اشترك بالحزمة الذهبية واحصل على وصول غير محدود شمرا أكاديميا
تسجيل مستخدم جديدAstrophysical Evidence of Wakefield Acceleration in Galactic and Extragalactic Jets via Gamma Rays and UHECRs
101
0
0.0
(
0
)
اسأل ChatGPT حول البحث
ﻻ يوجد ملخص باللغة العربية
We present six case studies from a broad mass range ($1 - 10^9$ $M_odot$) of astrophysical objects, each of which exhibit signs of jets and emit intense high energy gamma rays ($>10$ GeV). Many of these objects also emit spatially identifiable ultra high energy cosmic rays (UHECRs). In all cases it is found that wakefield acceleration (WFA) explains both the global properties and details. For blazars, we also explain the temporal structure of these signals, which includes neutrinos, and the correlations in their bursts and anti-correlation in flux and index. Blazars ($sim 10^9$ $M_odot$), radio galaxies ($sim 10^8, M_{odot}$), Seyfert galaxies ($sim 10^6 ,M_{odot}$), starburst galaxies ($sim 10^{3}, M_{odot}$), down to microquasars ($1 sim 10$ $M_odot$) interestingly exhibit the same physics since the nature of the accretion and acceleration is independent of the mass, aside from maximum values. It is possible to accelerate electrons to energies much greater than $10$ GeV, and protons beyond $10^{20}$ eV with WFA. We compare observational values with theoretical ones to illustrate they are in good agreement. This mechanism is also accompanied by related emissions, such as high-energy pin-pointed neutrinos, time varying radio, optical, and X-ray emissions, opening an opportunity to characterize these astrophysical objects via multi-messenger approaches.
قيم البحث
اقرأ أيضاً
In this chapter, we review some features of particle acceleration in astrophysical jets. We begin by describing four observational results relating to the topic, with particular emphasis on jets in active galactic nuclei and parallels between differe
nt sources. We then discuss the ways in which particles can be accelerated to high energies in magnetised plasmas, focusing mainly on shock acceleration, second-order Fermi and magnetic reconnection; in the process, we attempt to shed some light on the basic conditions that must be met by any mechanism for the various observational constraints to be satisfied. We describe the limiting factors for the maximum particle energy and briefly discuss multimessenger signals from neutrinos and ultrahigh energy cosmic rays, before describing the journey of jet plasma from jet launch to cocoon with reference to the different acceleration mechanisms. We conclude with some general comments on the future outlook.
From the analysis of the flux of high energy particles, $E>3cdot 10^{18}eV$, it is shown that the distribution of the power density of extragalactic rays over energy is of the power law, ${bar q}(E)propto E^{-2.7}$, with the same index of $2.7$ that
has the distribution of Galactic cosmic rays before so called knee, $E<3cdot 10^{15}eV$. However, the average power of extragalactic sources, which is of ${cal E}simeq 10^{43}erg ,s^{-1}$, at least two orders exceeds the power emitted by the Galaxy in cosmic rays, assuming that the density of galaxies is estimated as $N_gsimeq 1 Mpc^{-3}$. Considering that such power can be provided by relativistic jets from active galactic nuclei with the power ${cal E}simeq 10^{45} - 10^{46} erg , s^{-1}$, we estimate the density of extragalactic sources of cosmic rays as $N_gsimeq 10^{-2}-10^{-3}, Mpc^{-3}$. Assuming the same nature of Galactic and extragalactic rays, we conclude that the Galactic rays were produced by a relativistic jet emitted from the Galactic center during the period of its activity in the past. The remnants of a bipolar jet are now observed in the form of bubbles of relativistic gas above and below the Galactic plane. The break, observed in the spectrum of Galactic rays (knee), is explained by fast escape of energetic particle, $E>3cdot 10^{15}eV$, from the Galaxy because of the dependence of the coefficient of diffusion of cosmic rays on energy, $Dpropto E^{0.7}$. The obtained index of the density distribution of particles over energy, $N(E)propto E^{-2.7-0.7/2}=E^{-3.05}$, for $E>3cdot 10^{15}eV$ agrees well with the observed one, $N(E)propto E^{-3.1}$. Estimated time of termination of the jet in the Galaxy is $4.2cdot 10^{4}$ years ago.
The use of Z-pinch facilities makes it possible to carry out well-controlled and diagnosable laboratory experiments to study laboratory jets with scaling parameters close to those of the jets from young stars. This makes it possible to observe proces
ses that are inaccessible to astronomical observations. Such experiments are carried out at the PF-3 facility (plasma focus, Kurchatov Institute), in which the emitted plasma emission propagates along the drift chamber through the environment at a distance of one meter. The paper presents the results of experiments with helium, in which a successive release of two ejections was observed. An analysis of these results suggests that after the passage of the first supersonic ejection, a region with a low concentration is formed behind it, the so-called vacuum trace, due to which the subsequent ejection practically does not experience environmental resistance and propagates being collimated. The numerical modeling of the propagation of two ejections presented in the paper confirms this point of view. Using scaling laws and appropriate numerical simulations of astrophysical ejections, it is shown that this effect can also be significant for the jets of young stars.
Magnetized jets in GRBs and AGNs are thought to be efficient accelerators of particles, however, the process responsible for the acceleration is still a matter of active debate. In this work, we study the kink-instability in non-rotating force-free j
ets using first-principle particle-in-cell simulations. We obtain similar overall evolution of the instability as found in MHD simulations. The instability first generates large scale current sheets, which at later times break up into small-scale turbulence. Reconnection in these sheets proceeds in the strong guide field regime, which results in a formation of steep power laws in the particle spectra. Later evolution shows heating of the plasma, which is driven by small-amplitude turbulence induced by the kink instability. These two processes energize particles due to a combination of ideal and non-ideal electric fields.
We briefly review sources of cosmic rays, their composition and spectra as well as their propagation in the galactic and extragalactic magnetic fields, both regular and fluctuating. A special attention is paid to the recent results of the X-ray and g
amma-ray observations that shed light on the origin of the galactic cosmic rays and the challenging results of Pierre Auger Observatory on the ultra high energy cosmic rays. The perspectives of both high energy astrophysics and cosmic-ray astronomy to identify the sources of ultra high energy cosmic rays, the mechanisms of particle acceleration, to measure the intergalactic radiation fields and to reveal the structure of magnetic fields of very different scales are outlined.
سجل دخول لتتمكن من نشر تعليقات
التعليقات
جاري جلب التعليقات
سجل دخول لتتمكن من متابعة معايير البحث التي قمت باختيارها
