High energy astrophysics studies the most extreme phenomena in the Universe. It therefore naturally involves black holes, neutron stars, supernova explosions and relativistic jets or outflows. Such objects often release large amounts of energy into a small volume within a short time and involve a wide variety of physical environments and mechanisms. They probe some of the most extreme conditions in nature, such as strong gravity, extreme densities and temperatures, huge magnetic fields and relativistic bulk velocities. A better understanding of such extreme environments holds the key to interpreting the most extreme astrophysical phenomena that occur in active galactic nuclei, gamma-ray bursts, supernovae, fast radio bursts or magnetars. The field of high-energy astrophysics has experienced great progress in recent years, both in the quality and quantity of available observational data (multiwavelength, high cadence and large field of view observations in addition to new multi-messenger observations – gravitational waves, high energy neutrinos and cosmic rays), as well as in the level of detail and sophistication of the theoretical models, in particular great progress in numerical simulations, which have all led to many novel discoveries. This opens new room for much more theoretical work, both analytic and numerical. Some of the main high energy astrophysics topics studied in our group include: Gamma-ray bursts, magnetars, fast radio bursts, pulsars, pulsar wind nebulae, gravitational lensing, cosmic rays, Lorentz invariance violation, high energy neutrinos, binary neutron stars and formation of r-process elements in the Universe.

Gamma Ray Bursts


R-process Nucleosynthesis

Gravitational Wave Sources

Fast Radio Bursts

Probing Cosmology and Fundamental Physics

GRB spectrum from gradual dissipation in a magnetized outflow

Gamma-ray bursts (GRBs) are the most (electromagnetically) luminous transient phenomenon in the Universe, outshining the entire gamma-ray sky during their brief prompt emission phase.  The latter typically lasts for ~0.03-1 s (in short-hard GRBs, produced by mergers of two neutron stars or a neutron star and a black hole) or ~3-300 s (in long-soft GRBs, produced during the explosion of massive, rapidly rotating stars, accompanied by a powerful supernova explosion). This emission is powered by a relativistic jet but the exact radiation mechanism is still a mystery. Most popular explanations include synchrotron emission from relativistic electrons with a power-law energy distribution, or Compton scattering of thermal photons trapped in the jet by warm electrons. Both of these emission mechanisms often feature in a general class of photospheric emission models that include a prominent quasi-thermal spectral component. In this work, Dr. Ramandeep Gill, Prof. Jonathan Granot and Dr. Paz Beniamini (all from ARCO) studied how the non-thermal smoothly broken power law spectrum of the prompt GRB emission is produced in magnetized jets. Such jets are accelerated by the gradual and continuous dissipation of the magnetic field energy, where particles are accelerated or heated via magnetic reconnection and/or magnetohydrodynamic (MHD) instabilities. This work shows in great detail how the final spectrum is generated by a magnetized jet as it expands (see the figure). It clearly demonstrates that if electrons are accelerated into a relativistic power-law energy distribution, then synchrotron emission is the dominant radiation mechanism (left panel). Alternatively, if electrons are heated into a warm plasma (all particles having the same average energy), then the prompt GRB spectrum forms via Compton scattering of thermal photons (right panel). The shown spectra are obtained from a specially designed numerical code that accurately accounts for all relevant high-energy processes, including production and annihilation of electron-positron pairs, in a relativistically expanding jet. GRB spectrum from gradual dissipation in a magnetized outflow GRB spectrum from gradual dissipation in a magnetized outflow 2 The way the low- and high-energy (below and above the spectral peak) parts of the spectrum are generated has important implications for energy-dependent linear polarization. In the left panel, synchrotron emission can yield strong linear polarization, depending on the magnetic field geometry. In the right panel, however, multiple Compton scatterings wash out any polarization and only produce a negligible global polarization in a uniform (with no local angular structure) jet. Using these results, more sensitive spectro-polarimetric observations from detectors onboard upcoming space missions will help to pin down the exact prompt GRB radiation mechanism.


