PIRSA:17090068

Video URL

https://pirsa.org/17090068

Secondary Astrophysical Production of Anti-Deuteron and Anti-Helium3 Cosmic Ray

Sato, R. (2017). Secondary Astrophysical Production of Anti-Deuteron and Anti-Helium3 Cosmic Ray. Perimeter Institute for Theoretical Physics. https://pirsa.org/17090068

Sato, Ryosuke. Secondary Astrophysical Production of Anti-Deuteron and Anti-Helium3 Cosmic Ray. Perimeter Institute for Theoretical Physics, Sep. 22, 2017, https://pirsa.org/17090068 

          @misc{ scivideos_PIRSA:17090068,
            doi = {10.48660/17090068},
            url = {https://pirsa.org/17090068},
            author = {Sato, Ryosuke},
            keywords = {Particle Physics},
            language = {en},
            title = {Secondary Astrophysical Production of Anti-Deuteron and Anti-Helium3 Cosmic Ray},
            publisher = {Perimeter Institute for Theoretical Physics},
            year = {2017},
            month = {sep},
            note = {PIRSA:17090068 see, \url{https://scivideos.org/index.php/pirsa/17090068}}
          }

Ryosuke Sato Weizmann Institute of Science

Talk numberPIRSA:17090068
DOI10.48660/17090068
Source RepositoryPIRSA
Collection
Talk Type Scientific Series
Subject

Abstract

Cosmic-ray anti-deuterium and anti-helium have long been suggested as probes of dark matter, as their secondary astrophysical production was thought extremely scarce. But how does one actually predict the secondary flux? Anti-nuclei are dominantly produced in pp collisions, where laboratory cross section data is lacking. We make a new attempt at tackling this problem by appealing to a scaling law of nuclear coalescence with the physical volume of the hadronic emission region. The same volume is probed by Hanbury Brown-Twiss (HBT) two-particle correlations. We demonstrate the consistency of the scaling law with systems ranging from central and off-axis AA collisions to pA collisions, spanning 3 orders of magnitude in coalescence yield. Extending the volume scaling to the pp system, HBT data allows us to make a new estimate of coalescence, that we test against preliminary ALICE pp data. For anti-helium the resulting cross section is 1-2 orders of magnitude higher than earlier estimates. The astrophysical secondary flux of anti-helium could be within reach of a five-year exposure of AMS02.