Additionally, for the first time, the temporal variations in the helium and electron intensities during a Forbush decrease were studied. The daily averaged GCR proton intensity was used to investigate the rigidity dependence of the amplitude and the recovery time of the Forbush decrease. For the first time, thanks to the unique features of the PAMELA magnetic spectrometer, the Forbush decrease, commencing on 2006 December 14 and following a CME at the Sun on 2006 December 13, was studied in a wide rigidity range (0.4–20 GV) and for different species of GCRs detected directly in space. These techniques allow only the indirect detection of the overall GCR intensity over an integrated energy range. Most of the past measurements of this phenomenon were carried out with ground-based detectors such as neutron monitors or muon telescopes. Forbush decreases are sudden suppressions of the GCR intensities, which are associated with the passage of interplanetary transients such as shocks and interplanetary coronal mass ejections (ICMEs). New results on the short-term galactic cosmic-ray (GCR) intensity variation (Forbish decrease) in 2006 December measured by the PAMELA instrument are presented. A related observable based on the third-order harmonic flow is proposed to further investigate such background effects in charge-dependent correlations.Įvidence of Energy and Charge Sign Dependence of the Recovery Time for the 2006 December Forbush Event Measured by the PAMELA Experiment The results of a (3 + 1)-dimensional hydrodynamic model show that the preliminary experimental data of the STAR Collaboration can be explained as due to background effects, such as resonance decays and local charge conservation in the particle production. Recently, a sensitive observable comparing event-by-event distributions of the charge splitting projected on the directions along and perpendicular to the direction of the elliptic flow has been proposed. The experimental search for the chiral magnetic effect in heavy-ion collisions is based on charge-dependent correlations between emitted particles. Similarly, we show that in a>c theories, the logarithmic negativity does not always exceed the entanglement entropy.Īzimuthal angle dependence of the charge imbalance from charge conservation effects The negative contribution is proportional to the product of a-c and the genus of the surface. The PAMELA space experiment, in orbit since 2006, has measured cosmic rays (CRs) through the most recent period of minimum solar activity with the magnetic field polarity as A  c, the entanglement across certain classes of entangling surfaces can become arbitrarily negative, depending on the geometry and topology of the surface. NEW EVIDENCE FOR CHARGE-SIGN-DEPENDENT MODULATION DURING THE SOLAR MINIMUM OF 2006 TO 2009 Analytic formulas are given for all C and all L point sign inversions.
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In all cases, the sign of the charge seen by an observer can change as she changes the direction from which she views the singularity. We describe observer- dependent sign inversions of the topological charges of vector field polarization singularities: C points (points of circular polarization), L points (points of linear polarization), and two virtually unknown singularities we call γ(C) and α(L) points. Observer- dependent sign inversions of polarization singularities. We present some examples for proton, antiproton and positron fluxes in the light of the recent PAMELA and AMS-02 data.
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SOLARPROP is able to use the output of popular tools like GALPROP or DRAGON and offers the possibility to embed new models for solar modulation. We present SOLARPROP, a tool to compute the influence of charge-sign dependent solar modulation for cosmic ray spectra. SOLARPROP: Charge-sign dependent solar modulation for everyone