GRB Polarization: A Unique Probe of GRB Physics

Gamma-ray bursts (GRBs) are  the most powerful explosions in the Universe. They are powered by ultra-relativistic jets (highly collimated outflows moving at ~99.995% of the speed of light). The huge isotropic-equivalent gamma-ray luminosities of Lɣ,iso~1051 - 1054 erg/s of their brightest prompt emission phase places GRBs as the most (electromagnetically) luminous transient events in nature. This makes them detectable out to the far reaches of the Universe, from down to barely a billion years after the Big Bang. The exact radiation mechanism that produces this prompt emission is still a mystery. The two most popular candidates are synchrotron emission from relativistic electrons with a power-law energy distribution and Compton scattering of thermal radiation by warm electrons. Both mechanisms can explain the majority of the observed prompt GRB spectra equally well, making it hard to distinguish between them. However, they can lead to very different linear polarization, depending on the magnetic field geometry (for synchrotron emission) and the jet’s angular structure (for both). Therefore, high-sensitivity linear polarization measurements can help distinguish between them and reveal the dominant radiation mechanism. Moreover, for synchrotron emission they can also teach us about the magnetic field structure in the emission region. GRB Polarization: In this work, Dr. Ramandeep Gill (ARCO), Dr. Merlin Kole (University of Geneva) and Prof. Jonathan Granot (ARCO) provide a comprehensive review of the predictions for prompt GRB linear polarization from theoretical models and the current status of polarization measurements. The work gives a concise overview of the fundamental questions in GRB physics, namely what are the jet composition and dynamics, how and where is the energy dissipated, and what are the different candidate radiation mechanisms capable of producing the non-thermal prompt GRB spectrum. It presents relevant formulae and polarization predictions (both time-integrated and time-resolved) for different radiation mechanisms, magnetic field configurations (relevant for synchrotron emission), jet angular structures and dynamics. On the observational front, this work presents the basics of gamma-ray polarimetry and chronicles the GRB polarization measurements made by different detectors over the years. The figure shows example lightcurve (black) and time-resolved polarization (Π) curves for synchrotron emission from different magnetic field configurations in one realization of a uniform (lacking angular structure) jet seen at an angle from the symmetry axis of the jet (for a single pulse in the GRB prompt emission lightcurve). The detailed polarization predictions presented in this work will enable observers to compare high-sensitivity measurements from upcoming gamma-ray polarimeters with theoretical models and constrain fundamental properties of the GRB relativistic jet and prompt emission mechanism.


