191 research outputs found
Afterglows from precursors in Gamma Ray Bursts. Application to the optical afterglow of GRB 091024
About 15% of Gamma Ray Bursts have precursors, i.e. emission episodes
preceding the main event, whose spectral and temporal properties are similar to
the main emission. We propose that precursors have their own fireball,
producing afterglow emission due to the dissipation of the kinetic energy via
external shock. In the time lapse between the precursor and the main event, we
assume that the central engine is not completely turned off, but it continues
to eject relativistic material at a smaller rate, whose emission is below the
background level. The precursor fireball generates a first afterglow by the
interaction with the external circumburst medium. Matter injected by the
central engine during the "quasi-quiescent" phase replenishes the external
medium with material in relativistic motion. The fireball corresponding to the
main prompt emission episode crashes with this moving material, producing a
second afterglow, and finally catches up and merges with the first precursor
fireball. We apply this new model to GRB 091024, an event with a precursor in
the prompt light curve and two well defined bumps in the optical afterglow,
obtaining an excellent agreement with the existing data.Comment: 11 pages, 6 figures, 3 tables. Accepted for publication in MNRAS,
Main Journa
The faster the narrower: characteristic bulk velocities and jet opening angles of Gamma Ray Bursts
The jet opening angle theta_jet and the bulk Lorentz factor Gamma_0 are
crucial parameters for the computation of the energetics of Gamma Ray Bursts
(GRBs). From the ~30 GRBs with measured theta_jet or Gamma_0 it is known that:
(i) the real energetic E_gamma, obtained by correcting the isotropic equivalent
energy E_iso for the collimation factor ~theta_jet^2, is clustered around
10^50-10^51 erg and it is correlated with the peak energy E_p of the prompt
emission and (ii) the comoving frame E'_p and E'_gamma are clustered around
typical values. Current estimates of Gamma_0 and theta_jet are based on
incomplete data samples and their observed distributions could be subject to
biases. Through a population synthesis code we investigate whether different
assumed intrinsic distributions of Gamma_0 and theta_jet can reproduce a set of
observational constraints. Assuming that all bursts have the same E'_p and
E'_gamma in the comoving frame, we find that Gamma_0 and theta_jet cannot be
distributed as single power-laws. The best agreement between our simulation and
the available data is obtained assuming (a) log-normal distributions for
theta_jet and Gamma_0 and (b) an intrinsic relation between the peak values of
their distributions, i.e theta_jet^2.5*Gamma_0=const. On average, larger values
of Gamma_0 (i.e. the "faster" bursts) correspond to smaller values of theta_jet
(i.e. the "narrower"). We predict that ~6% of the bursts that point to us
should not show any jet break in their afterglow light curve since they have
sin(theta_jet)<1/Gamma_0. Finally, we estimate that the local rate of GRBs is
~0.3% of all local SNIb/c and ~4.3% of local hypernovae, i.e. SNIb/c with
broad-lines.Comment: 15 pages, 8 figures, 1 table. Accepted for publication in MNRA
Spectral evolution of Fermi/GBM short Gamma-Ray Bursts
We study the spectral evolution of 13 short duration Gamma Ray Bursts (GRBs)
detected by the Gamma Burst Monitor (GBM) on board Fermi. We study spectra
resolved in time at the level of 2-512 ms in the 8 keV-35 MeV energy range. We
find a strong correlation between the observed peak energy Ep and the flux P
within individual short GRBs. The slope of the Ep P^s correlation for
individual bursts ranges between ~0.4 and ~1. There is no correlation between
the low energy spectral index and the peak energy or the flux. Our results show
that in our 13 short GRBs Ep evolves in time tracking the flux. This behavior
is similar to what found in the population of long GRBs and it is in agreement
with the evidence that long GRBs and (the still few) short GRBs with measured
redshifts follow the same rest frame Ep-Liso correlation. Its origin is most
likely to be found in the radiative mechanism that has to be the same in both
classes of GRBs.Comment: 5 pages, 1 table, 3 figures. Accepted by MNRA
Cementitious composite materials for thermal energy storage applications: a preliminary characterization and theoretical analysis
The lack of robust and low-cost sorbent materials still represents a formidable technological barrier for long-term storage of (renewable) thermal energy and more generally for Adsorptive Heat Transformations—AHT. In this work, we introduce a novel approach for synthesizing cement-based composite sorbent materials. In fact, considering the number of available hygrosopic salts that can be accommodated into a cementitious matrix—whose morphological properties can be also fine-tuned—the new proposed in situ synthesis paves the way to the generation of an entire new class of possible sorbents for AHT. Here, solely focusing on magnesium sulfate in a class G cement matrix, we show preliminary morphological, mechanical and calorimetric characterization of sub-optimal material samples. Our analysis enables us to theoretically estimate one of the most important figures of merit for the considered applications, namely the energy density which was found to range within 0.088–0.2 GJ/m3 (for the best tested sample) under reasonable operating conditions for space heating applications and temperate climate. The above estimates are found to be lower than other composite materials in the literature. Nonetheless, although no special material optimization has been implemented, our samples already compare favourably with most of the known materials in terms of specific cost of stored energy. Finally, an interesting aspect is found in the ageing tests under water sorption-desorption cycling, where a negligible variation in the adsorption capability is demonstrated after over one-hundred cycles
