Cosmic Ray Anisotropy Workshop CRA2019

7 Oct 2019, 09:00 → 11 Oct 2019, 15:20 Europe/Rome

Ex-ISEF/Building-Main Lecture Hall (GSSI)

Carmelo Evoli (GSSI), Giovanni Morlino (Gran Sasso Science Institute), Pasquale Blasi (GSSI), Pierre Cristofari (GSSI)

 

 

Science Goals

The Workshop will bring together scientists from around the world to discuss the origin, composition, propagation, and modulation of cosmic-rays, with a focus upon the anisotropy on small and large scales, and the effects of interstellar and heliospheric processes on the signal observed at the Earth.

Topics of the workshop

    *   Cosmic ray anisotropy and local sources of acceleration

    *   Cosmic ray propagation through interstellar magnetized plasma

    *   Cosmic ray interaction with the heliosphere

    *   Properties of galactic and interstellar medium and magnetic fields

    *   Properties of the heliosphere and astrospheres

    *   Recent results on cosmic ray anisotropy observations

    *   Analysis techniques in cosmic ray anisotropy studies

    *   Gamma rays as probes of cosmic ray acceleration and transport

    *   Anomalies in cosmic ray composition

Important deadlines

• 1 April 2019: open call for abstract.
• 30 May 2019: call for abstract close. (postponed to 10 June 2019)
• 1 June 2019: early registration open (fee 150€). (postponed to 10 June 2019)
• 7 June 2019: confirmation of abstract acceptance.
• 12 August 2019: early registration close. After this date the registration fee will be 200 €.
• 7  September 2019: registration close.
• 7-11 October 2019: Conference

Pay the fee

To pay the conference fee, please go here: http://registration.gssi.it/index.php/cra2019

CRA2019_group_photo.JPG

CRA2019_poster.jpg

Monday, 7 October

09:00 → 09:40 Opening talks

09:40 → 10:20 Recent Advances in (Galactic) Cosmic Ray Observations

Speaker: Prof. Ivan De Mitri (Gran Sasso Science Institute (GSSI) and INFN)

CRA2019-IDM.pdf

10:20 → 11:00 Coffee break

11:00 → 11:40 Cosmic Ray Anisotropies with space-based detectors

In the last years, Cosmic Ray Physics has profited from the rise in space research and space-based experiments are currently providing direct measurements with unprecedented precision. In particular, the measurement of the anisotropy may provide complementary information to the features observed in the spectra of
several cosmic ray species.
In this talk, an overview of the latest results on the cosmic ray anisotropy studies performed by space-based detectors will be presented.

Speaker: Miguel Angelo Velasco (CIEMAT)

MAVelasco_CRA2019.pdf

11:40 → 12:20 Anisotropy of ultra-high energy cosmic rays

Important observational results have been recently reported on the angular distributions of cosmic rays at ultra-high energies, calling into question their perception a decade ago. The extragalactic origin of the particles has been determined observationally. While no discrete source of ultrahigh-energy cosmic rays has been identified so far, the noose is tightening around nearby extragalactic objects. These results together with their in-progress interpretations are summarized in this contribution, covering both large-scale and small-scale anisotropies from sub-EeV energies to the highest ones. Some prospects are finally discussed.

Speaker: Olivier Deligny (Institut de Physique Nucléaire d'Orsay)

2019-10-CRAW.pdf

12:20 → 13:00 Full-Sky Cosmic-Ray Anisotropy with HAWC and IceCube

We present the joint analysis of the arrival direction distribution of Galactic cosmic rays by the High-Altitude Water Cherenkov and IceCube Neutrino observatories at the same median primary particle energy of 10 TeV. The combined sky map and angular power spectrum largely eliminate biases that result from partial sky coverage. The trajectories and observed distribution of particles are distorted by magnetic structures of scales comparable to their gyro-radii such as the heliosphere and the local interstellar magnetic field. We infer the direction of the interstellar magnetic field from the boundary between large scale excess and deficit regions. Using the field direction, we then estimate the 'vertical' dipole component of the large scale anisotropy which is generally not observable by ground-based detectors.

Speaker: Juan Carlos Díaz Vélez (University of Wisconsin-Madison)

IC-HAWC-CRA19.pdf

13:00 → 14:30 Lunch break

14:30 → 15:00 Anisotropy results from Telescope Array

The latest results of anisotropy searches with the Telescope Array will be presented, including the current status of the hot spot, spectrum declination dependence, search for energy-ordered clusters, correlation with supergalactic plane.