Gamma ray burst afterglows from neutron star merger jets

One of the key results of Einstein’s general theory of relativity was the prediction of gravitational waves (GWs) – `ripples’ in space-time that travel at the speed of light and carry gravitational energy. Such waves are abundantly created when compact massive objects are accelerated. Mergers of very dense objects, such as black holes and neutron stars are an especially prolific source of GWs. Almost 100 years after their prediction by Einstein, they were directly measured for the first time in 2015, coming from a pair of merging black holes, by the LIGO interferometer. This groundbreaking discovery was awarded the Nobel prize in physics in 2017. It was on the 17th of August 2017 that GW detectors observed another type of cataclysmic event: the merger of two neutron stars. Such mergers are particularly interesting, as they are linked to some of the brightest electromagnetic transients in the Universe - short gamma-ray bursts (GRBs). In short GRBs jets traveling at very close to the speed of light create high-intensity radiation (mainly in gamma rays at first and later across the electromagnetic spectrum, in the stage known as the GRB afterglow). The beaming of light emitted by objects moving at near-light speeds, combined with the jetted geometry of the emitting material, implies that we typically detect such bursts `face on’, where our line of sight lies within the jet’s core. GRBs are so bright that they are typically seen from distances of billions of light-years from Earth. Although GRBs have been observed for over 50 years, some of the most basic questions about their nature remain unsolved, including the structure and composition of their jets and the physical process powering different phases of their emission. [caption id="attachment_1166" align="alignright" width="647"] Figure 1 Flux per unit area of the sky observed from an afterglow of a structured jet viewed off-axis at different times. The observer is initially dominated by the low energy material that is close to their line of sight (top left). Over time, as the jet slows down, and relativistic beaming less prominent, the emission becomes dominated by the energetic core (denoted by a white cross).[/caption] The event observed in 2017, dubbed GW170817, based on its detection date, lead astronomers to point a variety of electromagnetic telescopes to the same location on the sky. Indeed, a short GRB was detected, confirming the link between these two phenomena. However, this GRB was different than any of the previously seen bursts. In particular, the initial gamma-ray emission was much less luminous and the afterglow `light-curve’ (the temporal evolution of the recorded electromagnetic signal) evolved in a distinct way, initially rising gradually for over 150 days and then decaying rapidly. The reason for this difference is that the detection trigger by the GWs enabled astronomers for the first time, to view a GRB jet, quite literally, from a different point of view: from a line of sight far away from the jet axis (off-axis; see figure 1) and coming from a distance much closer to Earth. This enabled us, in turn, to learn in unprecedented detail about the lateral structure of the underlying GRB jet and to better understand how such jets propagate through their environments and develop this structure. The future of binary mergers jointly detected in GWs and as GRBs holds much promise. An investigation, that Dr. Beniamini, Prof. Granot and Dr. Ramandeep Gill (all members of ARCO) carried in “Afterglow light curves from misaligned structured jets” derives in detail the lightcurves from the accompanying GRB afterglows from jets with different lateral structures, observed from arbitrary viewpoints. Using analytical tools, the study reveals qualitatively different types of light curves that can be viewed in future off-axis GRBs, with either single or double peaks (Figure 2), depending on the jet structure and the viewing angle. It shows that focusing on the shape of the lightcurves from such jets rather than absolute times or fluxes, enables to deduce intrinsic properties of the jet and its angle to the observer, independently of many of the degenerate and therefore unconstrained physical parameters that affect the afterglow properties of `standard’ GRBs. Such robust parameter inferences will provide a crucial stepping stool for numerical investigations, attempting to deduce the underlying physical properties of individually observed GRBs. At the same time, our study can help guide future observational transient survey campaigns, attempting to search for `orphan afterglows’ – GRBs in which the early burst of gamma rays is missed (as the jet points away from Earth) but are detected later in shorter wavelengths (e.g. X-ray, optical or radio) during the afterglow phase when the jet decelerates and its radiation beam widens and reaches our line of sight.  

Figure 2 Different types of light-curves that can be viewed by observers misaligned with the jet core. Focusing on the temporal slopes, as well as the ratio of the characteristic times and frequencies provides robust information on the jet properties and observer’s viewing angle, independently of the many other unconstrained physical parameters.


