A predictive analytic model for the solar modulation of cosmic rays

Cholis, Ilias; Hooper, Dan; Linden, Tim

doi:10.1103/physrevd.93.043016

Cited by 107 publications

(141 citation statements)

References 64 publications

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“…During the completion of this work, we became aware of related studies by Ghelfi et al (2016) and by Cholis et al (2016). The data sets and methods used differ from those of our study, making the three analyses complementary.…”

Section: Discussionmentioning

confidence: 99%

Solar Modulation of the Local Interstellar Spectrum With Voyager 1, Ams-02, Pamela, and Bess

Corti

Bindi

Consolandi

et al. 2016

ApJ

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In recent years, the increasing precision of direct cosmic rays measurements opened the door to high-sensitivity indirect searches of dark matter and to more accurate predictions for radiation doses received by astronauts and electronics in space. The key ingredients in the study of these phenomena are the knowledge of the local interstellar spectrum (LIS) of galactic cosmic rays and the understanding of how the solar modulation affects the LIS inside the heliosphere. Voyager 1, AMS-02, PAMELA, and BESS measurements of proton and helium fluxes provide valuable information, allowing us to shed light on the shape of the LIS and the details of the solar modulation during solar cycles 22-24. A new parametrization of the LIS is presented, based on the latest data from Voyager 1 and AMS-02. Using the framework of the force-field approximation, the solar modulation parameter is extracted from the time-dependent fluxes measured by PAMELA and BESS. A modified version of the force-field approximation with a rigidity-dependent modulation parameter is introduced, yielding better fits than the forcefield approximation. The results are compared with the modulation parameter inferred by neutron monitors.

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Section: Discussionmentioning

confidence: 99%

Solar Modulation of the Local Interstellar Spectrum With Voyager 1, Ams-02, Pamela, and Bess

Corti

Bindi

Consolandi

et al. 2016

ApJ

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“…(ii) We employ high-energy losses by taking a conservative choice for magnetic fields, of B ⊙ ¼ 8.9 μG at the Sun. (iii) We take the largest value of the solar modulation potential, Φ ¼ 0.6 GV, measured for AMS during its data-taking period [95]. In Fig.…”

Section: B Quantifying "Conservative"mentioning

confidence: 99%

“…The largest measured value of the solar modulation potential during AMS's data taking period of Φ ¼ 0.6 GV is taken [95], and we employ the force-field approximation, which is valid for positron fluxes [95,96]. …”

Section: A Cosmic-ray Propagationmentioning

confidence: 99%

GeV-scale thermal WIMPs: Not even slightly ruled out

et al. 2018

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Weakly interacting massive particles (WIMPs) have long reigned as one of the leading classes of dark matter candidates. The observed dark matter abundance can be naturally obtained by freezeout of weakscale dark matter annihilations in the early Universe. This "thermal WIMP" scenario makes direct predictions for the total annihilation cross section that can be tested in present-day experiments. While the dark matter mass constraint can be as high as m χ ≳ 100 GeV for particular annihilation channels, the constraint on the total cross section has not been determined. We construct the first model-independent limit on the WIMP total annihilation cross section, showing that allowed combinations of the annihilationchannel branching ratios considerably weaken the sensitivity. For thermal WIMPs with s-wave 2 → 2 annihilation to visible final states, we find the dark matter mass is only known to be m χ ≳ 20 GeV. This is the strongest largely model-independent lower limit on the mass of thermal-relic WIMPs; together with the upper limit on the mass from the unitarity bound (m χ ≲ 100 TeV), it defines what we call the "WIMP window." To probe the remaining mass range, we outline ways forward.

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“…These differences will be displayed respectively as proton and electron time profiles, from 2006 to 2009, together with the e − /p ratio as a function of rigidity for the mentioned period. Evidently, with the observation of precise spectra for protons, electrons, positrons and even anti-protons, on an almost continuous time-scale, charge-sign dependent modulation, and other important 3D effects, should no longer be ignored when interpreting these data, so that surpassing the force-field model has become necessary; see also Maccione (2013); Cholis et al (2016).…”

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confidence: 99%

New Evidence for Charge-Sign-Dependent Modulation During the Solar Minimum of 2006 to 2009

Felice

Munini

Vos

et al. 2017

ApJ

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The PAMELA space experiment, in orbit since 2006, has measured cosmic rays through the most recent A < 0 solar minimum activity period. During this entire time, galactic electrons and protons have been detected down to 70 MV and 400 MV, respectively, and their differential intensity variation in time has been monitored with unprecedented accuracy. These observations are used to show how differently electrons and protons responded to the quiet modulation conditions that prevailed from 2006 to 2009. It is well known that particle drifts, as one of four major mechanisms for the solar modulation of cosmic rays, cause charge-sign dependent solar modulation. Solar minimum activity periods provide optimal conditions to study these drift effects. The observed behaviour is compared to the solutions of a three-dimensional model for cosmic rays in the heliosphere, including drifts. The numerical results confirm that the difference in the evolution of electron and proton spectra during the last prolonged solar minimum is attributed to a large extent to particle drifts. We therefore present new evidence of charge-sign dependent solar modulation, with perspective on its peculiarities for the observed period from 2006 to 2009.

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A predictive analytic model for the solar modulation of cosmic rays

Cited by 107 publications

References 64 publications

Solar Modulation of the Local Interstellar Spectrum With Voyager 1, Ams-02, Pamela, and Bess

Solar Modulation of the Local Interstellar Spectrum With Voyager 1, Ams-02, Pamela, and Bess

GeV-scale thermal WIMPs: Not even slightly ruled out

New Evidence for Charge-Sign-Dependent Modulation During the Solar Minimum of 2006 to 2009

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