825 research outputs found
Multi-GeV Neutrino Emission from Magnetized Gamma Ray Bursts
We investigate the expected neutrino emissivity from nuclear collisions in
magnetically dominated collisional models of gamma-ray bursts, motivated by
recent observational and theoretical developments. The results indicate that
significant multi-GeV neutrino fluxes are expected for model parameter values
which are typical of electromagnetically detected bursts. We show that for
detecting at least one muon event in Icecube and its Deep Core sub-array, a
single burst must be near the high end of the luminosity function and at a
redshift . We also calculate the luminosity and distance ranges
that can generate muon events per GRB in the same detectors, which may
be of interest if simultaneously detected electromagnetically, or if measured
with future extensions of Icecube or other neutrino detectors with larger
effective volume and better sensitivity.Comment: 12 pages, 7 figures, accepted version for Phys.Rev.
Photon acceleration in variable ultra-relativistic outflows and high-energy spectra of Gamma-Ray Bursts
MeV seed photons produced in shocks in a variable ultra-relativistic outflow
gain energy by the Fermi mechanism, because the photons Compton scatter off
relativistically colliding shells. The Fermi-modified high-energy photon
spectrum has a non-universal slope and a universal cutoff. A significant
increase in the total radiative efficiency is possible. In some gamma ray
bursts, most of the power might be emitted at the high-energy cutoff for this
mechanism, which would be close to 100 MeV for outflows with a mean bulk
Lorentz factor of 100.Comment: 8 pages, submitted to ApJ
Physical parameters and emission mechanism in Gamma-Ray Bursts
Detailed information on the physical parameters in the sources of
cosmological Gamma-Ray Bursts (GRBs) is obtained from few plausible assumptions
consistent with observations. Model-independent requirements posed by these
assumptions on the emission mechanism in GRBs are formulated. It is found that
the observed radiation in sub-MeV energy range is generated by the synchrotron
emission mechanism, though about ten per cent of the total GRB energy should be
converted via the inverse Compton process into ultra-hard spectral domain
(above 100 GeV). We estimate the magnetic field strength in the emitting
region, the Lorentz factor of accelerated electrons, and the typical energy of
IC photons.
We show that there is a "line-of-death" relation for GRBs and derive from
this relation the lower limits on both GRB duration and GRB variability
timescale. The upper limit on the Lorentz factor of GRB fireballs is also
found. We demonstrate that steady-state electron distribution consistent with
the Compton losses may produce different spectral indices, e.g., 3/4 as opposed
to the figure 1/2 widely discussed in the literature. It is suggested that the
changes in the decline rate observed in the lightcurves of several GRB
afterglows may be due to the time evolution of spectral break, which appears in
the synchrotron emission generated by steady-state self-consistent electron
distribution.Comment: Journal reference added, introduction extended, minor changes in
notation
Hidden source of high-energy neutrinos in collapsing galactic nucleus
We propose the model of a short-lived very powerful source of high energy
neutrinos. It is formed as a result of the dynamical evolution of a galactic
nucleus prior to its collapse into a massive black hole and formation of
high-luminosity AGN. This stage can be referred to as ``pre-AGN''. A dense
central stellar cluster in the galactic nucleus on the late stage of evolution
consists of compact stars (neutron stars and stellar mass black holes). This
cluster is sunk deep into massive gas envelope produced by destructive
collisions of a primary stellar population. Frequent collisions of neutron
stars in a central stellar cluster are accompanied by the generation of
ultrarelativistic fireballs and shock waves. These repeating fireballs result
in a formation of the expanding rarefied cavity inside the envelope. The
charged particles are effectively accelerated in the cavity and, due to
pp-collisions in the gas envelope, they produce high energy neutrinos. All high
energy particles, except neutrinos, are absorbed in the thick envelope.