High-energy emission from a magnetar giant flare in the Sculptor galaxy

Magnetars are young neutron stars with the strongest magnetic fields in the Universe (surface fields of 1013–1015 G). They probe some of the most extreme physical conditions in nature, such as strong field gravity, huge (nuclear) densities and extreme energy densities. The evolution and decay of their ultra-strong magnetic field powers a variety of X-ray bursting activity, ranging from relatively frequent short bursts to very rare and much more energetic giant flares (GFs), which can dissipate a good part of their magnetospheric energy and eject plasma at relativistic speeds. Magnetar GFs consist of a short-duration (0.1–0.5 s) bright initial spike followed by a longer (300–400 s) and much dimmer pulsating tail, strongly modulated at the magnetar’s known spin period (of typically a few to several seconds). So far three GFs were clearly recorded – two Galactic and one from the Large Magellanic Cloud (LMC) – a small satellite galaxy of our Milky Way. The most recent and energetic of these events, detected on Dec. 27, 2004, from the Galactic magnetar SGR 1806–20, produced measureable changes in Earth’s upper atmosphere despite erupting from a magnetar located about 40,000 light-years away.  The two Galactic GFs showed longer lasting (days to many months) radio emission, which provided good evidence for the ejection of plasma at mildly relativistic speeds (about 50%–70% of the speed of light, close to the escape velocity from the neutron star) with a kinetic energy comparable to the energy radiated in the GF’s initial spike. This work reports the first high-energy (with photon energies of the order of giga-electronvolt – GeV) detection of emission from a magnetar GF. This event was from the nearby (3.5 megaparsecsHigh-energy emission from a magnetar giant flare in the Sculptor galaxy – Mpc) Sculptor galaxy, which is much further away than the Galactic GFs (10-15 kiloparsecs – kpc) or the GF from the LMC (50 kpc), and therefore only its initial spike was bright enough to be detected while its pulsating tails was too dim. The Large Area Telescope (LAT) on board the Fermi Gamma-ray Space Telescope detected GeV γ rays from 19 s until 284 s after the initial detection of a signal in the megaelectronvolt (MeV) band (which lasted 0.14 s, corresponding to the GF’s initial spike). Our analysis shows that these γ rays are spatially associated with the Sculptor galaxy and are unlikely to originate from a cosmological γ-ray burst. Thus, we infer that the γ rays originated with the magnetar GF in Sculptor. A magnetar produces a steady magnetized wind powered by the very gradual slowing down of its rotation. As the magnetar moves through space, this wind plows into, slows, and diverts interstellar gas. The gas piles up, becomes heated and compressed into a thin curved shell, and forms a type of oblique shock wave called a bow shock. In the model proposed by the LAT team, with leading roles by Prof. Jonathan Granot and Dr. Ramandeep Gill of ARCO at the Open University of Israel, the GF’s MeV initial spike travels outwardHigh-energy emission from a magnetar giant flare in the Sculptor galaxy at the speed of light, followed by the cloud of ejected matter consisting of protons, electrons and positrons, which is moving nearly as fast (at about 99.995% the speed of light). After several days, they both reach the bow shock. The MeV γ rays pass through. Then, several seconds later, the cloud of particles – now expanded into a vast thin shell – collides with gas at the bow shock shell. This collision between the two shells drives shock into both of them that accelerates particles, which produce the highest-energy GeV γ rays several seconds to minutes after the main burst. This new and exciting event shows both similarities and differences relative to the magnetar GFs in our Milky way galaxy. On the one hand, in all of these events the energy radiated in γ rays and the kinetic energy of the ejected matter are comparable. On the other hand, in this new event the ejected matter is much faster, at about 99.995% of the speed of light, compared to about 50%–70% of the speed of light in the two GFs in the Milky way. This much faster velocity implies, in turn, a much smaller amount of protons in the ejected matter, which demonstrates a much wider diversity between different magnetar GFs than was known so far. This work was published in Nature Astronomy See also a short illustrative video.


Constraining the magnetic field structure in collisionless relativistic shocks with a radio afterglow polarization upper limit in GW 170817

Shocks (a.k.a blast waves) are a ubiquitous phenomenon in the Universe. In many astrophysical objects, emission all the way from radio through X-rays to very high energy gamma-rays is powered by collisionless shocks (which are mediated by collective electromagnetic interactions rather than by particle collisions). These include relativistic (traveling at very close to the speed of light) blast waves powered by stellar-mass black holes in gamma-ray bursts (GRBs) and supermassive black holes in active galactic nuclei, or non-relativistic blast waves in supernovae. It is well established that the broad-band (radio to gamma-rays) afterglow emission in GRBs is produced by relativistic electrons that are accelerated at collisionless shock fronts. In particular, these electrons emit synchrotron radiation as they gyrate in the shock-generated magnetic fields behind the shock front. Several theoretical works and numerical (particle in cell - PIC) simulations are devoted to understanding the structure of this magnetic field, which is posited to be tangled and anisotropic -  constrained entirely to the plane of the shock - perpendicular to the shocked fluid’s local velocity. Since synchrotron emission is generally partially linearly polarized, this has important implications for the measured degree of polarization (Π). GRB afterglows show polarization of up to a few percent, which already suggests that the shock-generated field is closer to isotropic (a fully isotropic field gives Π = 0) than anisotropic. Better understanding of the magnetic field structure in GRBs, the majority of which have been observed at distances of billions of light-years, is limited by our incomplete knowledge of the angular structure of the relativistic jet and our viewing angle relative to its symmetry axis, which also affects the degree of polarization Π, thereby creating a degeneracy. Constraining the magnetic field structure A golden opportunity was provided by the afterglow of GW170817 / GRB 170817A that originated in the aftermath of a merger between two neutron stars only 130 million lightyears away from us.  Dr. Ramandeep Gill and Prof. Jonathan Granot (both from ARCO) used the afterglow from this source to study the properties of the relativistic jet, including its angular structure, in several joint works. In the present work, they used their knowledge of the jet’s angular structure (either a gaussian jet (GJ) or power-law jet (PLJ) and our viewing angle (about 25 to 30 degrees or 5 to 6 times the jet’s core angle), to isolate the effects of the shock-generated magnetic field structure on the afterglow linear polarization. The figure shows several polarization curves marked by ξf, the parameter characterizing the anisotropy of the magnetic field (becoming more anisotropic away from unity) just behind the shock front. The two arrows show the upper limit on the afterglow polarization obtained from radio observations. This work improved the constraints on the magnetic field anisotropy (0.57 < ξf < 0.89) and clearly showed that the magnetic field just behind the shock front is only mildly anisotropic, contrary to several earlier works. The implications of this study are of fundamental importance for collisionless shock physics. In particular, it suggests that the magnetic field may be produced not only by small-scale plasma instabilities but is instead also strongly affected by macroscopic turbulence in the region behind the shock front, which generally yields more isotropic magnetic fields.


