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Ultra-High-Energy Cosmic-Ray Nuclei and Neutrinos in Models of Gamma-Ray Bursts and Extragalactic Propagation

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Ultra-High-Energy Cosmic-Ray Nuclei and Neutrinos in Models of Gamma-Ray Bursts and Extragalactic Propagation Ultra-high-energy cosmic-ray nuclei and neutrinos in models of gamma-ray bursts and extragalactic propagation DISSERTATION zur Erlangung des akademischen Grades doctor rerum naturalium (Dr. rer. nat.) im Fach: Physik Spezialisierung: Theoretische Physik eingereicht an der Mathematisch-Naturwissenschaftlichen Fakultät der Humboldt-Universität zu Berlin von M.Sc. Jonas Heinze Präsidentin der Humboldt-Universität zu Berlin: Prof. Dr.-Ing. Dr. Sabine Kunst Dekan der Mathematisch-Naturwissenschaftlichen Fakultät: Prof. Dr. Elmar Kulke Gutachter: 1. PD Dr. Walter Winter 2. Prof. Dr. Thomas Lohse 3. Prof. Dr. Günter Sigl Tag der mündlichen Prüfung: 27. Januar 2020 Selbständigkeitserklärung Ich erkläre, dass ich die Dissertation selbständig und nur unter Verwendung der von mir gemäß § 7 Abs. 3 der Promotionsordnung der Mathematisch-Naturwissenschaftlichen Fakultät, veröf- fentlicht im Amtlichen Mitteilungsblatt der Humboldt-Universität zu Berlin Nr. 42/2018 am 11.07.2018, angegebenen Hilfsmittel angefertigt habe. Abstract Ultra-high-energy cosmic rays (UHECRs) are the most energetic particles observed in the Uni- verse. Their energy spectrum, chemical composition and arrival directions are observed in extensive air-shower (EAS) experiments, notably the Pierre Auger Observatory (Auger) and Telescope Array (TA). While the astrophysical sources of UHECRs have not yet been uniquely identified, there are strong indications for an extragalactic origin. The interpretation of theob- servations requires both simulations of UHECR acceleration and energy losses inside the source environment as well as interactions during extragalactic propagation. Due to their extreme en- ergies, UHECR will interact with photons in these environments, producing a flux of secondary neutrinos. The IceCube observatory has detected a neutrino flux of astrophysical origin, which likely consists of neutrinos from astrophysical sources and not of neutrinos produced during extragalactic propagation of UHECRs (so-called ‘cosmogenic’ neutrinos). This dissertation deals with models of UHECR sources and the accompanying neutrino pro- duction in the source environment and during extragalactic propagation. At present, there is a wide range of possible UHECR source candidates with different UHECR acceleration and inter- action mechanisms. Therefore, the generic source properties imposed by propagation are studied in this thesis, as well as gamma-ray burst (GRBs) as one specific source candidate. These mod- els depend on the cross sections for photo-nuclear and hadronic interactions of UHECRs, which are only sparsely measured. This affects the photo-disintegration and photo-meson production both in the source and during extragalactic propagation. Furthermore, the EAS development is driven by hadronic interactions of UHECRs with air atoms, which introduces degeneracies in the interpretation of the observed data in terms of chemical composition. We have developed a new, computationally efficient code, PriNCe, for the extragalactic propagation of UHECR nuclei. The computational speed allows to efficiently vary the cross sections and photon-environments between runs. The PriNCe code is applied for an extensive parameter scan of a generic source model that is described by the spectral index, the maximal rigidity, the cosmological source evolution and the injected mass composition. In this scan, we demonstrate the impact of different disintegration and air-shower models on the inferred source properties. A prediction for the expected flux of cosmogenic neutrinos is derived, which is found to be out of range for future neutrino detectors, independent of the model uncertainties. GRBs are discussed as specific UHECR source candidates in the multi-collision internal-shock model. This model takes the radiation from different radii in the GRB outflow into account. We demonstrate how different assumptions about the initial setup of the jet and the hydrodynamic collision model impact the production of UHECRs and neutrinos. Motivated by the multi- messenger observation of GRB170817A, we discuss the expected neutrino production from this GRB and its dependence on the observation angle. We show that the neutrino flux for this event is at least four orders of magnitude below the detection limit for different geometries of the plasma jet. Kurzzusammenfassung Utrahochenergetische kosmische Strahlung (ultra-high-energy cosmic rays – UHECR) besteht aus ionisierten Atomkernen mit den höchsten Teilchenergien, die je gemessen wurden. Sie er- zeugen Luftschauer in der Erdatmosphäre, anhand derer Experimente wie das Pierre Auger Observatory (Auger) und