Duration of this pre-AGN phase is about 10 yr, the number of the sources can be
\~ 10 per cosmological horizon. High energy neutrino signal can be detected by
underground neutrino telescope with effective area ~1 km^2.Comment: small changes, to be published in Astroparticle Physic
Theory of photospheric emission from relativistic outflows
In this paper we reexamine the optical depth of ultrarelativistic spherically
symmetric outflows and reevaluate the photospheric radius for each model during
both the acceleration and coasting phases. It is shown that for both the wind
and the shell models there are two asymptotic solutions for the optical depth
during the coasting phase of the outflow. In particular we show that quite
counterintuitively a geometrically thin shell may appear as a thick wind for
photons propagating inside it. For this reason we introduce notions of photon
thick and photon thin outflows, which appear more general and better physically
motivated with respect to winds and shells. Photosphere of relativistic outflow
is a dynamic surface. We study its geometry and find that the photosphere of
photon thin outflow has always a convex shape, while in the photon thick one it
is initially convex (there is always a photon thin layer in any outflow) and
then it becomes concave asymptotically approaching the photosphere of an
infinitely long wind. We find that both instantaneous and time integrated
observed spectra are very close to the thermal one for photon thick outflows,
in line with existing studies. It is our main finding that the photospheric
emission from the photon thin outflow produces non thermal time integrated
spectra, which may be described by the Band function well known in the GRB
literature. We find that energetic GRBs should produce photon thin outflows
with photospheric emission lasting less than one second for the total energy
erg and baryonic loading parameter . It means
that only time integrated spectra may be observed from such GRBs.Comment: Revision of the previous version, new effect is discussed.
Conclusions remain unchange
Radiative cooling in relativistic collisionless shocks. Can simulations and experiments probe relevant GRB physics?
We address the question of whether numerical particle-in-cell (PIC)
simulations and laboratory laser-plasma experiments can (or will be able to, in
the near future) model realistic gamma-ray burst (GRB) shocks. For this, we
compare the radiative cooling time, t_cool, of relativistic electrons in the
shock magnetic fields to the microscopic dynamical time of collisionless
relativistic shocks -- the inverse plasma frequency of protons, omega_pp^{-1}.
We obtain that for t_cool*omega_pp^{-1}\lesssim ~few hundred, the electrons
cool efficiently at or near the shock jump and are capable of emitiing away a
large fraction of the shock energy. Such shocks are well-resolved in existing
PIC simulations; therefore, the microscopic structure can be studied in detail.
Since most of the emission in such shocks would be coming from the vicinity of
the shock, the spectral power of the emitted radiation can be directly obtained
from finite-length simulations and compared with observational data. Such
radiative shocks correspond to the internal baryon-dominated GRB shocks for the
conventional range of ejecta parameters. Fermi acceleration of electrons in
such shocks is limited by electron cooling, hence the emitted spectrum should
be lacking a non-thermal tail, whereas its peak likely falls in the multi-MeV
range. Incidentally, the conditions in internal shocks are almost identical to
those in laser-produced plasmas; thus, such GRB-like plasmas can be created and
studied in laboratory experiments using the presently available Petawatt-scale
laser facilities. An analysis of the external shocks shows that only the highly
relativistic shocks, corresponding to the extremely early afterglow phase, can
have efficient electron cooling in the shock transition. We emphasize the
importance of radiative PIC simulations for further studies.Comment: 15 pages, submitted to Ap
Recovering a spinning inspiralling compact binary waveform immersed in LIGO-like noise with spinning templates
We investigate the recovery chances of highly spinning waveforms immersed in
LIGO S5-like noise by performing a matched filtering with 10^6 randomly chosen
spinning waveforms generated with the LAL package. While the masses of the
compact binary are reasonably well recovered (slightly overestimated), the same
does not hold true for the spins. We show the best fit matches both in the
time-domain and the frequency-domain. These encompass some of the spinning
characteristics of the signal, but far less than what would be required to
identify the astrophysical parameters of the system. An improvement of the
matching method is necessary, though may be difficult due to the noisy signal.Comment: 5 pages, 1 figure + 4 figure panels; Proceedings of the Eight Edoardo
Amaldi Conference on Gravitational Waves (Amaldi8), New York, 2009; to be
published in J. Phys.: Conf. Series (JPCS
TeV Neutrinos from Successful and Choked Gamma-Ray Bursts
Core collapse of massive stars resulting in a relativistic fireball jet which
breaks through the stellar envelope is a widely discussed scenario for
gamma-ray burst production. For very extended or slow rotating stars, the
fireball may be unable to break through the envelope. Both penetrating and
choked jets will produce, by photo-meson interactions of accelerated protons, a
burst of neutrinos with energies in excess of 5 TeV while propagating in the
envelope. The predicted flux, from both penetrating and chocked fireballs,
should be easily detectable by planned cubic kilometer neutrino telescopes.Comment: Phys.Rev.Letters, in press, final version accepted 8/31/01 (orig.
