 
                         and Los Alamos Natl Lab, Los Alamos, NM 87545 USA and Natl Space 
                         Dev Agcy Japan, Tsukuba Space Ctr, Tsukuba, Ibaraki 3058505 Japan 
                         and MIT, Ctr Space Res, Cambridge, MA 02139 USA and Observ Midi 
                         Pyrenees, Astrophys Lab, Toulouse, F-31400 France and Natl Astron 
                         Observ, Tokyo, 1818588 Japan and Osaka Univ, Grad Sch Sci, Dept 
                         Earth \& Space Sci, Osaka, 5600043 Japan and Univ Calif Berkeley, 
                         Space Sci Lab, Berkeley, CA 94720 USA and UPS, CNRS, Ctr Etud 
                         Spatiale Rayonnements, Toulouse, F-31028 France and Univ Calif 
                         Santa Cruz, Dept Astron \& Astrophys, Santa Cruz, CA 95064 USA 
                         and Instituto Nacional de Pesquisas Espaciais, Divis{\~a}o de 
                         Geofisica Espacial(INPE,DGE) and Tata Inst Fundamental Res, Dept 
                         Astron \& Astrophys, Bombay, Maharashtra 400005 India and INAF 
                         IASF, Sez Bologna, Bologna, I-40129 Italy and Miyazaki Univ, Fac 
                         Engn, Miyazaki, 8892192 Japan",
                title = "Global characteristics of X-ray flashes and X-ray-rich gamma-ray 
                         bursts observed by HETE-2",
              journal = "Astrophysical Journal",
                 year = "2005",
               volume = "629",
               number = "1",
                pages = "311--327 Part 1",
                month = "Aug.",
             keywords = "gamma rays : bursts / JET MODEL, ENERGY, BATSE, PERFORMANCE, 
                         UNIVERSAL, DISTRIBUTIONS, XRF-020903, AFTERGLOW, SPECTRA, 
                         CATALOG.",
             abstract = "We describe and discuss the global properties of 45 gamma-ray 
                         bursts (GRBs) observed by HETE-2 during the first 3 years of its 
                         mission, focusing on the properties of X- ray flashes (XRFs) and 
                         X- ray - rich GRBs (XRRs). We find that the numbers of XRFs, XRRs, 
                         and GRBs are comparable, and that the durations and the sky 
                         distributions of XRFs and XRRs are similar to those of GRBs. We 
                         also find that the spectral properties of XRFs and XRRs are 
                         similar to those of GRBs, except that the values of the peak 
                         energy E-peak(obs) of the burst spectrum in nu F-nu, the peak 
                         energy flux F-peak, and the energy fluence S-E of XRFs are much 
                         smaller ( and those of XRRs are smaller) than those of GRBs. 
                         Finally, we find that the distributions of all three kinds of 
                         bursts form a continuum in the [S-E(2 - 30 keV), S-E(30 - 400) 
                         keV] plane, the [S-E( 2 - 400 keV), E-peak] plane, and the 
                         [F-peak(50 - 300 keV), E-peak] plane. These results provide strong 
                         evidence that all three kinds of bursts arise from the same 
                         phenomenon.",
           copyholder = "SID/SCD",
                 issn = "0004-637X and 1538-4357",
             language = "en",
           targetfile = "global characteristics.pdf",
        urlaccessdate = "05 maio 2024"
}