Speaker: Petr Tiniakov (Universite Libre de Bruxelles)

2019-Aquila-CRA-Tinyakov.pdf

15:00 → 15:30 Constraining astrophysical models by using the energy spectrum and mass composition data measured at the Pierre Auger Observatory

The Pierre Auger Observatory, thanks to its hybrid detection technique, provides information about the energy, the mass composition and the arrival direction of ultra-high energy cosmic rays (UHECRs). Starting from a simple astrophysical scenario for origin and propagation of cosmic rays, it is possible to perform a combined fit to both the energy spectrum and the mass composition data.
We considered only events with energies above the region where the transition between Galactic and extragalactic cosmic rays is supposed to occur (E > few $10^{18}$ eV), hence data can be interpreted assuming a pure extragalactic origin. The adopted astrophysical model consists of identical sources uniformly distributed in a comoving volume, which accelerate nuclei through a rigidity-dependent mechanism. The fit results suggest that nuclei are injected with a hard spectrum up to a relatively low maximum energy. A quite heavy chemical composition at the acceleration sites is favoured.
The measured fluxes can be sensitive to poorly-known physical quantities relevant to the UHECRs propagation, e.g. the extra-galactic background light spectrum and the photo-disintegration cross sections of nuclei, and to the hadronic interaction models used to take into account the shower development in atmosphere. A discussion of the effects of such choices on the combined fit results will be presented.

Speaker: Eleonora Guido (INFN Sezione Torino)

cra_workshop_EGuido.pdf

15:30 → 16:00 Coffee break

16:00 → 16:30 Anisotropy Searches with DAMPE

The DArk Matter Particle Explorer (DAMPE) is a satellite-borne experiment successfully launched in December 2015. The main scientific goal of the mission is to perform high precision measurements of the High Energy Cosmic Ray (HECR) sky looking also for Dark Matter signals. After more than three years of data taking, DAMPE has collected over 5.6 billion events.
In recent years the anisotropy of CRs results have been presented by several collaborations with the use of ground-based and space-based experiments from energies above tens of GeV up to EeV. In this work we present the sensitivity of DAMPE experiment to the anisotropy signal. We discuss the method used for anisotropy searches and present the preliminary results using the DAMPE 2016 data for all particle types at energy deposit in the calorimeter from 100 to 500 GeV. This includes studies on the different angular scales.

Speaker: Mikhail Stolpovskiy (University of Geneva)

DAMPE_Stolpovskiy.pdf

16:30 → 17:00 Studies of a possible large-scale anisotropy of UHECRs with future orbital detectors

We study capabilities of future orbital detectors of ultra-high-energy cosmic rays (UHECRs) like KLYPVE (K-EUSO) and POEMMA to reveal a large-scale anisotropy of their arrival directions at energies beyond ~50 EeV assuming a nearby active galactic nucleus provides a noticeable fraction of the total flux. We find that such a detector with a uniform exposure of the whole celestial sphere will be able to reveal an anisotropy at high confidence level providing it registers ~300 or more UHECRs and the fraction of the flux coming from a nearby source is of the order of 10%. We also demonstrate that such an anisotropy does not manifest itself clearly at energies above ~8 EeV, contrary to the dipole anisotropy found recently by the Pierre Auger Observatory, so that it can escape from being found by the existing ground-based experiments.

Speaker: Mikhail Zotov

keuso.pdf

Tuesday, 8 October

09:00 → 09:40 Anisotropies in the flux of cosmic ray leptons

The cosmic electrons and positrons have been measured with unprecedented
statistics up to several hundreds GeV, thus permitting to explore the role that close single
sources can have in shaping the flux at different energies.
The Fermi-LAT Collaboration has provided a new
energy spectrum for the upper bounds on the e+ + e- dipole anisotropy. This observable
can bring information on the emission from local Galactic sources, notably measured with
high precision at radio frequencies. We develop a framework in which e+ and e- measured
at Earth from GeV up to tens of TeV energies have a composite origin. We discuss in particular the
constraints imposed by the most recent data
on the e+ + e- dipole anisotropy.

Speaker: Fiorenza Donato (University of Turin )

CRA_GSSI.pdf

09:40 → 10:20 On Cosmic Ray transport in the magnetized Interstellar Medium: a bias towards microphysics.

