@Article{RuffiniMKORBEPPWZ:2015:ShGRBi,
               author = "Ruffini, R. and Muccino, M. and Kovacevic, M. and Oliveira, F. G. 
                         and Rueda, J. A. and Bianco, C. L. and Enderli, M. and 
                         Penacchioni, Ana Virg{\'{\i}}nia and Pisani, G. B and Wang, Y. 
                         and Zaninoni, E.",
          affiliation = "{Sapienza Universita di Roma} and {Sapienza Universita di Roma} 
                         and {Sapienza Universita di Roma} and {Sapienza Universita di 
                         Roma} and {Sapienza Universita di Roma} and {Sapienza Universita 
                         di Roma} and {Sapienza Universita di Roma} and {Instituto Nacional 
                         de Pesquisas Espaciais (INPE)} and {Sapienza Universita di Roma} 
                         and {Sapienza Universita di Roma} and {Centro Brasileiro de 
                         Pesquisas Fisicas (CBPF)}",
                title = "GRB 140619B: a short GRB from a binary neutron star merger leading 
                         to black hole formation",
              journal = "Astrophysical Journal",
                 year = "2015",
               volume = "808",
               number = "2",
                pages = "190",
                month = "Aug.",
             keywords = "gamma, ray burst: general.",
             abstract = "We show the existence of two families of short gamma-ray bursts 
                         (GRBs), both originating from the merger of binary neutron stars 
                         (NSs): family-1 with Eiso <1052erg, leading to a massive NS as the 
                         merged core, and family- 2 with Eiso >1052 erg, leading to a black 
                         hole (BH). Following the identification of the prototype GRB 
                         090227B, we present the details of a new example of family-2 short 
                         burst: GRB 140619B. From the spectral analysis of the 
                         early\∼0.2 s, we infer an observed temperature kT = 
                         (324±33) keV of the e+e--plasma at transparency (P-GRB), a 
                         theoretically derived redshift Z= 2.67±0.37, a total burst energy 
                         E tot e+e (6.03=± 0.79) 1052erg, a rest-frame peak energy Ep,i = 
                         4.7MeV, and a baryon load B = (5.52±0.73)x1052. We also estimate 
                         the corresponding emission of gravitational waves. Two additional 
                         examples of family-2 short bursts are identified: GRB 081024B and 
                         GRB 090510, remarkable for its well determined cosmological 
                         distance. We show that marked differences exist in the nature of 
                         the afterglows of these two families of short bursts: family-2 
                         bursts, leading to BH formation, consistently exhibit high energy 
                         emission following the proper-GRB emission; family-1 bursts, 
                         leading to the formation of a massive NS, should never exhibit 
                         high energy emission. We also show that both the families fulfill 
                         an Ep,i-Eiso relation with slope \γ=0.59±0.07 and a 
                         normalization constant incompatible with the one for long GRBs. 
                         The observed rate of such family-2 events is po=(2.1-1.4 
                         +2.8)x10-4Gpc-3yr-1.",
                  doi = "10.1088/0004-637X/808/2/190",
                  url = "http://dx.doi.org/10.1088/0004-637X/808/2/190",
                 issn = "0004-637X and 1538-4357",
             language = "en",
           targetfile = "2015_ruffini.pdf",
        urlaccessdate = "27 abr. 2024"
}