共查询到20条相似文献,搜索用时 15 毫秒
1.
Hjorth J Watson D Fynbo JP Price PA Jensen BL Jørgensen UG Kubas D Gorosabel J Jakobsson P Sollerman J Pedersen K Kouveliotou C 《Nature》2005,437(7060):859-861
It has long been known that there are two classes of gamma-ray bursts (GRBs), mainly distinguished by their durations. The breakthrough in our understanding of long-duration GRBs (those lasting more than approximately 2 s), which ultimately linked them with energetic type Ic supernovae, came from the discovery of their long-lived X-ray and optical 'afterglows', when precise and rapid localizations of the sources could finally be obtained. X-ray localizations have recently become available for short (duration <2 s) GRBs, which have evaded optical detection for more than 30 years. Here we report the first discovery of transient optical emission (R-band magnitude approximately 23) associated with a short burst: GRB 050709. The optical afterglow was localized with subarcsecond accuracy, and lies in the outskirts of a blue dwarf galaxy. The optical and X-ray afterglow properties 34 h after the GRB are reminiscent of the afterglows of long GRBs, which are attributable to synchrotron emission from ultrarelativistic ejecta. We did not, however, detect a supernova, as found in most nearby long GRB afterglows, which suggests a different origin for the short GRBs. 相似文献
2.
Villasenor JS Lamb DQ Ricker GR Atteia JL Kawai N Butler N Nakagawa Y Jernigan JG Boer M Crew GB Donaghy TQ Doty J Fenimore EE Galassi M Graziani C Hurley K Levine A Martel F Matsuoka M Olive JF Prigozhin G Sakamoto T Shirasaki Y Suzuki M Tamagawa T Vanderspek R Woosley SE Yoshida A Braga J Manchanda R Pizzichini G Takagishi K Yamauchi M 《Nature》2005,437(7060):855-858
Gamma-ray bursts (GRBs) fall into two classes: short-hard and long-soft bursts. The latter are now known to have X-ray and optical afterglows, to occur at cosmological distances in star-forming galaxies, and to be associated with the explosion of massive stars. In contrast, the distance scale, the energy scale and the progenitors of the short bursts have remained a mystery. Here we report the discovery of a short-hard burst whose accurate localization has led to follow-up observations that have identified the X-ray afterglow and (for the first time) the optical afterglow of a short-hard burst; this in turn led to the identification of the host galaxy of the burst as a late-type galaxy at z = 0.16 (ref. 10). These results show that at least some short-hard bursts occur at cosmological distances in the outskirts of galaxies, and are likely to be caused by the merging of compact binaries. 相似文献
3.
Greiner J Klose S Reinsch K Schmid HM Sari R Hartmann DH Kouveliotou C Rau A Palazzi E Straubmeier C Stecklum B Zharikov S Tovmassian G Bärnbantner O Ries C Jehin E Henden A Kaas AA Grav T Hjorth J Pedersen H Wijers RA Kaufer A Park HS Williams G Reimer O 《Nature》2003,426(6963):157-159
The association of a supernova with GRB030329 strongly supports the 'collapsar' model of gamma-ray bursts, where a relativistic jet forms after the progenitor star collapses. Such jets cannot be spatially resolved because gamma-ray bursts lie at cosmological distances; their existence is instead inferred from 'breaks' in the light curves of the afterglows, and from the theoretical desire to reduce the estimated total energy of the burst by proposing that most of it comes out in narrow beams. Temporal evolution of the polarization of the afterglows may provide independent evidence for the jet structure of the relativistic outflow. Small-level polarization ( approximately 1-3 per cent) has been reported for a few bursts, but its temporal evolution has yet to be established. Here we report polarimetric observations of the afterglow of GRB030329. We establish the polarization light curve, detect sustained polarization at the per cent level, and find significant variability. The data imply that the afterglow magnetic field has a small coherence length and is mostly random, probably generated by turbulence, in contrast with the picture arising from the high polarization detected in the prompt gamma-rays from GRB021206 (ref. 18). 相似文献
4.
