Antiprotons and Elementary Particles over a Solar Cycle: Results from the Alpha Magnetic Spectrometer Article Swipe
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· 2025
· Open Access
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· DOI: https://doi.org/10.1103/physrevlett.134.051002
· OA: W4407100443
We present results over an 11-year Solar cycle of cosmic antiprotons based on <a:math xmlns:a="http://www.w3.org/1998/Math/MathML" display="inline"><a:mn>1.1</a:mn><a:mo>×</a:mo><a:msup><a:mn>10</a:mn><a:mn>6</a:mn></a:msup></a:math> events in the rigidity range from 1.00 to 41.9 GV. The <c:math xmlns:c="http://www.w3.org/1998/Math/MathML" display="inline"><c:mover accent="true"><c:mi>p</c:mi><c:mo stretchy="false">¯</c:mo></c:mover></c:math> fluxes exhibit distinct properties. The magnitude of the <g:math xmlns:g="http://www.w3.org/1998/Math/MathML" display="inline"><g:mover accent="true"><g:mi>p</g:mi><g:mo stretchy="false">¯</g:mo></g:mover></g:math> flux temporal variation is significantly smaller than those of <k:math xmlns:k="http://www.w3.org/1998/Math/MathML" display="inline"><k:mi>p</k:mi></k:math>, <m:math xmlns:m="http://www.w3.org/1998/Math/MathML" display="inline"><m:msup><m:mi>e</m:mi><m:mo>−</m:mo></m:msup></m:math>, and <o:math xmlns:o="http://www.w3.org/1998/Math/MathML" display="inline"><o:msup><o:mi>e</o:mi><o:mo>+</o:mo></o:msup></o:math>. A hysteresis between the <q:math xmlns:q="http://www.w3.org/1998/Math/MathML" display="inline"><q:mover accent="true"><q:mi>p</q:mi><q:mo stretchy="false">¯</q:mo></q:mover></q:math> fluxes and the <u:math xmlns:u="http://www.w3.org/1998/Math/MathML" display="inline"><u:mi>p</u:mi></u:math> fluxes is observed, whereas the <w:math xmlns:w="http://www.w3.org/1998/Math/MathML" display="inline"><w:mover accent="true"><w:mi>p</w:mi><w:mo stretchy="false">¯</w:mo></w:mover></w:math> and <ab:math xmlns:ab="http://www.w3.org/1998/Math/MathML" display="inline"><ab:msup><ab:mi>e</ab:mi><ab:mo>−</ab:mo></ab:msup></ab:math> fluxes show a linear correlation. With a model-independent analysis, we found a universal relation between the shape of the rigidity spectrum and the magnitude of flux temporal variation over an 11-year Solar cycle for both positively and negatively charged particles. The simultaneous results on <cb:math xmlns:cb="http://www.w3.org/1998/Math/MathML" display="inline"><cb:mover accent="true"><cb:mi>p</cb:mi><cb:mo stretchy="false">¯</cb:mo></cb:mover></cb:math> and <gb:math xmlns:gb="http://www.w3.org/1998/Math/MathML" display="inline"><gb:mi>p</gb:mi></gb:math>, <ib:math xmlns:ib="http://www.w3.org/1998/Math/MathML" display="inline"><ib:msup><ib:mi>e</ib:mi><ib:mo>−</ib:mo></ib:msup></ib:math>, and <kb:math xmlns:kb="http://www.w3.org/1998/Math/MathML" display="inline"><kb:msup><kb:mi>e</kb:mi><kb:mo>+</kb:mo></kb:msup></kb:math> provide unique information for understanding particle transport in the Solar System as a function of mass, charge, and spectral shape.
