The American Chemical Society to launch a chemistry preprint server

Kulkarni, Sneha

doi:10.34193/ei-a-5840

Cited by 16 publications

(25 citation statements)

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“…These include the localization of GRB 050724 Prochaska et al 2006) and most likely GRB 050509b Bloom et al 2006) to bright elliptical galaxies, the lack of supernova emission in several lowredshift short GRBs (Hjorth et al 2005a;Fox et al 2005;Bloom et al 2006;Soderberg et al 2006), and the location of GRB 050709 outside of any star-forming region in its host galaxy ( Fox et al 2005). While this supports the popular notion that the progenitors are compact object binaries (DNS or NS-BH; e.g., Eichler et al 1989;Narayan et al 1992;Rosswog et al 2003), the lack of direct observations (e.g., gravitational waves or a subrelativistic, radioactive component: Li & Paczyński 1998;Kulkarni 2005) suggests that a more detailed understanding of the progenitor population has to rely on statistical studies.…”

Section: Introductionmentioning

confidence: 90%

Galaxy Clusters Associated with Short GRBs. I. The Fields of GRBs 050709, 050724, 050911, and 051221a

Berger

Shin

Mulchaey

et al. 2007

ApJ

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We present a search for galaxy clusters in the fields of three bona fide short gamma-ray bursts (050709, 050724, and 051221a) and the putative short-burst GRB 050911, using multislit optical spectroscopy. These observations are part of a long-term program to constrain the progenitor age distribution based on the fraction of short GRBs in galaxy clusters and early-type galaxies. We find no evidence for cluster associations at the redshifts of the first three bursts, but we confirm the presence of the cluster EDCC 493 within the error circle of GRB 050911 and determine its redshift, z ¼ 0:1646, and velocity dispersion, % 660 km s À1 . In addition, our analysis of Swift XRT observations of this burst reveals diffuse X-ray emission coincident with the optical cluster position, with luminosity L X % 4:9 ; 10 42 ergs s À1 and temperature kT % 0:9 keV. The inferred mass of the cluster is 2:5 ; 10 13 M , and the probability of chance coincidence is about 0.1%Y1%, indicating an association with GRB 050911 at the 2.6Y3.2 confidence level. A search for diffuse X-ray emission in coincidence with the 15 other short GRBs observed with XRT and Chandra reveals that, with the exception of the previously noted cluster ZwCl 1234.0+02916 likely associated with GRB 050509b, no additional associations are evident to a typical limit of 3 ; 10 À14 ergs s À1 cm À2 , or M P 5 ; 10 13 M , assuming a typical z ¼ 0:3. The estimated fraction of short GRBs hosted by galaxy clusters of about 5%Y20% is in rough agreement with the fraction of stellar mass in clusters of $10%Y20%.

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Section: Introductionmentioning

confidence: 90%

Galaxy Clusters Associated with Short GRBs. I. The Fields of GRBs 050709, 050724, 050911, and 051221a

Berger

Shin

Mulchaey

et al. 2007

ApJ

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“…4 is the toy model of LP98 (cf. Kulkarni 2005; ), calculated assuming an electron scattering opacity and an ‘ f ’ value = 3 × 10 −6 , as calibrated to match the radioactive heating rate in . Fig.…”

Section: Light Curvesmentioning

confidence: 99%

“… Bolometric light curve of the radioactively powered transients from NS–NS/NS–BH mergers, calculated assuming a total ejecta mass M tot = 10 −2 M ⊙ with electron fraction Y e = 0.1 and mean outflow speed v ≃ 0.1 c , and for two values of the thermalization efficiency (), ε therm = 1 (solid line) and ε therm = 0.5 (dotted line). Also shown for comparison (dashed line) is a one‐zone calculation based on the LP98 model (as implemented in Kulkarni 2005; Metzger et al 2008b) assuming f = 3 × 10 −6 (see ) and the same values for M tot and v . …”

Section: Light Curvesmentioning

confidence: 99%

“…One proposed source of relatively isotropic optical/NIR emission following a NS–NS/NS–BH merger is a supernova (SN)‐like transient powered by the radioactive decay of merger ejecta (Li & Paczyński 1998, hereafter LP98; cf. Kulkarni 2005; Metzger, Piro & Quataert 2008b). Although Type Ia supernova light curves are powered largely by the decay of 56 Ni (e.g.…”

Section: Introductionmentioning

confidence: 99%

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Electromagnetic counterparts of compact object mergers powered by the radioactive decay of r-process nuclei