Gehrels N Sarazin CL O'Brien PT Zhang B Barbier L Barthelmy SD Blustin A Burrows DN Cannizzo J Cummings JR Goad M Holland ST Hurkett CP Kennea JA Levan A Markwardt CB Mason KO Meszaros P Page M Palmer DM Rol E Sakamoto T Willingale R Angelini L Beardmore A Boyd PT Breeveld A Campana S Chester MM Chincarini G Cominsky LR Cusumano G de Pasquale M Fenimore EE Giommi P Gronwall C Grupe D Hill JE Hinshaw D Hjorth J Hullinger D Hurley KC Klose S Kobayashi S Kouveliotou C Krimm HA Mangano V 《Nature》2005,437(7060):851-854
Gamma-ray bursts (GRBs) come in two classes: long (> 2 s), soft-spectrum bursts and short, hard events. Most progress has been made on understanding the long GRBs, which are typically observed at high redshift (z approximately 1) and found in subluminous star-forming host galaxies. They are likely to be produced in core-collapse explosions of massive stars. In contrast, no short GRB had been accurately (< 10') and rapidly (minutes) located. Here we report the detection of the X-ray afterglow from--and the localization of--the short burst GRB 050509B. Its position on the sky is near a luminous, non-star-forming elliptical galaxy at a redshift of 0.225, which is the location one would expect if the origin of this GRB is through the merger of neutron-star or black-hole binaries. The X-ray afterglow was weak and faded below the detection limit within a few hours; no optical afterglow was detected to stringent limits, explaining the past difficulty in localizing short GRBs. 相似文献
5.
Fox DB Frail DA Price PA Kulkarni SR Berger E Piran T Soderberg AM Cenko SB Cameron PB Gal-Yam A Kasliwal MM Moon DS Harrison FA Nakar E Schmidt BP Penprase B Chevalier RA Kumar P Roth K Watson D Lee BL Shectman S Phillips MM Roth M McCarthy PJ Rauch M Cowie L Peterson BA Rich J Kawai N Aoki K Kosugi G Totani T Park HS MacFadyen A Hurley KC 《Nature》2005,437(7060):845-850
The final chapter in the long-standing mystery of the gamma-ray bursts (GRBs) centres on the origin of the short-hard class of bursts, which are suspected on theoretical grounds to result from the coalescence of neutron-star or black-hole binary systems. Numerous searches for the afterglows of short-hard bursts have been made, galvanized by the revolution in our understanding of long-duration GRBs that followed the discovery in 1997 of their broadband (X-ray, optical and radio) afterglow emission. Here we present the discovery of the X-ray afterglow of a short-hard burst, GRB 050709, whose accurate position allows us to associate it unambiguously with a star-forming galaxy at redshift z = 0.160, and whose optical lightcurve definitively excludes a supernova association. Together with results from three other recent short-hard bursts, this suggests that short-hard bursts release much less energy than the long-duration GRBs. Models requiring young stellar populations, such as magnetars and collapsars, are ruled out, while coalescing degenerate binaries remain the most promising progenitor candidates. 相似文献
6.
Soderberg AM Kulkarni SR Berger E Fox DW Sako M Frail DA Gal-Yam A Moon DS Cenko SB Yost SA Phillips MM Persson SE Freedman WL Wyatt P Jayawardhana R Paulson D 《Nature》2004,430(7000):648-650
Over the six years since the discovery of the gamma-ray burst GRB 980425, which was associated with the nearby (distance approximately 40 Mpc) supernova 1998bw, astronomers have debated fiercely the nature of this event. Relative to bursts located at cosmological distance (redshift z approximately 1), GRB 980425 was under-luminous in gamma-rays by three orders of magnitude. Radio calorimetry showed that the explosion was sub-energetic by a factor of 10. Here we report observations of the radio and X-ray afterglow of the recent GRB 031203 (refs 5-7), which has a redshift of z = 0.105. We demonstrate that it too is sub-energetic which, when taken together with the low gamma-ray luminosity, suggests that GRB 031203 is the first cosmic analogue to GRB 980425. We find no evidence that this event was a highly collimated explosion viewed off-axis. Like GRB 980425, GRB 031203 appears to be an intrinsically sub-energetic gamma-ray burst. Such sub-energetic events have faint afterglows. We expect intensive follow-up of faint bursts with smooth gamma-ray light curves (common to both GRB 031203 and 980425) to reveal a large population of such events. 相似文献
7.