Under the effect of magnetic turbulence Cosmic Rays (CRs) adopt a random walk during their journey from their sources to the Earth. The talk addresses the interplay between the turbulence and Cosmic Rays. At first we will examine the effect of turbulence over Cosmic Ray transport through the derivation of diffusion coefficients. We will discuss the impact of the turbulence injected at large scales. Then we will discuss the effect of Cosmic rays over turbulence through the triggering of different plasma instabilities. These effects are likely important for the propagation of CRs with energies below a few hundred of GeV. But we will see that in sources self-generated turbulence is mandatory to explain CR acceleration. Finally we will discuss how to handle in the same framework CR transport and turbulence generation, this is now possible mainly because of some recent progresses in some numerical modeling combining kinetic and magnetohydrodynamics. In each these three steps we will discuss some connection to the study of CR anisotropy.

Speaker: Alexandre Marcowith (Universite Montpellier)

CRA-AM-CRTURB.pdf

10:20 → 11:00 Coffee break

11:00 → 11:40 Cosmic ray propagation in the Galaxy: the role of self-confinement

Understanding the transport of charged particles in the Galaxy is fundamental to solve the mystery of the origin of Galactic cosmic rays (CR) and to asses their role in several Galactic processes. Recent results from direct experiments, especially AMS-02 and PAMELA, are revealing a fine structure in the CR spectrum which is difficult to explain in the standard picture of Galactic propagation. Some of these features could be understood when the self generated turbulence is taken into account. When CR propagate through a plasma they can trigger the streaming instability which produces resonant Alfvén waves modifying the diffusive properties of the plasma and changing the CR transport itself in a complex non-linear fashion. In this talk I will highlight the role of this self-generated turbulence in several context of the CR journey: during the escape from their sources, close to molecular clouds and during the escape from the Galactic disk.

Speaker: Giovanni Morlino (Gran Sasso Science Institute)

Morlino_CRA2019.pdf

11:40 → 12:00 Waiting for the Nobel Prize in Physics announcement

12:00 → 12:30 Particle escape in middle-aged SNRs

The escape process of particles accelerated at supernova remnant (SNR) shocks is one of the poorly understood aspects of the shock acceleration theory. In this talk I will describe a phenomenological approach to study the particle escape and its impact on the gamma-ray spectrum resulting from hadronic collisions both inside and outside of a middle-aged SNR. Under the assumption that in the spatial region immediately outside of the remnant diffusion is suppressed with respect to the average Galactic one, I will show that a significant fraction of particles are still located inside the SNR long time after their nominal release from the acceleration region. This fact results into a gamma-ray spectrum that resembles a broken power law, similar to those observed in several middle-aged SNRs. Above the break, the spectral steepening is determined by the diffusion coefficient outside of the SNR and by the time dependency of the maximum energy. Consequently, the comparison between the model prediction and actual data will contribute to determining these two quantities, the former being particularly relevant within the predictions concerning the gamma-ray emission from the halo of escaping particles around SNRs which could be detected with future Cherenkov telescope facilities.

Speaker: Silvia Celli

Celli_CRA2019.pdf

12:30 → 13:00 Discussion

13:00 → 14:30 Lunch break

14:30 → 15:00 Recent results from the Tibet ASgamma experiment and related topics

The Tibet air shower array is located at 4,300 m above sea level, Tibet, China.
In 2014, an array of underground muon detectors is added under the surface
air shower array. We would like to present recent results from the Tibet
ASgamma experiment on cosmic ray anisotropy, Sun shadow, and gamma-ray observation, together with some related topics.

Speaker: Dr Masato TAKITA (ICRR, the University of Tokyo)

CRA2019_tibet-takita_20191008_v2.pdf

15:00 → 15:30 Diffusive shock reacceleration at Supernova remnant shocks

Diffusive shock acceleration has been successful in describing many aspects of particle acceleration at strong shocks. In the standard description, thermal particles are energized as they cross a shock and complete cycles of Fermi acceleration. Additionally, it has been proposed that non—thermal particles placed upstream of a shock can also be energized. This process, already discussed in Bell 1978, is known as diffusive shock reacceleration, and has recently been shown to be of importance, as for example to account for the non-trivial behavior of the secondary-to-primary Boron-to-Carbon ratio.

In this contribution, we propose to discuss the importance of particle reacceleration at SNR shocks, and on the subsequent gamma—ray emission from reaccelerated particles.

Speaker: Dr Pierre Cristofari (GSSI)

CRA2019_cristofari.pdf

15:30 → 16:00 Coffee break

16:00 → 16:30 Using Machine Learning to Interpret Arrival Directions of Ultra-high-energy Cosmic Rays

We propose a machine-learning-based method to test various
hypotheses about possible sources of ultra-high-energy cosmic rays (UHECR)
using their arrival directions. We test the discriminating power of
the method on the recently proposed realistic UHECR origin scenario [1], assuming several particular nearby active galaxies as source candidates.