das Telescope Array (TA) ihre Energien, chemische Komposition und Ankunftsrichtungen rekonstruieren. Zwar wurden die Quellen von UHECRs noch nicht eindeutig identifiziert, doch gibt es deutliche Anzeichen, dass sie extragalaktisch sind. Um die Beobachtun- gen zu interpretieren, wird sowohl ein Modell der UHECR Beschleunigung und Wechselwirkun- gen in der Quelle als auch der Wechselwirkungen während der extragalaktischen Propagation benötigt. Dabei werden astrophysikalische Neutrinos erzeugt, welche vom IceCube Observatory nachgewiesen wurden. Der gemessene Fluss besteht wahrscheinlich aus Neutrinos aus astro- physikalischen Quellen und nicht aus sogenannten kosmogenischen Neutrinos, die während der UHECR Propagation entstehen. Diese Dissertation behandelt Modelle der Quellen von UHECRs und die damit verbundene Produktion von Neutrinos sowohl in den Quellen als auch während der Propagation. Momentan gibt es eine Vielzahl von möglichen Quellen von UHECRs, in denen verschiedene Mechanismen zur Beschleunigung und Wechselwirkung von UHECRs führen können. In dieser Arbeit werden daher sowohl die generellen Eigenschaften der Quellen anhand der Propagation abgeleitet als auch Gammastrahlenblitze (gamma-ray bursts – GRBs) als eine spezielle Quelle behandelt. Für photohadronische Wechselwirkungen, welche einen wichtigen Einfluss auf die Disintegration in der Quelle und während der Propagation haben, liegen nur unzureichende Messungen vor. Zusätzlich hängt die Interpretation der chemischen Komposition in Luftschauerexperimenten von Modellen der hadronischen Wechselwirkungen von UHECR Atomen mit der Luft ab. Für diese Arbeit wurde ein neuer Code, PriNCe, für die Propagation von UHECRs entwickelt, der ermöglicht, die Wirkungsquerschnitte und Photonumgebungen effizient zwischen einzelnen Berechnungen zu variieren. Dieser Code wird in einem umfangreichen Parameterscan für ein generisches Quellenmodell angewendet, welches mit dem Spektralindex, der maximalen Rigidi- tät, der kosmologischen Quellenverteilung und der chemischen Komposition als freie Parameter definiert ist. Dabei wird der Einfluss von verschiedenen Photodisintegrations- und Luftschauer- modellen auf die erwarteten Eigenschaften der Quellen demonstriert. Der Fluss kosmogenischer Neutrinos, welcher sich aus dem erlaubten Parameterraum ableiten lässt, liegt unabhängig von den Modellunsicherheiten außerhalb der Reichweite aller derzeit geplanten Neutrinodetektoren. GRBs als mögliche Quellen von UHECRs werden im Multi-Collision Internal-Shock Modell simuliert, welches die Abhängigkeit der Strahlungsprozesse von den verschiedenen Dissipations- radien im Plasmajet berücksichtigt. Für dieses Modell wird der Effekt demonstriert, den ver- schiedene Annahmen über die anfängliche Verteilung des Plasmajets und das hydrodynamische Modell auf die resultierende UHECR- und Neutrinosstrahlung haben. Für den Gammastrahlen- blitz GRB170817A, welcher zusammen mit einem Gravitationswellensignal beobachtet wurde, werden Vorhersagen für den Neutrinofluss und ihre Abhängigkeit vom Beobachtungswinkel ge- macht. Diese liegen mindestens vier Größenordnungen unterhalb der Detektionslimits. Acknowledgements First, I would like to thank Walter Winter for his supervision and support during the three years of this PhD project. He taugh me alot about how to work as a scientist as well as about multi-messenger astrophysics in particular. I want to thank everyone in the NEUCOS group that I worked with and learned from. A special thanks goes to Anatoli Fedynitch and Denise Boncioli who I worked most closely with and who both taught me many different things about science. I also appreciate the collaboration with all of my co-authors in the publications written during this project, who have not been mentioned yet: Daniel Biehl, Mauricio Bustamante, Annika Rudolph, and Kohta Murase. I wish to thank everyone who helped me during the writing of this thesis. Denise, Anatoli, Arjen, Shan and Annika for reading different parts of the draft versions and providing valuable feedback. Thanks also to Sasha and Christina for proofreading the almost final version. Finally, I want to thank all of my friends and family, who have given me support and distrac- tion during the sometimes exhausting times of this project. I want to thank both my parents who have always supported me. Without them I would surely not have made it to this point. During my work leading to this thesis, I was supported by the European Research Council (ERC) under the European Union’s Horizon 2020 research and innovation program (Grant No. 646623) List of publications The following articles were published in connection with this dissertation. Peer-reviewed publications: • Mauricio Bustamante, Kohta Murase, Walter Winter, and Jonas Heinze. Multi-messenger light curves from gamma-ray bursts in the internal shock model. Astrophys. J., 837(1):33, 2017. doi: 10.3847/1538-4357/837/1/33
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