TRIUMF Science Week

16 Jul 2018, 08:00 → 19 Jul 2018, 18:00 UTC

TRIUMF and UBC

 

– TRIUMF SCIENCE WEEK 2019 –

TRIUMF's Science Week 2018 will be held from July 16 – July 19, 2018. In celebration of TRIUMF's 50th anniversary, the week will include a special alumni event and a 50th Anniversary Science Symposium, in addition to the ARIEL Science Workshop and the TRIUMF User's Group Annual General Meeting.

Registration is now open for the Science Symposium, the ARIEL Workshop, and the TUG AGM; the cost for registration is $10. Registration for the alumni event on July 16th is free, and tickets are now available online here (https://www.eventbrite.ca/e/bringing-together-triumfs-history-and-future-tickets-45992613144)   (password: TRIUMF50).

Register for Science Week here: http://mis.triumf.ca/events/event.jsf?confcode=SW2018

 

More information: 

https://www.triumf50.com/

http://www.triumf.ca/science-week-2018

 

Slides Bagger_50.pdf

Monday, 16 July

09:30 → 10:00 Welcome

10:00 → 12:30 Morning Sessions | TRIUMF's Building Years | TRIUMF's Scientific and Technical Evolution | TRIUMF as a Training Tool

12:30 → 13:30 TRIUMF BBQ Lunch

BBQ Lunch

13:15 → 13:30 TRIUMF Group Photo

13:30 → 15:00 TRIUMF Working Groups Poster Session)

TARA is looking for help in creating posters for the TRIUMF Working Groups Poster Session: a celebration of this community, past and present.
The posters should feature photos that focus on the people of TRIUMF, with minimal text. The goal of these posters is to spark discussions and connections between past and current employees at TRIUMF. There are many untold stories at TRIUMF – this is an opportunity to share those stories with the members of our community. Many legacy photos can be found at http://archive.triumf.ca/gallery/.

15:00 → 16:00 Reception

Tuesday, 17 July

09:00 → 09:15 Welcome, Jonathan Bagger, Director, TRIUMF

slides Bagger_50.pdf

09:15 → 09:25 Remarks, Santa Ono, President, University of British Columbia

09:25 → 10:00 Early Cyclotron Days: Dave Axen (UBC Emeritus)

slides D_Axen_Science_week.pptx

10:00 → 10:35 Science at the Meson Facility: Ryugo Hayano (Tokyo Emeritus)

slides Hayano_TRIUMF50.pdf

10:35 → 11:10 Always at the Forefront - From NN Experiments to Ab-Initio Theory: Achim Schwenk (Darmstadt)

slides Schwenk_TRIUMF50_2018.pdf

11:10 → 11:25 BREAK

11:25 → 12:00 Life Sciences at TRIUMF: Suzy Lapi (Alabama)

slides Lapi_TRIUMF_July_2018_final.pptx

12:00 → 12:35 Material Sciences and Quantum Materials at TRIUMF: Rob Kiefl (UBC)

slides RobKiefl_Scienceweek2018.pdf

12:35 → 13:00 Accelerator Science and Achievements - SRF at TRIUMF: Lia Merminga (Fermilab)

slides Merminga_SRF-TRIUMF-final.pptx

13:00 → 13:45 LUNCH

13:45 → 13:55 Remarks, Mario Pinto, President, Natural Sciences and Engineering Research Council of Canada

13:55 → 14:30 On-Site Program - From TWIST & PIENU to UCN: Luca Doria (Mainz)

slides Doria_ScienceWeek.pdf

14:30 → 15:05 TRIUMF Neutrino Program - T2K: Dean Karlen (UVic)

slides karlen_T2K.pdf

15:05 → 15:40 High-Energy Frontier - TRIUMF and HERA & LHC: Manuella Vincter (Carleton)

slides ManuellaVincter_TRIUMF_Vincter.pptx

15:40 → 15:55 BREAK

15:55 → 16:30 From TISOL to ISAC to ARIEL: Paul Schmor (TRIUMF Retired)

slides Schmor_T2I2A_final.ppt

16:30 → 17:05 Nuclear Astrophysics - Red Giants and Neutron Star Mergers: Gavin Lotay (Surrey)

slides Lotay_TRIUMF_ScienceWeek.pptx

17:05 → 18:00 Panel Discussion - TRIUMF: Past, Present, Future

Moderator: Paolo Pietropaolo,
Panelists: Angela Bracco (INFN, Milano),
Gilles Patry (U15),
Jerry Porter (Nordion),
Genevieve Tanguay (NRC)

18:00 → 19:30 RECEPTION

Light reception in Atrium foyer.