[1] Phys.Rev. D96 (2017) no.8, 083006

Speaker: Oleg Kalashev (Institute for Nuclear Research RAS, Moscow, Russia)

cra19kalashev.pdf

16:30 → 17:00 Cosmic ray anisotropy study by means of muon bundles

In this work, muon bundles detected at the ground level are used as a tool for high energy cosmic ray anisotropy search. Due to their penetrating ability, muons with a good accuracy retain the direction of a primary particle. Long-term muon bundle registration from 2012 to 2019 was performed with the coordinate-tracking detector DECOR, which is a part of the Unique Scientific Facility “Experimental complex NEVOD” (Moscow, Russia). About 10 million events with primary energies more than 1 PeV were recorded. We describe a method which compensates the influence of the meteorological conditions on the intensity of muon bundles at the Earth surface. Results of the search of the dipole anisotropy of cosmic rays with energy more than 1 PeV are presented, and their comparison with those of other facilities is also given.

Speaker: Dr Mikhail Amelchakov (National Research Nuclear University MEPhI (Moscow Engineering Physics Institute))

CRA2019_Amelchakov.pdf

17:30 → 19:30 L'Aquila guided tour

Wednesday, 9 October

09:00 → 09:40 What can the cosmic ray composition tell us about the acceleration site

I will present some thoughts about the possible relation between the acceleration site of Galactic cosmic rays and the "anomalies" observed in their bulk source composition (like the Ne22/Ne20 excess and the recently detected abundance of radioactive Fe60).

Speaker: Nikos Prantzos (IAP)

09:40 → 10:20 Recent Cosmic Ray Observations from Voyagers 1 and 2

Voyagers 1 and 2 are now both in the interstellar medium. Voyager 1 crossed the heliopause on 25 August 2012 and Voyager 2 recently crossed on 5 November 2018. We find that the energy spectra of H, He, and electrons, which for the first time are being measured unaffected by the effects of solar modulation, are essentially identical at the two spacecraft. This implies that there are no significant gradients of these particles over a distance of ~167 AU in the local interstellar medium. We review some of the results contained in Cummings et al., ApJ, 2016, including the estimates of the energy density of cosmic rays and of the ionization rates of atomic H in the interstellar medium by cosmic rays. We also present preliminary spectra of a significant number of isotopes. With respect to the crossings of the heliopause by the two spacecraft, we compare observations at Voyager 2 with those at Voyager 1 and report on several differences. Finally, we report on the anisotropy of a few hundred MeV protons, which is observed by Voyager 1 much of the time in the local interstellar medium.
This work was supported by NASA under contract NNN12AA01C.

Speaker: Alan Cummings (Caltech, Pasadena US)

Cummings_CRA_2019_16x9_7.pdf

Cummings_CRA_2019_16x9_7.pptx

10:20 → 11:00 Coffee break

11:00 → 11:40 Solar Wind Interaction with the Local Interstellar Medium: Consequences for Cosmic Ray Propagation

We present the results of our investigation of the solar wind (SW) interaction with the local interstellar medium (LISM). The model is based on MHD treatment of ions and takes into account their charge exchange with neutral atoms. We focus on the structures that affect the Galactic cosmic ray (GCR) transport: magnetic barriers in the heliosheath, instability of the heliopause, heliospheric boundary layer of strongly depressed plasma density on the LISM side of the heliopause, the effect of the neutral solar wind on the bow wave in the LISM flow, and new discontinuities identified in the LISM at distances exceeding 2,000 au into the heliotail. Simulation results are validated by multiple observational data sets. In particular, we show strong correlation of GCR fluxes with Voyager 1 observations before it ultimately crossed the heliospheric boundary and entered the LISM. Our SW-LISM interaction pattern is also in agreement with the anisotropy of 1-10 TeV CRs observed in air shower experiments. We also discuss the properties of the SW and LISM turbulence observed in situ by the Voyager spacecraft.

