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Bereits 1912 entdeckte Viktor Hess die als kosmische Strahlen bekannten hochenergetischen Teilchen, die im Sekundentakt aus dem Weltall auf die Erdatmosphäre treffen. Einige von ihnen stammen aus unserer Sonne, andere von Quellen in unserer eigenen Galaxie – bei den höchsten Energien liegen die Ursprünge allerdings vermutlich in weit entfernten Galaxien. Unglücklicherweise handelt es sich größteils um geladene Ionen, die auf ihrem Weg durch das Universum durch Magnetfelder abgelenkt werden und nicht zu ihren Quellen zurückverfolgt werden können. Deswegen konnte in den mehr als 100 Jahren seit ihrer Entdeckung keine eindeutige Quelle extragalaktischer kosmischer Strahlen identifiziert werden.
Trotz allem gibt es dort draußen Objekte, die winzige Teilchen mit den unvorstellbar geringen Massen von 10^-24g auf die Energie beschleunigen, mit der Rafael Nadal seine Tennisbälle aufschlägt. In irgendeiner Form müssen diese Objekte strahlen und neben kosmischen Strahlen auch andere Teilchen emittieren. Hier setzt die Idee von Multi-Messenger Astroteilchenphysik an: Bei der Untersuchung der energiereichsten Objekte unseres Universums werden zugleich Licht, Neutrinos und Gravitationswellen betrachtet, allesamt ungeladene Boten, die Informationen von den Quellen direkt zu unseren Detektoren tragen. Während 2017 Gravtitationswellen eines Gammastrahlenblitzes identifiziert werden konnten, war der diesjährige Durchbruch in der Multi-Messenger Astroteilchenphysik die Assoziation eines von IceCube detektierten Neutrinos mit einem bekannten Blazar in einer weit entfernten Galaxie.
In diesem Vortrag erklären wir, was Menschen zum Bau komplexer Detektoren an den exotischsten Plätzen der Welt motiviert, um hochenergetische Teilchen aus dem Weltall zu jagen. Wir sprechen über die bahnbrechende Entdeckung diesen Jahres und beleuchten, wie der Durchbruch durch twitter-ähnliche Echtzeit-Monitoring-Systeme überhaupt erst möglich wurde.
5.7 billion years ago, the blazar TXS0506+056, a gigantic particle accelerator driven by the super-massive black hole at the center of its host galaxy, emitted a large number of weakly interacting elementary particles, known as neutrinos. One of these particles found its way to Earth and interacted with water molecules in the South-Antarctic Ice Sheet. Fortunately, the IceCube Observatory, a cubic kilometer of instrumented ice recorded a track of light that pointed directly back to its origin, unlike many other neutrinos captured in the past. This event, called IceCube-170922A writes history, since for the first time a concrete astrophysical object can be associated to the origin of this neutrino and thus the presence of strongly accelerated, interacting matter. A second look at the data recorded in 2014-2015 confirmed that the blazar has indeed periods of high-neutrino emission, strengthening the confidence in the 2017 event to be a real discovery and great success for Multi-Messenger Astrophysics.
As discovered by Victor Hess already in 1912, there are particles impinging the Earth’s atmosphere every couple of seconds called Cosmic Rays. Some of them are accelerated in the sun, others by sources in our galaxy but at the highest energies, these particles are very likely coming from distant galaxies. Unfortunately, most of them are charged ions that are deflected by magnetic fields on their way through the universe and they do not point back to the point where they have been accelerated. Therefore, even 100 years after the discovery of cosmic rays a definite and obvious source has not been discovered. However, there is something out there that can accelerate a tiny particle with a mass as little as 10-24g (this is a number with !23! decimal zeros) to the energy equivalent to a tennis ball served by Rafael Nadal, then it must somehow shine and emit other radiation among the Cosmic Rays. This is the basic idea of multi-messenger astrophysics that aims to study the most violent objects in the universe by looking simultaneously at the emitted light, the neutrinos and the gravitational waves, which are all uncharged messengers carrying the information from the sources directly to our detectors. While n 2017, gravitational waves from a Gamma-Ray Burst were identified, this years major breakthrough in the field of multi-messenger astrophysics was the association of a high energy neutrino detected by IceCube with a known blazar in a far away galaxy.
In this lecture, we will aim to explain what motivates mankind to build complex observatories at the most exotic location around the globe to haunt for very high energy particles from space. We will shed light on this brand new detection and highlight that without the recent developments in a real-time monitoring/Twitter-like system the detection would have gone unnoticed.
Image / Video Credits
Titelbild: NASA
B2 Uni Wien
B3 NASA
B4 CERN / LHC
B5 Auger Collaboration
B6 Sven Lafebre
B7 NASA
B8 A. Fedynitch DESY
B9 IceCube Observatory
B10 freier-grafiker.de
B11 IceCube Collaboration
B12 https://military.id.me/
B13 Argonne National Laboratory
B14 IceCube Collaboration
B15 IceCube Collaboration
B16 DESY (Renderbild)
B17 IceCube Collaboration
B18 IceCube Collaboration
B19 IceCube Collaboration
B20 Science Communication Lab und DESY (https://multimessenger.desy.de/ )
B21 Science Communication Lab und DESY (https://multimessenger.desy.de/ )
References
R1 https://www.mpi-hd.mpg.de/hfm/HESS/public/vfHess.pdf (DE) ausführliche Diploma-Thesis
R2 https://arxiv.org/abs/1808.02927 Original-Paper inkl. Kommentare
R3 https://arxiv.org/abs/1701.07305 Proceedings on electron positron fluxes (AMS Coll. )
R4 https://arxiv.org/abs/astro-ph/0609060 Auger Observatory
R5 https://arxiv.org/abs/1502.01323 ausführliche Detektorbeschreibung
R6 https://arxiv.org/abs/1604.03637 AugerPrime Design Report, ohne AERA Radio Det.
R7 https://arxiv.org/abs/1311.7346 Galactic Cosmic Rays Review
R8 https://arxiv.org/abs/1804.02331 Galactic CR from young massive stars
R9 https://arxiv.org/abs/0711.2256 2008 Correlation of UHECR with AGN (Auger Coll.)
R10 https://arxiv.org/abs/1709.07321 2017 large scale UHECR anisotropy (Auger Coll.)
R11 https://arxiv.org/abs/0812.3809 High Energy Neutrino Detectors overview
R12 https://arxiv.org/abs/1412.5106 IceCube Gen2
R13 https://arxiv.org/abs/1607.02671 PINGU IceCube
R14 https://arxiv.org/abs/1612.05093 IceCube Instrumentation and Online Systems (DOM)
R15 http://science.sciencemag.org/content/342/6161/1242856.full (https://arxiv.org/abs/1311.5238 )
R16 https://arxiv.org/abs/1805.11112 Neutrino Astronomy focus IceCube
R17 http://science.sciencemag.org/content/361/6398/eaat1378 (open access: https://arxiv.org/abs/1807.08816 )
R18 http://science.sciencemag.org/content/361/6398/147 (open access: https://arxiv.org/abs/1807.08794 )
R19 https://arxiv.org/abs/1807.04275 modeling TXS2
R20 http://adsabs.harvard.edu/abs/1993ARA%26A..31..473A AGN Unification scheme 1993
R21 https://arxiv.org/abs/1107.5576 AGN UHECR
R22 https://arxiv.org/abs/1812.05939 Historical flare conventional models
R23 https://arxiv.org/abs/1809.00601 Gas - Jet interaction model for historical flare