Racusin JL Karpov SV Sokolowski M Granot J Wu XF Pal'shin V Covino S van der Horst AJ Oates SR Schady P Smith RJ Cummings J Starling RL Piotrowski LW Zhang B Evans PA Holland ST Malek K Page MT Vetere L Margutti R Guidorzi C Kamble AP Curran PA Beardmore A Kouveliotou C Mankiewicz L Melandri A O'Brien PT Page KL Piran T Tanvir NR Wrochna G Aptekar RL Barthelmy S Bartolini C Beskin GM Bondar S Bremer M Campana S Castro-Tirado A Cucchiara A Cwiok M D'Avanzo P D'Elia V Valle MD de Ugarte Postigo A 《Nature》2008,455(7210):183-188
Long-duration gamma-ray bursts (GRBs) release copious amounts of energy across the entire electromagnetic spectrum, and so provide a window into the process of black hole formation from the collapse of massive stars. Previous early optical observations of even the most exceptional GRBs (990123 and 030329) lacked both the temporal resolution to probe the optical flash in detail and the accuracy needed to trace the transition from the prompt emission within the outflow to external shocks caused by interaction with the progenitor environment. Here we report observations of the extraordinarily bright prompt optical and gamma-ray emission of GRB 080319B that provide diagnostics within seconds of its formation, followed by broadband observations of the afterglow decay that continued for weeks. We show that the prompt emission stems from a single physical region, implying an extremely relativistic outflow that propagates within the narrow inner core of a two-component jet. 相似文献
8.
Gehrels N Norris JP Barthelmy SD Granot J Kaneko Y Kouveliotou C Markwardt CB Mészáros P Nakar E Nousek JA O'Brien PT Page M Palmer DM Parsons AM Roming PW Sakamoto T Sarazin CL Schady P Stamatikos M Woosley SE 《Nature》2006,444(7122):1044-1046
Gamma-ray bursts (GRBs) are known to come in two duration classes, separated at approximately 2 s. Long-duration bursts originate from star-forming regions in galaxies, have accompanying supernovae when these are near enough to observe and are probably caused by massive-star collapsars. Recent observations show that short-duration bursts originate in regions within their host galaxies that have lower star-formation rates, consistent with binary neutron star or neutron star-black hole mergers. Moreover, although their hosts are predominantly nearby galaxies, no supernovae have been so far associated with short-duration GRBs. Here we report that the bright, nearby GRB 060614 does not fit into either class. Its approximately 102-s duration groups it with long-duration GRBs, while its temporal lag and peak luminosity fall entirely within the short-duration GRB subclass. Moreover, very deep optical observations exclude an accompanying supernova, similar to short-duration GRBs. This combination of a long-duration event without an accompanying supernova poses a challenge to both the collapsar and the merging-neutron-star interpretations and opens the door to a new GRB classification scheme that straddles both long- and short-duration bursts. 相似文献
9.
Price PA Fox DW Kulkarni SR Peterson BA Schmidt BP Soderberg AM Yost SA Berger E Djorgovski SG Frail DA Harrison FA Sari R Blain AW Chapman SC 《Nature》2003,423(6942):844-847
Past studies of cosmological gamma-ray bursts (GRBs) have been hampered by their extreme distances, resulting in faint afterglows. A nearby GRB could potentially shed much light on the origin of these events, but GRBs with a redshift z 相似文献
10.