3/17/01
MAP kináz jelátvitel funkcionális vizsgálat mitokondriumban = Functional studies on mitochondrial MAP kinase signalling
Munkánk során a növényekre specifikus, kevésbé vizsgált, D típusú MAPKok családjának egyik tagját az AtMPK9-t tanulmányoztuk. Élesztő kettős-hibrid rendszerrel a kalmodulint, mint lehetséges AtMPK9 fehérje partnert azonosítottuk, majd a kölcsönhatást in vitro transzlációval előállított fehérjékkel többféle megközelítéssel igazoltuk. Az AtMPK9 poszttranszlációs módosításokon keresztül történő szabályozása korábban ismeretlen volt. A pályázat keretében tömegspektrometriás vizsgálatokkal és in vitro mutagenezissel előállított AtMPK9 variánsokkal bizonyítottuk, hogy az aktiválásért felelős T hurok régióban elhelyezkedő TDY aminosav triplet treoninjának és tirozinjának foszforilálása nélkül a kináz nem rendelkezik aktivitással. A tömegspektrometriás adatok alapján az is nyilvánvaló vált, hogy az AtMPK9 kináz doménjét követő C-terminális doménben további négy aminosav foszforilálódik. Vizsgálataink szerint az összes általunk azonosított foszforiláció autofoszforiláció eredménye. Feltételezésünk szerint a kináz autofoszforilációs aktivitásának szabályozásában a kölcsönható partnerként azonosított kalmodulin kaphat szerepet. Az AtMPK9 in planta funkcióját protoplaszt tranziens expresszióval és null-mutáns növényekkel tanulmányoztuk. Vizsgálataink alapján a fehérje kináz abiotikus stresszel aktiválható, azonban ennek ellenére a null-mutáns növények fenotípusa még stressz körülmények között sem tér el a vadtípusétól, így az AtMPK9 valószínűsíthetően funkcionálisan redudáns kináz. | The project aimed at studying AtMPK9, a member of plant specific, D type mitogen activated protein kinase (MAPK). We identified calmodulin as its putative protein interacting partner by yeast two-hybrid assay. In order to evaluate this result, AtMPK9 and calmodulin were produced by in vitro translation and the interaction was confirmed by pull-down assays and surface plasmone resonance analysis. The kinase activity regulation of AtMPK9 was unknown previously. We demonstrated by mass spectrometry and in vitro mutagenesis studies that phosphorylation of threonine and tyrosine of TDY amino acid triad of T loop is inevitable for kinase activity. Further mass spectrometry analysis revealed another four phosphorylated amino acids in the C-terminal domain of AtMPK9. According to our in vitro translation based data, all the identified phosphorylations are caused by autophosphorylation. We hypothesize that the interacting partner calmodulin regulates the autophosphorylation activity of kinase. The in planta function of the protein kinase was studied by protoplast transient overexpression and application of AtMPK9 knock-out plants. Although the kinase activity of AtMPK9 was inducible by abiotic stress, the knock-out plants did not show any difference in phenotype, not even in stress conditions. These data imply that AtMPK9 is a functionally redundant protein kinase
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