The rate of r-process production in the Universe

[caption id="attachment_759" align="alignright" width="425"]The rate of r-process production in the Universe Figure 1 Colored regions denote different constraints on the rate and r-process mass produced per event (from the review by Hotokezka, Beniamini & Piran, 2018). The constraint from UFDs is shown by purple contours and that from GW 170817 by a pink square.[/caption] Since the dawn of humankind, people have been fascinated by the origin of gold. It appears prominently in mythologies all over the world: from the tears of the sun god Inti in the Incan culture to the cursed golden touch of king Midas in Greek mythology. This obsession resulted in a pursuit to try and artificially create gold that despite never being successful, was common enough to get its own term – alchemy. Modern physics provided us with the atomic theory, which teaches us that the distinction between different elements lies in the number of protons in their nucleus. Different types of atoms may indeed be transformed from one type to the next (as imagined by ancient followers of alchemy, although in a completely different manner), through nuclear processes such as fusion and fission. In the astrophysical context, the formation of different elements, are dominated by different processes. For example, while most of the H and He in the Universe are relics of the big bang, slightly heavier elements are formed mainly through cosmic spallation or through nuclear fusion in the hearts of stars. Elements heavier than iron require an external source of energy to form and can therefore only occur in environments with very large densities and temperatures. About half of these elements (including gold) are dominated by the so-called rapid (or for short r) process, which requires extreme physical conditions in order to take place. Since the fifties it has been thought that this process may take place in supernovae – the explosions that mark the end of massive stars’ lives. However, over the years, it gradually became clear that the required conditions for r-process are not readily achieved in standard supernovae. Furthermore, in the last several years, there has been growing evidence in an altogether rarer and much more exotic (but also potentially much more prolific) channel – mergers of binary neutron star systems (see figure 1). The r-process element abundances in stars in our own Galaxy is well measured. Nonetheless it does not immediately reveal the rate of the astrophysical process behind their formation. Broadly speaking, the process may either be very common but with each event creating a meager amount of r-process material or else the events may be rare but individually prolific. In a 2020 study, Dr. Beniamini and collaborator have shown that data from Milky Way stars can be used to constrain the rate of r-process events, as well as constrain the speed of their mixing in the interstellar medium. This is doneThe rate of r-process production in the Universe through several techniques. First, they consider the scatter of r-process abundance (of stable r-process elements) between stars with similar iron abundances (which were therefore created in most cases, around a similar time). A greater rate of r-process events and / or speed of their mixing, leads to a smaller scatter, and vice versa. Secondly, if the speed of mixing were slow and / or the rate of enrichment high, then a fraction of the observed stars should have been formed in areas that are still greatly enriched from the latest enrichment event. This would lead to stars with huge levels of r-process enrichment which are not observed. This condition can therefore rule out combinations of sufficiently slow mixing and rapid enrichment rate. A third constraint comes from studying isotope abundance ratios as compared to their formation ratios. A greater ratio indicates a lower r-process enrichment rate and / or mixing speed. Combining all these considerations together allows to put strong constraints on the rate of r-process enrichment and the speed of mixing of those elements in the interstellar medium, which are once more consistent with neutron star mergers. Studies such as this bring us closer to deciphering the origin of gold and other r-process in the Universe and critically test our astrophysical theories.  