Reeves JN Watson D Osborne JP Pounds KA O'Brien PT Short AD Turner MJ Watson MG Mason KO Ehle M Schartel N 《Nature》2002,416(6880):512-515
Now that gamma-ray bursts (GRBs) have been determined to lie at cosmological distances, their isotropic burst energies are estimated to be as high as 1054 erg (ref. 2), making them the most energetic phenomena in the Universe. The nature of the progenitors responsible for the bursts remains, however, elusive. The favoured models range from the merger of two neutron stars in a binary system to the collapse of a massive star. Spectroscopic studies of the afterglow emission could reveal details of the environment of the burst, by indicating the elements present, the speed of the outflow and an estimate of the temperature. Here we report an X-ray spectrum of the afterglow of GRB011211, which shows emission lines of magnesium, silicon, sulphur, argon, calcium and possibly nickel, arising in metal-enriched material with an outflow velocity of the order of one-tenth the speed of light. These observations strongly favour models where a supernova explosion from a massive stellar progenitor precedes the burst event and is responsible for the outflowing matter. 相似文献
11.
Gal-Yam A Fox DB Price PA Ofek EO Davis MR Leonard DC Soderberg AM Schmidt BP Lewis KM Peterson BA Kulkarni SR Berger E Cenko SB Sari R Sharon K Frail D Moon DS Brown PJ Cucchiara A Harrison F Piran T Persson SE McCarthy PJ Penprase BE Chevalier RA MacFadyen AI 《Nature》2006,444(7122):1053-1055
Over the past decade, our physical understanding of gamma-ray bursts (GRBs) has progressed rapidly, thanks to the discovery and observation of their long-lived afterglow emission. Long-duration (> 2 s) GRBs are associated with the explosive deaths of massive stars ('collapsars', ref. 1), which produce accompanying supernovae; the short-duration (< or = 2 s) GRBs have a different origin, which has been argued to be the merger of two compact objects. Here we report optical observations of GRB 060614 (duration approximately 100 s, ref. 10) that rule out the presence of an associated supernova. This would seem to require a new explosive process: either a massive collapsar that powers a GRB without any associated supernova, or a new type of 'engine', as long-lived as the collapsar but without a massive star. We also show that the properties of the host galaxy (redshift z = 0.125) distinguish it from other long-duration GRB hosts and suggest that an entirely new type of GRB progenitor may be required. 相似文献
12.
考虑同步自吸收效应后,讨论了Gamma射线暴余辉的谱并展示了Gamma射线暴GRB970508余辉在光学波段的光变曲线,尽管光学余辉很复杂,所得到的结果仍然与观测结果符合的很好,因此不管是在火球+激波模型还是在喷流模型中,都应该全面地研究同步自吸收效应和内部能源机制,以使理论计算更好的拟合观测到的光变曲线。 相似文献
13.
Uemura M Kato T Ishioka R Yamaoka H Monard B Nogami D Maehara H Sugie A Takahashi S 《Nature》2003,423(6942):843-844
Gamma-ray bursts (GRBs) are energetic explosions that for 0.01-100 s are the brightest gamma-ray sources in the sky. Observations of the early evolution of afterglows are expected to provide clues about the nature of the bursts, but their rapid fading has hampered such studies; some recent rapid localizations of bursts have improved the situation. Here we report an early detection of the very bright afterglow of the burst of 29 March 2003 (GRB030329). Our data show that, even early in the afterglow phase, the light curve shows unexpectedly complicated structures superimposed on the fading background. 相似文献
14.
