GK Seminars WS 16/17


Tue 13.12.2016, 16.30 h (28B110)

P. Fischer (Heidelberg)

Novel fast and position sensitive photo detectors based on SiPMs and APDs


Tue 20.12.2016, 16.30 h (28B110)

K. Hagiwara (KEK and Wisconsin)

Physics potential of T2HKK: neutrino oscillation from Tokai to Hyper-Kamiokande in Kamioka and in Korea

We examine physics discovery potential of placing a far detector in Korea along the baseline of the T2HK (Tokai-to-HyperKamiokande) neutrino oscillation experiments, within the three neutrino standard model and its extentions.  Preliminary results for the determination of the neutrino mass ordering, the CP violating phase of the lepton flavor mixing matrix, and resolution of the octant degeneracy in the 2-3 mixing angle are reported for the following configuration of the T2HKK experiment: 2.5 degree off-axis beam (OAB) at T2K (22kton) and T2HK (100kton), both at the baseline of L=295km, and a 100kton HK type detector in Korean site H (Mt.Bisul) at L=1088km with 1.3 degree OAB, or in site C (Mt.Bohyun) at L=1040km with 2.3 degree OAB, with 1.35 x 10^{21} POT (protons on target) per year each for \numu and \numubar beam.


Tue 10.01.2017, 16.30 h (28B110)

F. Staub (KIT)

Introduction to gauge mediated SUSY breaking

After a brief introduction into SUSY and SUSY breaking in general, I discuss Gauge Mediated SUSY Breaking (GMSB). In the first part, the main phenomenological aspects of minimal gauge mediation are summarized, but also the main problems stemming from the measured Higgs mass as well as from cosmological observations are pointed out. In the second part, different ideas to circumvent these problems are presented.


Tue 17.01.2017, 16.30 h (28B110)

R. Beck (MPIfR, Bonn)

Magnetic fields of nearby galaxies, the Milky Way, and the intergalactic space

The strength and structure of cosmic magnetic fields can be well studied by observations of radio continuum emission, its polarisation and Faraday rotation. Total fields in spiral arms are strong due to amplification and compression of turbulent fields and are dynamically important. The strongest regular fields are found in interarm regions, sometimes forming 'magnetic spiral arms' between the material arms. Faraday rotation measures of the polarisation vectors reveal large-scale patterns that are signatures of a mean-field dynamo. Our Galaxy hosts magnetic fields of similar strength as in spiral galaxies, while the global field structure in the disk and halo is not yet known. Several large-scale field reversals have been claimed from rotation measure data of pulsars. Nothing similar has been found so far in external galaxies. Intergalactic magnetic fields are hard to observe, so that (not surprisingly) only crude estimates are available so far.