The central engine of GRB 130831A and the energy breakdown of a relativistic explosion
Por:
De Pasquale, M., Oates, S. R., Racusin, J. L., Kann, D. A., Zhang, B., Pozanenko, A., Volnova, A. A., Trotter, A., Frank, N., Cucchiara, A., Troja, E., Sbarufatti, B., Butler, N. R., Schulze, S., Cano, Z., Page, M. J., Castro-Tirado, A. J., Gorosabel, J., Lien, A., Fox, O., Littlejohns, O., Bloom, J. S., Prochaska, J. X., de Diego, J. A., Gonzalez, J., Richer, M. G., Roman-Zuniga, C., Watson, A. M., Gehrels, N., Moseley, H., Kutyrev, A., Zane, S., Hoette, V., Russell, R. R., Rumyantsev, V., Klunko, E., Burkhonov, O., Breeveld, A. A., Reichart, D. E., Haislip, J. B.
Publicada:
1 ene 2016
Resumen:
Gamma-ray bursts (GRBs) are the most luminous explosions in the Universe, yet the nature and physical properties of their energy sources are far from understood. Very important clues, however, can be inferred by studying the afterglows of these events. We present optical and X-ray observations of GRB 130831A obtained by Swift, Chandra, Skynet, Reionization And Transients Infra-Red camera, Maidanak, International Scientific Optical-Observation Network, Nordic Optical Telescope, Liverpool Telescope and Gran Telescopio Canarias. This burst shows a steep drop in the X-ray light curve at ?105 s after the trigger, with a power-law decay index of a ~6. Such a rare behaviour cannot be explained by the standard forward shock (FS) model and indicates that the emission, up to the fast decay at 105 s, must be of 'internal origin', produced by a dissipation process within an ultrarelativistic outflow. We propose that the source of such an outflow, which must produce the X-ray flux for ?1 d in the cosmological rest frame, is a newly born magnetar or black hole. After the drop, the faint X-ray afterglow continues with a much shallower decay. The optical emission, on the other hand, shows no break across the X-ray steep decrease, and the late-time decays of both the X-ray and optical are consistent. Using both the X-ray and optical data, we show that the emission after ?105 s can be explained well by the FS model. We model our data to derive the kinetic energy of the ejecta and thus measure the efficiency of the central engine of a GRB with emission of internal origin visible for a long time. Furthermore, we break down the energy budget of this GRB into the prompt emission, the late internal dissipation, the kinetic energy of the relativistic ejecta, and compare it with the energy of the associated supernova, SN 2013 fu. © 2015 The Authors.
Filiaciones:
De Pasquale, M.:
Univ Coll London, Mullard Space Sci Lab, Dorking RH5 6NT, Surrey, England
Ist Astrofis Spaziale Fis Cosm, I-90146 Palermo, Italy
Ist Euro Mediterraneo Sci & Tecnol, I-90139 Palermo, Italy
Oates, S. R.:
Univ Coll London, Mullard Space Sci Lab, Dorking RH5 6NT, Surrey, England
CSIC, Ist Astrofis Andalucia, E-18008 Granada, Spain
Racusin, J. L.:
CRESST, Greenbelt, MD 20771 USA
Kann, D. A.:
Thuringer Landessternwarte Tautenburg, D-07778 Tautenburg, Germany
Zhang, B.:
Univ Nevada, Dept Phys & Astron, Las Vegas, NV 89154 USA
Pozanenko, A.:
Space Res Inst IKI, Moscow 117997, Russia
Natl Res Nucl Univ MEPhI, Moscow Engn Phys Inst, Moscow 115409, Russia
Volnova, A. A.:
Space Res Inst IKI, Moscow 117997, Russia
Trotter, A.:
Univ N Carolina, Chapel Hill, NC 27599 USA
Frank, N.:
Univ N Carolina, Chapel Hill, NC 27599 USA
Cucchiara, A.:
CRESST, Greenbelt, MD 20771 USA
NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA
Troja, E.:
CRESST, Greenbelt, MD 20771 USA
NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA
Sbarufatti, B.:
Penn State Univ, University Pk, PA 16802 USA
Butler, N. R.:
Arizona State Univ, Tempe, AZ 85281 USA
Schulze, S.:
Pontificia Univ Catolica Chile, Fac Fis, Inst Astrofis, Santiago 7820436, Chile
Millennium Inst Astrophys, Santiago 7820436, Chile
Cano, Z.:
Univ Iceland, Inst Sci, Ctr Astrophys & Cosmol, IS-107 Reykjavik, Iceland
Page, M. J.:
Univ Coll London, Mullard Space Sci Lab, Dorking RH5 6NT, Surrey, England
Castro-Tirado, A. J.:
Univ Malaga, Unidad Asociada, Dept Ingn Sistemas & Automat, E-29071 Malaga, Spain
Gorosabel, J.:
Univ Basque Country, Unidad Asociada, Grp Ciencia Planetarias, Dept Fis Aplicada 1,ETS Ingn,UPV EHU IAA CSIC, E-48013 Bilbao, Spain
Ikerbasque, Basque Fdn Sci, E-48008 Bilbao, Spain
Lien, A.:
CRESST, Greenbelt, MD 20771 USA
NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA
Univ Maryland, Dept Phys, Baltimore, MD 21250 USA
Fox, O.:
Univ Calif Berkeley, Berkeley, CA 94720 USA
Littlejohns, O.:
Arizona State Univ, Tempe, AZ 85281 USA
Bloom, J. S.:
Univ Calif Berkeley, Berkeley, CA 94720 USA
Prochaska, J. X.:
Univ Calif Santa Cruz, Santa Cruz, CA 95064 USA
de Diego, J. A.:
Univ Nacl Autonoma Mexico, Inst Astron, Mexico City 04510, DF, Mexico
Gonzalez, J.:
Univ Nacl Autonoma Mexico, Inst Astron, Mexico City 04510, DF, Mexico
Roman-Zuniga, C.:
Univ Nacl Autonoma Mexico, Inst Astron, Ensenada 22800, Baja California, Mexico
Watson, A. M.:
Univ Nacl Autonoma Mexico, Inst Astron, Mexico City 04510, DF, Mexico
Gehrels, N.:
CRESST, Greenbelt, MD 20771 USA
NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA
Moseley, H.:
CRESST, Greenbelt, MD 20771 USA
NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA
Kutyrev, A.:
CRESST, Greenbelt, MD 20771 USA
NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA
Zane, S.:
Univ Coll London, Mullard Space Sci Lab, Dorking RH5 6NT, Surrey, England
Hoette, V.:
Univ Chicago, Chicago, IL 60637 USA
Russell, R. R.:
Univ Chicago, Chicago, IL 60637 USA
Rumyantsev, V.:
Crimean Astrophys Observ, UA-98409 Pgt Nauchny, Crimea, Ukraine
Klunko, E.:
Russian Acad Sci, Inst Solar Terr Phys, Irkutsk 664033, Russia
Burkhonov, O.:
Ulugh Beg Astron Inst, Tashkent, Uzbekistan
Breeveld, A. A.:
Univ Coll London, Mullard Space Sci Lab, Dorking RH5 6NT, Surrey, England
Reichart, D. E.:
Univ N Carolina, Chapel Hill, NC 27599 USA
Haislip, J. B.:
Univ N Carolina, Chapel Hill, NC 27599 USA
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