Campana S Lodato G D'Avanzo P Panagia N Rossi EM Della Valle M Tagliaferri G Antonelli LA Covino S Ghirlanda G Ghisellini G Melandri A Pian E Salvaterra R Cusumano G D'Elia V Fugazza D Palazzi E Sbarufatti B Vergani SD 《Nature》2011,480(7375):69-71
The tidal disruption of a solar-mass star around a supermassive black hole has been extensively studied analytically and numerically. In these events, the star develops into an elongated banana-shaped structure. After completing an eccentric orbit, the bound debris falls into the black hole, forming an accretion disk and emitting radiation. The same process may occur on planetary scales if a minor body passes too close to its star. In the Solar System, comets fall directly into our Sun or onto planets. If the star is a compact object, the minor body can become tidally disrupted. Indeed, one of the first mechanisms invoked to produce strong gamma-ray emission involved accretion of comets onto neutron stars in our Galaxy. Here we report that the peculiarities of the 'Christmas' gamma-ray burst (GRB 101225A) can be explained by a tidal disruption event of a minor body around an isolated Galactic neutron star. This would indicate either that minor bodies can be captured by compact stellar remnants more frequently than occurs in the Solar System or that minor-body formation is relatively easy around millisecond radio pulsars. A peculiar supernova associated with a gamma-ray burst provides an alternative explanation. 相似文献
15.
Kawai N Kosugi G Aoki K Yamada T Totani T Ohta K Iye M Hattori T Aoki W Furusawa H Hurley K Kawabata KS Kobayashi N Komiyama Y Mizumoto Y Nomoto K Noumaru J Ogasawara R Sato R Sekiguchi K Shirasaki Y Suzuki M Takata T Tamagawa T Terada H Watanabe J Yatsu Y Yoshida A 《Nature》2006,440(7081):184-186
The prompt gamma-ray emission from gamma-ray bursts (GRBs) should be detectable out to distances of z > 10 (ref. 1), and should therefore provide an excellent probe of the evolution of cosmic star formation, reionization of the intergalactic medium, and the metal enrichment history of the Universe. Hitherto, the highest measured redshift for a GRB has been z = 4.50 (ref. 5). Here we report the optical spectrum of the afterglow of GRB 050904 obtained 3.4 days after the burst; the spectrum shows a clear continuum at the long-wavelength end of the spectrum with a sharp cut-off at around 9,000 A due to Lyman alpha absorption at z approximately 6.3 (with a damping wing). A system of absorption lines of heavy elements at z = 6.295 +/- 0.002 was also detected, yielding the precise measurement of the redshift. The Si ii fine-structure lines suggest a dense, metal-enriched environment around the progenitor of the GRB. 相似文献
16.
Observations of the afterglows of gamma-ray bursts (GRBs) have revealed that they lie at cosmological distances, and so correspond to the release of an enormous amount of energy. The nature of the central engine that powers these events and the prompt gamma-ray emission mechanism itself remain enigmatic because, once a relativistic fireball is created, the physics of the afterglow is insensitive to the nature of the progenitor. Here we report the discovery of linear polarization in the prompt gamma-ray emission from GRB021206, which indicates that it is synchrotron emission from relativistic electrons in a strong magnetic field. The polarization is at the theoretical maximum, which requires a uniform, large-scale magnetic field over the gamma-ray emission region. A large-scale magnetic field constrains possible progenitors to those either having or producing organized fields. We suggest that the large magnetic energy densities in the progenitor environment (comparable to the kinetic energy densities of the fireball), combined with the large-scale structure of the field, indicate that magnetic fields drive the GRB explosion. 相似文献
17.
Tagliaferri G Goad M Chincarini G Moretti A Campana S Burrows DN Perri M Barthelmy SD Gehrels N Krimm H Sakamoto T Kumar P Mészáros PI Kobayashi S Zhang B Angelini L Banat P Beardmore AP Capalbi M Covino S Cusumano G Giommi P Godet O Hill JE Kennea JA Mangano V Morris DC Nousek JA O'Brien PT Osborne JP Pagani C Page KL Romano P Stella L Wells A 《Nature》2005,436(7053):985-988
'Long' gamma-ray bursts (GRBs) are commonly accepted to originate in the explosion of particularly massive stars, which give rise to highly relativistic jets. Inhomogeneities in the expanding flow result in internal shock waves that are believed to produce the gamma-rays we see. As the jet travels further outward into the surrounding circumstellar medium, 'external' shocks create the afterglow emission seen in the X-ray, optical and radio bands. Here we report observations of the early phases of the X-ray emission of five GRBs. Their X-ray light curves are characterised by a surprisingly rapid fall-off for the first few hundred seconds, followed by a less rapid decline lasting several hours. This steep decline, together with detailed spectral properties of two particular bursts, shows that violent shock interactions take place in the early jet outflows. 相似文献
18.