Speaker: Prof. Nikolai Pogorelov (Department of Space Science, University of Alabama in Huntsville)

11:40 → 12:20 Global Anisotropies in TeV Cosmic Rays Related to the Sun’s Local Galactic Environment from IBEX

The Interstellar Boundary Explorer (IBEX) observes enhanced Energetic Neutral Atom emission from a narrow “ribbon” centered on the local interstellar medium (LISM) magnetic field direction. IBEX has improved knowledge of the local interstellar velocity based on interstellar atom measurements and provides global views of the structure of the evolving heliosphere.
These determinations are consistent with the interstellar modulation of high energy (TeV) cosmic rays and diffusive propagation from supernova sources revealed in global anisotropy maps of ground-based high-energy cosmic-ray instruments (Milagro, Asγ and IceCube). We discuss recent observations of the global heliosphere, the ribbon, and the properties of the local interstellar medium, which have implications for observed global anisotropies in TeV cosmic rays.

Speaker: Dr Nathan Schwadron (University of New Hampshire, Princeton University)

SchwadronAnisotropy-Oct6-2019-shorter2.pptx

12:20 → 13:00 The true anisotropy of TeV cosmic rays in the local interstellar medium

The Earth resides deep in the heliosphere. The trajectories of CRs measured in air shower experiments are affected by the electromagnetic fields of the heliosphere and disturbed LISM surrounding it. This may severely distort anisotropy maps. To study the properties of interstellar CRs, we should first remove the heliospheric influence. Recent advances in the heliospheric modeling based on observations from Voyager and IBEX have made it possible. In this paper, we reconstruct the anisotropy of TeV CRs in the pristine LISM. The results show a potential source of CR anisotropy and shed light onto the mechanisms of CR transport in the ISM.

Speaker: Prof. Ming Zhang (Florida Institute of Technology)

13:00 → 14:30 Lunch break

14:30 → 15:10 Magnetic fields in the Milky Way

I will present a quick summary of the current state of knowledge of interstellar magnetic fields in the Milky Way. I will focus on their turbulent component, which plays a decisive role in the acceleration, propagation and confinement of cosmic rays. I will discuss some recent observational breakthroughs, describe the theoretical tools that were developed to interpret radio observations, and summarize what we have ultimately learned from the new observations/

Speaker: Ferrière Katia (Observatoire Midi-Pyrenées, Toulouse (France))

ferriere.pdf

15:10 → 15:40 Relativistic charged particle diffusion in turbulent fields: synthetic vs dynamically-generated fields

The transport of high-energy cosmic rays in the Galaxy (energy about $10^{17}$ eV for protons) can be approached by means of numerical simulations, where relativistic charged test-particles propagate in a prescribed turbulent magnetic field. Thanks to the improvement in the computing capabilities, it is nowadays possible to investigate the particle propagation by using direct computations of the electromagnetic field performed through magnetohydrodynamic (MHD) simulations.

Here, by comparing the results obtained by adopting a synthetic model of turbulence or the fields produced through MHD simulations, we are able to analyze several important features, such as the rigidity dependence of the diffusion coefficient with and without a background magnetic field, the role of compressible fluctuations as well as the effects produced by intermittency.

Speaker: Oreste Pezzi (GSSI)

PEZZI_CRA_TALK.pdf

15:40 → 16:10 Coffee break

16:10 → 16:40 Anisotropy Variability Induced by the Chaotic Behavior of Cosmic Rays in Magnetic Bottles.

Cosmic rays propagate through the galaxy and in doing so, magnetic fields can generate chaotic behavior in their trajectories. Occasionally, these particles can get temporarily trapped in magnetic bottles, which affect the overall description of their propagation. As a result, anisotropy in the arrival distribution at Earth can emerge. In this work, we will show how the chaotic behavior of particles can be characterized by using the Finite-Time Lyapunov Exponents. Concretely, we will study cosmic rays trapped in a magnetic bottle that is subjected to different time perturbations, using the heliosphere as our motivation. Here, we also suggest that time-variability in the anisotropy can be a relevant factor in the understanding of how cosmic rays arrive at the Earth.

Speaker: Vanessa Lopez-Barquero (University of Wisconsin-Madison)

Vanessa_Lopez-Barquero_CRA2019.pdf

16:40 → 17:10 Recent progress in solar modulation modelling in light of new cosmic-ray data from AMS-02

After entering the Galactic cosmic rays (CRs) into the heliosphere, their intensities decrease during their propagation toward the Earth. This effect is subjected to a variety of physical processes through their propagation which referred to as CR solar modulation. The key ingredients in the study of this phenomenon are the knowledge of the local interstellar spectrum (LIS) of Galactic cosmic rays and the understanding of how the solar modulation affects the LIS inside the heliosphere. For this purpose, here we present an improved data-driven description of the solar modulation phenomenon, that is, the temporal evolution of the CR flux inside the heliosphere caused by the 11-year variability cycle of the Sun's magnetic activity. The model was applied to the Galactic proton flux measured by Voyager 1, AMS-02 and PAMELA missions which provide valuable information, allowing us to shed light on the shape of the LIS and the details of the solar modulation for the time period from mid-2006 to mid-2017. The new results for the temporal dependence of the key model parameters, their relationship with solar activity proxies, the implications for the CR transport in magnetic turbulence, and the new insights on our understanding of the solar modulation effect are presented.