Metzger¹,

Martı́nez-Pinedo²,

Darbha³

et al. 2010

Monthly Notices of the Royal Astronomical Society

1,142

1,273

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The most promising astrophysical sources of kHz gravitational waves (GWs) are the inspiral and merger of binary neutron star(NS)/black hole systems. Maximizing the scientific return of a GW detection will require identifying a coincident electromagnetic (EM) counterpart. One of the most likely sources of isotropic EM emission from compact object mergers is a supernova‐like transient powered by the radioactive decay of heavy elements synthesized in ejecta from the merger. We present the first calculations of the optical transients from compact object mergers that self‐consistently determine the radioactive heating by means of a nuclear reaction network; using this heating rate, we model the light curve with a one‐dimensional Monte Carlo radiation transfer calculation. For an ejecta mass ∼10−2 M⊙ (10−3 M⊙) the resulting light‐curve peaks on a time‐scale ∼1 d at a V‐band luminosity νLν∼ 3 × 1041 (1041) erg s−1[MV=−15(−14)]; this corresponds to an effective ‘f’ parameter ∼3 × 10−6 in the Li–Paczynski toy model. We argue that these results are relatively insensitive to uncertainties in the relevant nuclear physics and to the precise early‐time dynamics and ejecta composition. Since NS merger transients peak at a luminosity that is a factor of ∼103 higher than a typical nova, we propose naming these events ‘kilo‐novae’. Because of the rapid evolution and low luminosity of NS merger transients, EM counterpart searches triggered by GW detections will require close collaboration between the GW and astronomical communities. NS merger transients may also be detectable following a short‐duration gamma‐ray burst or ‘blindly’ with present or upcoming optical transient surveys. Because the emission produced by NS merger ejecta is powered by the formation of rare r‐process elements, current optical transient surveys can directly constrain the unknown origin of the heaviest elements in the Universe.

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“…Winds driven from deep within the BH potential well could produce relativistic jets and power late‐time central engine activity. Outflows driven from larger radii dominate the system's mass loss and may power supernova‐like optical transients through the decay of radioactive isotopes that are synthesized in the wind (Li & Paczyński 1998; Kulkarni 2005). In both cases, the mass‐loss rate and nuclear composition are critical for determining the observable signature.…”

Section: Disc Windsmentioning

confidence: 99%

Time-dependent models of accretion discs formed from compact object mergers

Metzger

Piro

Quataert

2008

Monthly Notices of the Royal Astronomical Society

216

262

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We present time‐dependent models of the remnant accretion discs created during compact object mergers, focusing on the energy available from accretion at late times and the composition of the disc and its outflows. We calculate the dynamics near the outer edge of the disc, which contains the majority of the disc's mass and determines the accretion rate on to the central black hole. This treatment allows us to follow the evolution over much longer time‐scales (100 s or longer) than current hydrodynamic simulations. At late times the disc becomes advective and its properties asymptote to self‐similar solutions with an accretion rate (neglecting outflows). This late‐time accretion can in principle provide sufficient energy to power the late‐time activity observed by Swift from some short‐duration gamma‐ray bursts. However, because outflows during the advective phase unbind the majority of the remaining mass, it is difficult for the remnant disc alone to produce significant accretion power well beyond the onset of the advective phase. Unless the viscosity is quite low (α≲ 10−3), this occurs before the start of observed flaring at ∼30 s; continued mass inflow at late times thus appears required to explain the late‐time activity from short‐duration gamma‐ray bursts. We show that the composition of the disc freezes‐out when the disc is relatively neutron rich (electron fraction Ye≃ 0.3). Roughly 10−2 M⊙ of this neutron‐rich material is ejected by winds at late times. During earlier, neutrino‐cooled phases of accretion, neutrino irradiation of the disc produces a wind with Ye≃ 0.5, which synthesizes at most ∼10−3 M⊙ of 56Ni. We highlight what conditions are favorable for 56Ni production and predict, in the best cases, optical and infrared transients peaking ∼0.5–2 d after the burst, with fluxes a factor of ∼10 below the current observational limits.

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The American Chemical Society to launch a chemistry preprint server

Cited by 16 publications

References 0 publications

Galaxy Clusters Associated with Short GRBs. I. The Fields of GRBs 050709, 050724, 050911, and 051221a

Galaxy Clusters Associated with Short GRBs. I. The Fields of GRBs 050709, 050724, 050911, and 051221a

Electromagnetic counterparts of compact object mergers powered by the radioactive decay of r-process nuclei

Time-dependent models of accretion discs formed from compact object mergers

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