Vestrand WT Wren JA Wozniak PR Aptekar R Golentskii S Pal'shin V Sakamoto T White RR Evans S Casperson D Fenimore E 《Nature》2006,442(7099):172-175
The taxonomy of optical emission detected during the critical first few minutes after the onset of a gamma-ray burst (GRB) defines two broad classes: prompt optical emission correlated with prompt gamma-ray emission, and early optical afterglow emission uncorrelated with the gamma-ray emission. The standard theoretical interpretation attributes prompt emission to internal shocks in the ultra-relativistic outflow generated by the internal engine; early afterglow emission is attributed to shocks generated by interaction with the surrounding medium. Here we report on observations of a bright GRB that, for the first time, clearly show the temporal relationship and relative strength of the two optical components. The observations indicate that early afterglow emission can be understood as reverberation of the energy input measured by prompt emission. Measurements of the early afterglow reverberations therefore probe the structure of the environment around the burst, whereas the subsequent response to late-time impulsive energy releases reveals how earlier flaring episodes have altered the jet and environment parameters. Many GRBs are generated by the death of massive stars that were born and died before the Universe was ten per cent of its current age, so GRB afterglow reverberations provide clues about the environments around some of the first stars. 相似文献
19.
Fox DW Yost S Kulkarni SR Torii K Kato T Yamaoka H Sako M Harrison FA Sari R Price PA Berger E Soderberg AM Djorgovski SG Barth AJ Pravdo SH Frail DA Gal-Yam A Lipkin Y Mauch T Harrison C Buttery H 《Nature》2003,422(6929):284-286
Observations of the long-lived emission--or 'afterglow'--of long-duration gamma-ray bursts place them at cosmological distances, but the origin of these energetic explosions remains a mystery. Observations of optical emission contemporaneous with the burst of gamma-rays should provide insight into the details of the explosion, as well as into the structure of the surrounding environment. One bright optical flash was detected during a burst, but other efforts have produced negative results. Here we report the discovery of the optical counterpart of GRB021004 only 193 seconds after the event. The initial decline is unexpectedly slow and requires varying energy content in the gamma-ray burst blastwave over the course of the first hour. Further analysis of the X-ray and optical afterglow suggests additional energy variations over the first few days. 相似文献
20.
Hjorth J Sollerman J Møller P Fynbo JP Woosley SE Kouveliotou C Tanvir NR Greiner J Andersen MI Castro-Tirado AJ Castro Cerón JM Fruchter AS Gorosabel J Jakobsson P Kaper L Klose S Masetti N Pedersen H Pedersen K Pian E Palazzi E Rhoads JE Rol E van den Heuvel EP Vreeswijk PM Watson D Wijers RA 《Nature》2003,423(6942):847-850
Over the past five years evidence has mounted that long-duration (>2 s) gamma-ray bursts (GRBs)-the most luminous of all astronomical explosions-signal the collapse of massive stars in our Universe. This evidence was originally based on the probable association of one unusual GRB with a supernova, but now includes the association of GRBs with regions of massive star formation in distant galaxies, the appearance of supernova-like 'bumps' in the optical afterglow light curves of several bursts and lines of freshly synthesized elements in the spectra of a few X-ray afterglows. These observations support, but do not yet conclusively demonstrate, the idea that long-duration GRBs are associated with the deaths of massive stars, presumably arising from core collapse. Here we report evidence that a very energetic supernova (a hypernova) was temporally and spatially coincident with a GRB at redshift z = 0.1685. The timing of the supernova indicates that it exploded within a few days of the GRB, strongly suggesting that core-collapse events can give rise to GRBs, thereby favouring the 'collapsar' model. 相似文献