Speaker: Dr Behrouz Khiali (INFN, Sez. di Tor Vergata, SSDC-ASI)

17:10 → 17:40 Telescope Array search for EeV photons

We present the results of a search for diffuse photons with energies higher than 1 EeV based on Telescope Array surface detector data and a novel neural network event analysis technique. The results of a search for point sources of photons for all directions in the Northern hemisphere and a search for several target source classes are also presented.

Speaker: Mikhail Kuznetsov (ULB & INR RAS)

mkuzn_091019.pdf

Thursday, 10 October

09:00 → 09:40 Observation and Interpretation of Small-Scale Cosmic-Ray Anisotropies

The arrival directions of Galactic cosmic rays are highly isotropic. This is expected from the presence of turbulent magnetic fields in our Galactic environment that repeatedly scatter charged particles during propagation. However, various cosmic ray observatories have identified weak anisotropies of various angular sizes and with relative intensities of up to a level of 1 part in 1,000. Whereas large-scale anisotropies are generally predicted by standard diffusion models, the appearance of small-scale anisotropies down to an angular size of 10 degrees is surprising. In this talk I will summarise the current experimental status of Galactic cosmic ray anisotropies and review theoretical ideas for the origin of small-scale anisotropies.

Speaker: Markus Ahlers (Niels Bohr Institute)

Ahlers_CRA2019.pdf

09:40 → 10:20 Cosmic ray small-scale anisotropies in quasi-linear theory

The paradigm for wave-particle interactions in cosmic ray physics, quasi-linear theory, cannot describe the small-scale anisotropies observed with high-precision observatories like IceCube and HAWC. This can be traced back to the loss of two-particle correlations when only the ensemble-averaged phase-space density is modelled.

After a brief review of standard quasi-linear theory, we consider two-particle correlations in a systematic and perturbative approach. We determine the angular power spectrum as the steady state of a differential equation describing the correlated transport of pairs of particles. As an example, we consider a toy model of isotropic turbulence and verify our result with numerical simulations. Our angular power spectrum compares favourably with data from the IceCube and HAWC observations.

Speaker: Philipp Mertsch (RWTH Aachen University)

Mertsch_CRA2019.pdf

10:20 → 11:00 Coffee break

11:00 → 11:40 MHD turbulence effects on energetic particle transport and acceleration

TBA

Speaker: William Matthaeus (University of Delaware)

11:40 → 12:20 Cosmic-Ray Anisotropy and Extended Gamma-Ray Emissions as Probes of Cosmic-Ray Transport

We calculate the shape of the anisotropy of TeV-PeV cosmic-rays (CR) in different models of the interstellar turbulence. In general, the large-scale CR anisotropy (CRA) is not a dipole, and its shape can be used as a probe of the turbulence and CR transport properties. The 400 TeV and 2 PeV data sets of IceTop can be fitted with Goldreich-Sridhar turbulence and a broad resonance function, but other possibilities are not excluded. We then present our first numerical calculations of the CRA down to 3 TeV energies in 3D Kolmogorov turbulence. At these low energies, the large-scale CRA aligns well with the direction of local magnetic field lines around the observer. In this type of turbulence, the CR intensity is flat in a broad region perpendicular to field lines. Even though the CRA is quite gyrotropic, we show that the local configuration of the turbulence around the observer does result in the appearance of weak, "non-gyrotropic" small-scale anisotropies, which contain information on the local turbulence level.
Finally, we show how extended gamma-ray emissions around CR sources can be used to extract information on the interstellar turbulence and CR transport properties. As an example, we use HAWC measurements to place constraints on the properties of the magnetic fields within $\simeq 25$ pc from Geminga pulsar. We also study the impact of CR-driven instabilities on the turbulence around CR sources, and show how one could use gamma-ray emissions to study these instabilities.

Speaker: Dr Gwenael Giacinti (MPIK Heidelberg)

Giacinti_CRA2019_Oct10_F.pdf

12:20 → 13:00 Modelling interstellar turbulence with anisotropy studies: options and difficulties

We report on recent simulations of small-scale anisotropy and its relation to the properties of interstellar turbulence. Emphasis will be placed on potential systematics in Monte-Carlo simulations of particle trajectories. We also describe a possible avenue to distinguish the contributions of the heliosphere and the local interstellar medium to the observed small-scale anisotropy of TeV-band cosmic rays.