Wednesday, 18 July

09:00 → 10:10 R-Process Sites

Convener: Dr Iris Dillmann (TRIUMF)

09:00 Introduction

Speaker: Greg Hackman (TRIUMF)

Slides intro-asw18.pdf

09:10 Daddy, Where Did I Come From?

I will outline how nearly all of the elements essential to you are produced in the evolution of low-mass and high-mass stars and in white-dwarf binaries. All the essential elements except for iodine, that is. The story of where did iodine come from along more common materials like platinum (yes, platinum is more common in the Universe) was a mystery for 60 years between when B2FH first posed the question and the discovery of the production of lanthanides in the merging of neutron stars in 2017. What are neutron stars, why did astronomers argue that they could be the source for the r-process elements, and what may we learn in the future?

Speaker: Jeremy Heyl (University of British Columbia)

Slides heyl-asw18.pdf

09:40 Neutron Stars and Mergers

We discuss observations of neutron stars and neutron star mergers and how these depend on the equation of state and other properties of dense neutron rich matter. We also discuss some related laboratory experiments with neutron rich nuclei.

Speaker: Chuck Horowitz (Indiana University)

Slides horowitz-asw18.pdf

10:10 → 10:40 Coffee Break

10:40 → 12:15 R-Process Theory

Convener: Dr Jason Holt (TRIUMF)

10:40 The R-Processes and their Astrophysical Sites

The r-process occurs in neutron star mergers. This has been confirmed by the observation of the decay of neutron rich radioactive nuclei as a kilonova light curve after the neutron star merger detected with gravitational waves GW170817. We study the nucleosynthesis and kilonova light curves from different ejecta of neutron star mergers discussing the astrophysical and nuclear physics uncertainties. Moreover, core-collapse supernovae driven by neutrinos can produce elements up to silver. The astrophysical and nuclear physics uncertainties of this weak r-process will be discussed. In order to have a successful r-process and to produce the heaviest elements in core-collapse supernovae, magnetic fields are necessary. We will report about the impact of rotation and magnetic fields based on recent simulations including detailed neutrino transport

Speaker: Almudena Arcones (Technical University of Munich)

Slides Arcones-ASW18.pdf

11:10 Fission in the R-Process

Last August marked the first observation of gravitational waves and electromagnetic signals from the merging of two neutron stars sending ripples through the astrophysics, atomic physics, nuclear physics and gravitational wave communities. In some components of neutron star merger ejecta fission is thought to re-cycle the material and impact the abundances. I will focus the talk on the sensitivity of the r-process to theoretical calculations of fission, in particular, the treatment of neutron-induced fission, beta-delayed fission and fission yields. The production of the heavy actinide Californium-254 will be discussed along with its impact on observational signatures of kilonovae.

Speaker: Matthew Mumpower (Los Alamos National Laboratory)

notes prism-movie.mp4

Slides http://matthewmumpower.com/content/presentations/ASW2018/index.html#/first

11:40 Onward and Upward: Prospects for applying ab initio methods to the structure of medium-heavy nuclei

The past decade or so has seen great progress in applying effective field theory ideas and non-perturbative many-body methods towards the quantitative prediction of the structure of light nuclei. I will give a brief overview of this program and discuss work in progress to extend this success up the nuclear chart beyond A=100, with a focus on binding energies, beta decay, and the limits of stability.

Speaker: Ragnar Stroberg (Reed College)

Slides stroberg-asw18.pdf

12:10 Discussion

12:15 → 13:15 Lunch Break

13:15 → 15:00 R-Process Experiments

Convener: Greg Hackman (TRIUMF)

13:15 R-Process Sensitivities and Measurements

The origins of the heavy elements have continued to be one of the grand challenges for all of science in the 21st century. The recent observation of gravitational waves from two neutron star mergers simultaneously with the spectroscopy showed that rare earth elements are in fact being made in neutron star mergers. While questions remain about sufficient numbers of mergers to account for the observed abundances of the heavy elements in the universe and whether mergers are the only sources of the heavy elements, measurements of the most exotic nuclei that we can make in our laboratories are the most powerful tools for understanding the astrophysical conditions in which the r-process operates. I will present results of our sensitivity studies and quantifications of nuclear uncertainties to point out the most impactful nuclei to measure and the precision with which they should be measured.