GRB orphan afterglows in present and future radio transient surveys
Orphan Afterglows (OA) are slow transients produced by Gamma Ray Bursts seen
off-axis that become visible on timescales of days/years at optical/NIR and
radio frequencies, when the prompt emission at high energies (X and gamma rays)
has already ceased. Given the typically estimated jet opening angle of GRBs
theta_jet ~ 3 deg, for each burst pointing to the Earth there should be a
factor ~ 700 more GRBs pointing in other directions. Despite this, no secure
OAs have been detected so far. Through a population synthesis code we study the
emission properties of the population of OA at radio frequencies. OAs reach
their emission peak on year-timescales and they last for a comparable amount of
time. The typical peak fluxes (which depend on the observing frequency) are of
few micro Jy in the radio band with only a few OA reaching the mJy level. These
values are consistent with the upper limits on the radio flux of SN Ib/c
observed at late times. We find that the OA radio number count distribution has
a typical slope -1.7 at high fluxes and a flatter (-0.4) slope at low fluxes
with a break at a frequency-dependent flux. Our predictions of the OA rates are
consistent with the (upper) limits of recent radio surveys and archive searches
for radio transients. Future radio surveys like VAST/ASKAP at 1.4 GHz should
detect ~ 3x10^-3 OA deg^-2 yr-1, MeerKAT and EVLA at 8.4 GHz should see ~
3x10^-1 OA deg-2 yr-1. The SKA, reaching the micro Jy flux limit, could see up
to ~ 0.2-1.5 OA deg^-2 yr^-1. These rates also depend on the duration of the OA
above a certain flux limit and we discuss this effect with respect to the
survey cadence.Comment: (10 pages, 5 figures, 1 table) Accepted for publication by PAS
XMM Follow-Up Observations of Three Swift BAT-Selected Active Galactic Nuclei
We present XMM-Newton observations of three AGN taken as part of a hunt to
find very heavily obscured Compton-thick AGN. For obscuring columns greater
than 10^25 cm^-2, AGN are only visible at energies below 10 keV via
reflected/scattered radiation, characterized by a flat power-law. We therefore
selected three objects (ESO 417-G006, IRAS 05218-1212, and MCG -01-05-047) from
the Swift BAT hard X-ray survey catalog with Swift X-ray Telescope XRT 0.5-10
keV spectra with flat power-law indices as candidate Compton-thick sources for
follow-up observations with the more sensitive instruments on XMM-Newton. The
XMM spectra, however, rule out reflection-dominated models based on the
weakness of the observed Fe K-alpha lines. Instead, the spectra are well-fit by
a model of a power-law continuum obscured by a Compton-thin absorber, plus a
soft excess. This result is consistent with previous follow-up observations of
two other flat-spectrum BAT-detected AGN. Thus, out of the six AGN in the
22-month BAT catalog with apparently flat Swift XRT spectra, all five that have
had follow-up observations are not likely Compton-thick. We also present new
optical spectra of two of these objects, IRAS 05218-1212 and MCG -01-05-047.
Interestingly, though both these AGN have similar X-ray spectra, their optical
spectra are completely different, adding evidence against the simplest form of
the geometric unified model of AGN. IRAS 05218-1212 appears in the optical as a
Seyfert 1, despite the ~8.5x10^22 cm^-2 line-of-sight absorbing column
indicated by its X-ray spectrum. MCG -01-05-047's optical spectrum shows no
sign of AGN activity; it appears as a normal galaxy.Comment: 18 pages including 4 figures, accepted by Ap
Two-color ionization of hydrogen by short intense pulses
Photoelectron energy spectra resulting by the interaction of hydrogen with
two short pulses having carrier frequencies, respectively, in the range of the
infrared and XUV regions have been calculated. The effects of the pulse
duration and timing of the X-ray pulse on the photoelectron energy spectra are
discussed. Analysis of the spectra obtained for very long pulses show that
certain features may be explained in terms of quantum interferences in the time
domain. It is found that, depending on the duration of the X-ray pulse, ripples
in the energy spectra separated by the infrared photon energy may appear.
Moreover, the temporal shape of the low frequency radiation field may be
inferred by the breadth of the photoelectron energy spectra.Comment: 12 pages, 8 figure
Precursors in Swift Gamma Ray Bursts with redshift
We study a sample of Gamma-Ray Bursts detected by the Swift satellite with
known redshift which show a precursor in the Swift-BAT light curve. We analyze
the spectra of the precursors and compare them with the time integrated spectra
of the prompt emission. We find neither a correlation between the two slopes
nor a tendency for the precursors spectra to be systematically harder or softer
than the prompt ones. The energetics of the precursors are large: on average,
they are just a factor of a few less energetic (in the source rest frame energy
range 15-150 keV) than the entire bursts. These properties do not depend upon
the quiescent time between the end of the precursor and the start of the main
event. These results suggest that what has been called a "precursor" is not a
phenomenon distinct from the main event, but is tightly connected with it, even
if, in some case, the quiescent time intervals can be longer than 100 seconds.Comment: 10 pages, 2 figures, 1 table. Accepted for publication by ApJ Letters
after minor revision
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