Coherent Neutrino Scattering
What is Coherent Elastic Neutrino-Nucleus Scattering?
As we like to call it, CEvNS (pronounced “sevens”) is a process that is well understood within the Standard Model of particle physics. The Standard Model has been well tested in many different experiments and includes the predicted Higgs boson that you have probably heard about. Since CEvNS is a Standard Model prediction, like the Higgs, it should in fact exist and it should be tested for. The main aim of the COHERENT collaboration is to make a first direct measurement of CEvNS.
As the name suggests, CEvNS is the process of a neutrino scattering off of a nucleus in both an elastic and coherent way. We won’t get into the many ways that neutrinos are interesting, but you can find a number of good sources out there. For our purposes, all you need to understand is that it is a fundamental particle (like an electron or a photon), it is very light, and it very rarely interacts in matter. In fact, on average, a low-energy neutrino would pass through an entire light-year of lead before interacting even once. Some people describe neutrinos as “elusive” particles because of the difficulty in detecting them.
When the neutrino scatters of the nucleus in a coherent and elastic way, this means that the neutrino “sees” the entire nucleus as one object. Sometimes neutrinos can scatter off of individual nucleons (protons and neutrons) within the nucleus. For CEvNS we are interested only in the case where all nucleons behave as one thing. For this process the target looks bigger to the neutrino and so this kind of process happens more often than scatters off of the individual nucleons.
How do you look for CEvNS and why hasn’t anyone seen it yet?
First we should talk about how you detect neutrinos. There are many experiments all around the world looking at neutrino interactions. In fact, the Nobel Prize in physics in 2015 went to the discovery that neutrinos have mass. Typically the way you detect a neutrino is through what is called the charged current interaction where a neutrino turns into its lepton counterpart. A fast moving neutrino can transform into an electron (or muon, or tau) and that particle moves through your detector. Scientists have gotten very good at detecting this process. It is still rare, because neutrinos rarely interact, but very large experiments have been built to look for neutrinos coming from the sun, the atmosphere, reactors, and other sources.
For CEvNS, the detection method is different. Here, the neutrino doesn’t change into another particle. It simply bounces off the target and continues on its way. So the signal for this process is not a fast moving electron or muon, but is a very slow-moving nucleus. The neutrino bounces off of the nucleus and just like in any collision, both objects feel the impact. It is very similar to bouncing a ping pong ball (the neutrino) off of a bowling ball (the nucleus) and measuring how the bowling ball rebounds. As you can imagine, doing this for a heavy nucleus is very challenging and this is why it has taken more than 40 years since theorists predicted CEvNS until detection. Only in recent years has detector technology (developed for looking for dark matter particle recoils) been available for detecting the tiny recoils from CEvNS.
For the COHERENT detectors, we are looking for these very small nuclear recoils on multiple kinds of nuclei. Using several different detectors allows us to take advantage of each systems strengths while working around weaknesses. We are also using one of the best neutrino sources in the world for this kind of measurement, although it was built to do entirely different things. The Spallation Neutron Source at Oak Ridge National Laboratory was built to do neutron physics, but their neutron production process also generates a huge number of neutrinos that have just the right energies for coherent scattering. Having very sensitive detectors near a very intense neutrino source with just the right neutrino energies will allow us to finally measure this process.
So why should we care?
We will need to do to determine if the CEvNS measurements that we make are consistent with the Standard Model. Measuring the predicted value would confirm that the Standard Model works well for this kind of interaction and would only increase our confidence in the model. If we were to measure a value that is different from the prediction, this would suggest that there is new physics there we don’t fully understand yet. And that would be very exciting.
In addition to confirming the model prediction, measurements of CEvNS on different nuclei would help us better understand some of the processes involved during supernovae (when stars explode). It will also help with backgrounds for future dark matter experiments. We could even possibly test for a potential mysterious sterile (non-interacting) neutrino. The CEvNS processes is an important one and we are excited about continuing the search on many on many other nuclei.
This is the current COHERENT collaborator list.
Note that some people are listed under more than one institution.
A * denotes the Collaboration Board member
Carnegie Mellon University
Diana Parno*, Rebecca Rapp, Yung-Ruey Yen
U. of Chicago
Peibo An, Connor Awe, Phil Barbeau, Baran Bodur, Erin Conley, Sam Hedges, Long Li, Daniel Pershey, Jay Runge, Kate Scholberg* (spokesperson), Gleb Sinev, Justin Raybern
University of Florida
Heather Ray*, Dipak Rimal
Maria del Valle Coello, Marissa D’Onofrio, Walt Fox, Max Hughes, Lisa Kaufman, Daniel Salvat, Mike Snow, Ben Suh, Rex Tayloe*, Tyler Thornton, Ivan Tolstukhin, Daniel Winney, John Vanderwerp, Gerard Visser, Jacob Zettlemoyer
Dmitri Akimov*, Vladimir Belov, Alexey Konovalov, Ekaterina Kozlova, Dmitry Rudik
KAIST (Korea Advanced Institute of Science and Technology)
Clarence Virtue*, Andrea Gallo-Rosso
Robert Cooper, Steve Elliott*
Dmitri Akimov, Vladimir Belov, Alexander Bolozdyna*, Yuri Efremenko, Alexander Etenko, Alexander Khromov, Alexey Konovalov, Alexander Kumpan, Yury Melikyan, Dmitry Rudik, Valery Sosnovtsev, Alexey Shakirov
Diane Markoff*, Jordan Sibley, Erem Ujah
Matt Green*, Keith Mann
Matthew Blackston, David Dean, Lorenzo Fabris, Michael Febbraro, Alfredo Galindo-Uribarri, Matt Green, Matt Heath, Erik Iverson, Wei Lu, Paul Mueller, Jason Newby*, Seppo Penttila, David Radford, Robert Varner, Chang-Hong Yu
Belkis Cabrera-Palmer*, David Reyna
U. of South Dakota
Dmitry Chernyak, Keyu Ding, Jing Liu*
U. of Tennessee
Brandon Becker, Jacob Daughhetee, Yuri Efremenko*
Peibo An, Connor Awe, Phil Barbeau*, Sam Hedges, Stuart Ki, Long Li, Justin Raybern, Jay Runge, Diane Markoff
Jon Link*, Karla Tellez-Giron-Flores
U. of Washington
Follow us on Twitter!