Speaker: Ani Aprahamian (University of Notre Dame)

Slides ARIEL-Aprahamian.pdf ARIEL-Aprahamian.pptx

13:45 Capabilities of ARIEL

The new beam delivery capabilities of the ARIEL facility offer many exciting science opportunities. Among these new possibilities is access to isotopes of particular importance to characterizing the rapid-neutron capture process. Understanding the mechanisms responsible for creating the elements in our universe is one of the most compelling open questions in contemporary science. I will give an overview of the capabilities of the ARIEL facility which will help answer these questions.

Speaker: Dr Adam Garnsworthy (TRIUMF)

Slides garnsworthy-asw18.pdf

14:15 Opportunities for Nucleosynthesis Studies with TI-STAR and TIGRESS at ARIEL

The goal of the TI-STAR (TIGRESS Silicon Tracker Array) project is to build a new tracking silicon detector, combined with an extended gas target that will fit in the TIGRESS gamma detection array at ISAC-II. Different from (active) gas detectors, TI-STAR will use a silicon tracker with an ultra-thin first silicon layer to track the emitted recoiling nuclei. In this talk we will focus on the future opportunities of TI-STAR and TIGRESS related to explosive nucleosynthesis studies at ARIEL. One main goal of TI-STAR is to use the intense and clean ARIEL beams to study neutron-capture rates in A=130 and A=200 r-process nuclei. The simultaneous measurement of excitation energy (TI-STAR) and gamma ray response (TIGRESS) will allow to deduce the neutron-capture rates for key nuclei along the r-process via the "Oslo" method. Also, precise spectroscopy of exotic, proton-rich nuclei along N=Z will dramatically improve our understanding of the rp-process. Another topic are indirect studies of low-lying resonance properties in unstable nuclei, relevant to characterize capture rates in the late stages of helium burning in AGB and Wolf-Rayet stars.

Speaker: Dennis Muecher (University of Guelph)

Slides muecher-asw18.pdf muecher-asw18.pptx

14:45 Discussion

15:00 → 15:30 Coffee Break

15:30 → 18:00 New Directions for Ariel

Convener: Dr David Morrissey (TRIUMF)

15:30 Theory of dark photons and dark sectors

I will review dark sectors—a generic name for new, light particles that couple weakly to the standard model—with a focus on dark photons. Dark sectors have received a large amount of attention in recent years as explanations of a number of experimental anomalies and as the source of the Universe's dark matter, required by astronomical and cosmological observations. I will discuss future prospects to discover dark photons and dark sectors, highlighting new experimental probes.

Speaker: David McKeen (TRIUMF)

Slides mckeen-asw18.pdf

16:00 Opportunities for Dark Sector Searches with ARIEL

The availability of a high-current electron accelerator at TRIUMF opens novel avenues for dark sector experiments. In particular, fixed-target experiments represent an excellent opportunity for testing dark sector scenarios with high sensitivity. After reviewing some existing experimental proposals, sensitivity calculations for an experiment at TRIUMF taking advantage of the ARIEL beam will be presented.

Speaker: Luca Doria (JGU Mainz)

Slides doria-asw18.pdf

16:30 TRIUMF e-linac production of weakly-coupled MeV-mass particles

I will discuss backgrounds and possible scenarios using TRIUMF's existing e-linac to produce and detect MeV-mass particles, assuming the previous talks and somewhat dated PPAC submission (daqshare.triumf.ca/~trinat/darkPPAC.pdf). The recent improved measurement of the fine-structure constant predicts a different electron g-2 compared to experiment, motivating experimentally accessible MeV-mass bosons. Assuming zero background-- essential for sensitivity to increase linearly with counting time-- the highest-energy electron beam will always win, as production scales like bremsstrahlung. Yet e-linac experiment backgrounds have two natural plateaus: pion threshold and (gamma,neutron) threshold. Thermal neutrons can produce 10 MeV single-gamma events distinguishable from exotic particles only by direction, so experiments at our low e-linac energies must face this issue both from the cyclotron (the BGO array at DRAGON sees those) and the e-linac . Neutron damage of electronics in the ISAC mass separator room may prove problematic for that location. This motivates a scenario that disturbs neither cyclotron beamtime nor e-linac production of neutron rich nuclei: two pulsed lasers on a photocathode to independently fill the half of the buckets left unused by ARIEL; Doug Storey's resonant chopper after either the 10 MeV injector (below (gamma,n) threshold on many materials) or the full 35 MeV; a high-Z detector technology with 10's of psec timing resolution to utilize the 10 psec/1.5 nsec duty cycle for Mev-mass TOF and suppress backgrounds; a detector after 1.5 meters of tungsten-steel shielding, either in the air in the e-hall to avoid scattered neutrons from the floor or burrowed west to suppress cosmic rays one order. The 10 MeV version appears compatabile with a THz radiation source (see workshop July 5)