Exploring the epoch of hydrogen reionization using FRBs

Immediately after the big bang, the Universe was filled with extremely dense and hot ionized gas. As the universe expanded and cooled, electrons, protons and neutrons became less energetic and for the first time were able to combine to form neutral atoms.  This era which took place only 380,000 years after the big bang and is known as the era of recombination, also marked the first time in the Universe’s history at which light was able to travel freely through space. However, at this point in the Universe’s history, there was little light to speak of. Only a few hundred million years later, as dense clouds of gas collapsed into the first stars, light was finally being created in abundance. The higher frequency UV light created by these first stars split hydrogen atoms back into electrons and protons, in a process known as ionization. As the electrons and protons were already separated from each other earlier in the evolution of the Universe (before the recombination era), this stage of the Universe is known in cosmology as “the era of reionization”. Reionization presents one of the few means by which we can (indirectly) study the conditions in the Universe very early on and the properties of the earliest stars that lived in it. However, the details of when exactly reionization occurred and how it proceeded over time and space thereafter, are still poorly constrained by data. [caption id="attachment_1175" align="aligncenter" width="800"] Figure 1 Simulation of cosmic reionization showing temperature variations as a function of cosmic redshift (larger values correspond to earlier cosmic times) for a given ‘slab’ of the Universe. Image courtesy of Raghunath Ghara and Saleem Zaroubi.[/caption] Fast Radio Bursts (FRBs) are brief (typically lasting a few milliseconds), very bright radio pulses arriving at Earth from billions of light-years away. The FRB field is relatively new (with the first detection taking place in 2007) and many properties of FRBs are still a topic of active investigation. Nonetheless, their connection to highly magnetized neutron stars – ‘magnetars’ was vividly established in April of 2020, when a known magnetar source in our own Galaxy, was observed to produce such a burst. Magnetars are known to be a common by-product of the collapse of massive stars (see work by Dr. Beniamini and collaborators), which in turn are thought to be a major contributor to the Universe’s reionization as mentioned above. Indeed, the conditions taking place in the early Universe are likely to make the extremely strong magnetic fields needed to power magnetars even easier to attain. Furthermore, some gamma-ray bursts, are known to take place during this era, and the creation of their jets almost definitely requires enormous magnetic fields. The existence of magnetars in the Early Universe, combined with the great abundance of FRBs (which are created at a rate of about 10,000 per day over the entire sky, several thousands of times more common than, for example, gamma ray bursts), and the relative ease of detecting them from large distances, make FRBs excellent probes of cosmology.  On top of this, for each FRB, astronomers get a measurement of the “dispersion measure”, a quantity which reflects the number of ionized electrons in a column between the FRB source and us, and which for remote FRBs, can illuminate the properties of the intervening intergalactic medium, which is not readily observed by other means. [caption id="attachment_1176" align="alignleft" width="213"] Figure 2 Top: Different possible histories for the fractions of ionized electrons as a function of cosmic 'redshift' (higher redshift corresponding to an earlier stage of the Universe). Bottom: The dispersion measures associated with these ionized electron fraction histories.[/caption]

In a work from 2021, Dr. Beniamini and collaborators have shown that the distribution of “dispersion measures” of FRBs from the early Universe holds great potential towards exploring the era of reionization. One aspect they explore, makes use of the fact that due to the reionization of the Universe taking place at a finite time, there is a maximum limit (which depends on the reionization history) to the column of ionized electrons that can lie between us and an FRB source (if the FRB is very distant, then the FRB signal was created before the Universe was fully reionized and the burst travelled a portion of its journey towards us through mostly neutral material). The research outlines three different methods, using either FRBs with known or unknown host galaxies which can be used to measure the Universe’s reionization history. FRBs have the potential to become the most accurate source of information about the era of reionization in a matter of several years.


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