Speaker: Martin Pohl

CR_Aniso_GSSI_MP.pptx

13:00 → 14:30 Lunch break

14:30 → 15:00 Unveil the origin of cosmic-ray leptons within a coherent multi-channel propagation scenario

The interpretation of cosmic-ray (CR) data still represents a major challenge that experiments have to face: a coherent interpretation of the measured CR spectra is hampered by our incomplete knowledge about both the acceleration mechanisms and the transport properties across the Galaxy. The main challenge in this context is to identify a unified picture that includes all the available observables. To this aim, we first perform a multi-channel fit of the available CR data based on the DRAGON numerical code, to set the relevant propagation parameters. On top of that, we discuss several physically-motivated possibilities (i.e. recent burst, constant injection, time-dependent emission) for the injection of $e^{+}e^{-}$ pairs accelerated at nearby antimatter factories, such as pulsar wind nebulae, and compute their propagation. Finally, we address the all-lepton spectrum and assess the contributions of both young, nearby supernova remnants, and possibly an additional hidden source, to the observed CR lepton flux above $\sim 1$ TeV recently measured by H.E.S.S., VERITAS, CALET and DAMPE.

Speaker: Mr Ottavio Fornieri (University of Siena/IFT Madrid)

CRA_fornieri.key

CRA_fornieri.pdf

15:00 → 15:30 Detection of a gamma-ray halo around Geminga with the Fermi-LAT and implications for the positron flux

An excess in the flux of cosmic positrons at Earth above 10 GeV has been
measured by Pamela, Fermi-LAT and with unprecedented precision by AMS-02.
The observed flux cannot be explained by the production of positrons in
the spallation reaction of hadronic cosmic rays with the interstellar
medium. Various interpretations have been invoked to explain this excess,
such as the production in Galactic supernova remnants and pulsar wind
nebulae (PWNe) or, intriguinly, in the dark matter halo of the Milky Way.
Recently, Milagro and HAWC experiments reported the detection of an
extended gamma-ray emission from Geminga and Monogem PWNe at TeV energies.
These nearby and powerful PWNe have been widely considered as the main
candidates to contribute to the cosmic positrons at Earth. Severe
constraints for a significant PWNe contribution to the positron excess can
be derived from this gamma-ray emission, which has been interpreted as
coming from the electrons and positrons accelerated in the PWNe and
undergoing inverse Compton scattering in the interstellar medium.
Moreover, the size of extension of these halos suggests that the diffusion
around PWNe is about two orders of magnitude less intense than the value
assumed to fit the cosmic-rays measured by AMS-02. In this contribution we
report the first detection of a significant emission from the Geminga halo
at GeV energies in Fermi-LAT data, derived by including the proper motion
of its pulsar. We present a detailed study of the gamma-ray halo around
Geminga and Monogem, and show the constraints found for the contribution
of these PWNe to the positron excess, combining Milagro and HAWC data with
measurements from the Fermi-LAT for the first time. The size of extension
and the consequences for the diffusion coefficient in these halos at GeV
energies are also explored. We demonstrate that using gamma-ray data from
the LAT is of central importance to provide a precise estimate for the PWN
contribution to the cosmic positron flux.

Speaker: Silvia Manconi

manconi_cra19.pdf

15:30 → 16:00 Coffee break

16:00 → 16:40 Surveying the Interstellar Magnetic Field within 40 parsecs with Polarized Starlight

An international group of scientists is mapping the configuration of
the very local interstellar magnetic field (ISMF) utilizing
high-sensitivity measurements of starlight that becomes linearly
polarized while traversing a medium containing magnetically aligned
interstellar dust grains. High-sensitivity polarization data for over
500 nearby stars reveal that the local interstellar medium within 40
pc contains magnetic filaments, some extending over 90 degrees in
angle. We discuss the relation between these filaments and
kinetically-defined local interstellar clouds, and similarities
between a filament and the ISMF shaping the heliosphere as deduced
from the IBEX ribbon of energetic neutral hydrogen atoms. The
polarizations indicate that magnetic filaments, common throughout the
interstellar medium, also extend into the immediate solar environment.
These new polarization data have been collected at eight observatories
located in both the northern and southern hemispheres; half of the new
polarization data were collected with the DIPOL instruments.