Speaker: John Behr (TRIUMF)

Slides ariel_workshop_behr.pdf ariel_workshop_behr_v3.pdf

17:00 From Nano Materials to Giant Resonances - ARIEL Target Ion Source Opportunities

ARIEL will dramatically increase the availability of radioactive ion beams by harvesting isotopes from three target stations simultaneously - a worldwide unprecedented technology - enhancing the scientific output of the laboratory. For the first time, high-power electrons (up to 500 kW) will be converted into gamma rays inducing photonuclear reactions in one target, while two others are being bombarded with protons from TRIUMF’s 500 MeV cyclotron. The intrinsic properties of 35-50 MeV electrons are fundamentally different than of MeV neutrons or 0.1 to 2 GeV protons, commonly used for ISOL, calling for a wide range of target ion source development. ARIEL will open new avenues towards functionalized materials, advanced target concepts, and improved ion sources, tailored for meeting tomorrow’s demand of exotic and pure radioisotope beams.

Speaker: Dr Alexander Gottberg (TRIUMF)

17:30 Discussion and Closeout

Speaker: Greg Hackman (TRIUMF)

18:00 → 20:00 BBQ

Thursday, 19 July

09:00 → 09:05 Welcome: Jon Bagger (TRIUMF)

09:05 → 09:20 Physical Science Division Report: Jens Dilling (TRIUMF)

09:20 → 09:35 Life Science Division Report: Paul Schaffer (TRIUMF)

09:35 → 09:50 Accelerator Division Report: Oliver Kester (TRIUMF)

09:50 → 10:05 ARIEL Update & Impact: Reiner Kruecken

slides ARIEL-TUG-AGM_July2018.pdf

10:05 → 10:25 ARIEL discussion: Moderated by Kyle Leach (Colorado Sch. Mines)

Convener: Dr Anna Kwiatkowski (TRIUMF)

10:25 → 10:50 COFFEE BREAK

10:50 → 11:10 Student Talk: 119Sb: Production, radiochemical separation, and chelation of a promising candidate for targeted radionuclide therapy: Jenasee Mynerich (McMaster U.)

11:10 → 12:10 Student Poster Slam

12:10 → 13:10 LUNCH

13:10 → 13:30 SNOmass white paper: Tony Noble (Queens U.)

13:30 → 13:50 Future prospects of rare isotope science with CANREB: Ritu Kanungo (St. Mary's U)

13:50 → 14:10 First ultracold neutrons at TRIUMF - TUCAN's path toward a neutron electric dipole moment search: Beatrice Franke (TRIUMF)

14:10 → 14:30 Extra-terrestrial neutrinos: the imprint of compact objects: Liliana Caballero (U. Guelph)

14:30 → 14:50 Prospects for THz/Infrared photon source powered by TRIUMF e-linac: Victor Verzilov (TRIUMF)

14:50 → 15:00 TUG updating charter & bylaws: Ania Kwiatkowski (TRIUMF) & Geoff Grinyer (U. Regina)

15:00 → 16:00 Poster Session & Break: Students and Postdoctoral Fellows

16:00 → 16:20 The 19Ne( p,γ) 20Na Reaction in ONe Novae - First Direct Measurement of the E_c.m. = 457 keV Key Resonance with DRAGON: Annika Lennarz (TRIUMF)

16:20 → 16:40 IAMI: Paul Schaffer (TRIUMF)

16:40 → 17:00 5YP & PPAC: Reiner Kruecken (TRIUMF)

slides TUG-AGM-July2018-web.pdf

17:00 → 17:20 5YP & PPAC disc.: Moderated by Ania Kwiatkowski (TRIUMF)

slides TUG-AGM-July2018-web.pdf

17:20 → 17:30 Open Discussion

17:30 → 17:35 Closing