Speaker: Priscilla C. Frisch (University of Chicago)

16:40 → 17:10 Expected arrival-direction correlations between ultra-high-energy cosmic rays and high-energy neutrinos

The discovery of a diffuse flux of astrophysical neutrinos by IceCube has opened up new possibilities for the search of cosmic-ray sources. The sources that accelerate cosmic rays to extreme energies are most-likely also high-energy neutrino emitters. To find such sources one can look for correlations in arrival directions between astrophysical neutrinos and ultra-high-energy cosmic rays (UHECRs). However, UHECRs are deflected by magnetic fields on their way from their sources to Earth, and are subject to energy-loss processes (resulting in a maximum distance from which they can arrive). We investigate how these effects influence the expected probability to find correlations between high-energy neutrinos and UHECRs, depending on the evolution with redshift of the sources. The possibility to observe correlations between UHECRs and neutrinos is already strongly constrained by the absence of neutrino multiplets in the IceCube measurements. However, if connections between neutrinos and cosmic rays are measured, it would give a precise indication for the local density of the emitters.

Speaker: Arjen van Vliet (DESY Zeuthen)

20191010_AvV_NeutrinoCRCorrelation_CRA.pdf

17:10 → 17:40 Effects of the Galactic magnetic field on the spectrum, composition and arrival direction of cosmic rays

The energy spectrum of cosmic rays is one of the central measurements in cosmic ray physics. Mostly following a power law relation, it contains small breaks at the higher end of the energy range. Of particular importance are the so-called "knee" at around 5 PeV, where the spectrum softens, the "ankle" at around 5 EeV, where it hardens again, and a high-energy cut-off at around 50 EeV. The energy range between the knee and the ankle is where the transition from Galactic cosmic rays (GCRs) to extragalactic cosmic rays (EGCRs) is expected to occur; the knee is considered to be the point where the maximum rigidity of known GCR accelerators is reached for protons, whereas the ankle is thought to represent the point where the extragalactic component begins to dominate, as all Galactic accelerators are exhausted past this point. However, fits to the spectrum using current Galactic and extragalactic acceleration and propagation models, fail to describe the measured flux in this region, leaving the details of the transition poorly understood.
I wish to present results from simulations with the Monte Carlo-based cosmic ray propagation software CRPropa3 of the effects of the Galactic magnetic field (GMF) on cosmic rays that are expected from the rigidity-dependence of the degree of deflection in a magnetic field. They include the shielding of EGCRs from the Galaxy for low rigidities and a concentration effect in the Galactic plane for intermediate rigidities
as well as the gradual escape of GCRs from the Galaxy with increasing rigidity, due to the increasing strength of the GMF increases towards lower Galactic latitudes. These effects all occur at ridigites within the transition region and beyond the ankle, so this study may provide a better understanding of the transition from GCRs to EGCRs by potentially reproducing observed features in the spectrum, composition and the arrival direction distribution, such as the spectral hardening, the "lightening" of the composition and anisotropies.

Speaker: Alex Kääpä (University of Wuppertal)

talkHiRes.pdf

Friday, 11 October

09:00 → 09:40 The origin of the ultra-high energy cosmic-ray dipole

Although their astrophysical sources remain a mystery, new measurements brought by experiments such as the Pierre Auger Observatory and Telescope Array have radically improved our knowledge of the ultra-high energy cosmic-rays (UHECRs). I will present new results on the interpretation of the first significant UHECR anisotropy: a ~7% dipole, recently reported by Auger for cosmic rays above 8 EeV.

Speaker: Noemie Globus (New York University/Flatiron Institute)

09:40 → 10:20 Local sources, the Local Bubble and the CR anisotropy

The contribution of a single source to the observed cosmic ray (CR) dipole anisotropy depends only on the fraction the source contributes to the total CR intensity, its age and its distance, but not on the energy. Therefore the observation of a constant dipole anisotropy indicates that importance of single, local sources. I review some source types suggested as, e.g., Vela, a 2 Myr old supernova or young pulsars, and their signatures. Finally, I discuss how this picture is modified if the magnetic field structure of the Local Bubble distorts the CR flux.

Speaker: Michael Kachelriess (NTNU)

cra19.pdf

10:20 → 11:00 Coffee break

11:00 → 11:40 Time-dependent models for cosmic ray propagation

TBA

Speaker: Igor Moskalenko (Stanford)

19.Moskalenko_GS.pdf

11:40 → 13:00 Discussion

Discussion.pdf

13:00 → 15:00 Lunch break