Breaks in interstellar spectra of positrons and electrons derived from time-dependent AMS data

Vittino, Andrea; Mertsch, Philipp; Gast, H.; Schael, S.

doi:10.1103/physrevd.100.043007

Cited by 43 publications

(54 citation statements)

References 66 publications

Supporting

Mentioning

Contrasting

Order By: Relevance

“…Several theoretical studies have hinted at the possible presence of breaks at low- (Ptuskin et al 2006) or high-rigidity (Blasi et al 2012;Evoli et al 2018). Actually, spectral breaks are seen in CR data at low- (Stone et al 2013) and high-rigidity (Aguilar et al 2018), and they can be connected to the presence of breaks in the diffusion coefficient at rigidities R l ≈ 4−5 GV (Génolini et al 2019;Vittino et al 2019;Weinrich et al 2020) and R h ≈ 250 GV (Génolini et al 2017(Génolini et al , 2019Reinert & Winkler 2018;Evoli et al 2019). For these reasons we take…”

Section: Model and Configurations (Big Slim Quaint)mentioning

confidence: 99%

Galactic halo size in the light of recent AMS-02 data

Weinrich

Boudaud

Derome

et al. 2020

A&A

130

View full text Add to dashboard Cite

Context. The vertical diffusive halo size of the Galaxy, L, is a key parameter for dark matter indirect searches. It can be better determined thanks to recent AMS-02 data. Aims. We set constraints on L from Be/B and 10Be/Be data, and we performed a consistency check with positron data. We detail the dependence of Be/B and 10Be/Be on L and forecast on which energy range better data would be helpful for future L improvements. Methods. We used USINE V3.5 for the propagation of nuclei, and e+ were calculated with the pinching method. Results. The current AMS-02 Be/B (∼3% precision) and ACE-CRIS 10Be/Be (∼10% precision) data bring similar and consistent constraints on L. The AMS-02 Be/B data alone constrain L = 5−2+3 kpc at a 68% confidence level (spanning different benchmark transport configurations), a range for which most models do not overproduce positrons. Future experiments need to deliver percent-level accuracy on 10Be/9Be anywhere below 10 GV to further constrain L. Conclusions. Forthcoming AMS-02, HELIX, and PAMELA 10Be/9Be results will further test and possibly tighten the limits derived here. Elemental ratios involving radioactive species with different lifetimes (e.g. Al/Mg and Cl/Ar) are also awaited to provide complementary and robuster constraints.

show abstract

Section: Model and Configurations (Big Slim Quaint)mentioning

confidence: 99%

Galactic halo size in the light of recent AMS-02 data

Weinrich

Boudaud

Derome

et al. 2020

A&A

130

View full text Add to dashboard Cite

show abstract

“…The Voyager 1 spacecraft has left the region influenced by the Solar wind in 2012 and has since then measured electron energy distributions in the range 2.7-79 MeV in the local interstellar medium (Cummings et al 2016). Cosmic ray propagation models constrained by Voyager 1 and AMS data (Aguilar et al 2019) have been developed that infer the cosmic ray electron density distribution in the local interstellar medium, outside the Solar wind bubble for energies between 1 MeV and 1 TeV (Vittino et al 2019). The resulting distribution can be approximated by n(E) ∝ E −p , with p = 1.4 (3.1) below (above) 1 GeV.…”

Section: Constraints On the Particle Energy Spectrummentioning

confidence: 99%

“…In the following, we use the electron and positron energy spectra tabulated in Vittino et al (2019) as representative for the cosmic ray electron energy spectrum in the Local Bubble.…”

Section: O R I Gmentioning

confidence: 99%

Can the Local Bubble explain the radio background?

Krause

Hardcastle

2021

Monthly Notices of the Royal Astronomical Society

View full text Add to dashboard Cite

The ARCADE 2 balloon bolometer along with a number of other instruments have detected what appears to be a radio synchrotron background at frequencies below about 3 GHz. Neither extragalactic radio sources nor diffuse Galactic emission can currently account for this finding. We use the locally measured Cosmic ray electron population, demodulated for effects of the Solar wind, and other observational constraints combined with a turbulent magnetic field model to predict the radio synchrotron emission for the Local Bubble. We find that the spectral index of the modelled radio emission is roughly consistent with the radio background. Our model can approximately reproduce the observed antenna temperatures for a mean magnetic field strength B between 3-5 nT. We argue that this would not violate observational constraints from pulsar measurements. However, the curvature in the predicted spectrum would mean that other, so far unknown sources would have to contribute below 100 MHz. Also, the magnetic energy density would then dominate over thermal and cosmic ray electron energy density, likely causing an inverse magnetic cascade with large variations of the radio emission in different sky directions as well as high polarisation. We argue that this disagrees with several observations and thus that the magnetic field is probably much lower, quite possibly limited by equipartition with the energy density in relativistic or thermal particles (B = 0.2 − 0.6 nT). In the latter case, we predict a contribution of the Local Bubble to the unexplained radio background at most at the per cent level.

show abstract

“…In both cases the local interstellar spectrum is taken from Ref. [21]. The lower part of the plots shows the pull distribution for the fit.…”

Section: Application To Experimental Datamentioning

confidence: 99%

Solar modulation of cosmic rays in a semi-analytical framework

Kuhlen¹,

Mertsch²

2019

Proceedings of 36th International Cosmic Ray Conference — PoS(ICRC2019)

Self Cite

View full text Add to dashboard Cite

When Galactic cosmic rays enter the heliosphere they encounter the solar wind with its frozen-in magnetic field, which modulates the cosmic ray flux in the heliosphere up to rigidities as high as 40 GeV. In this work, we present a new and straightforward extension to the force-field model that takes into account charge sign dependent modulation due to drifts in the heliospheric magnetic field. We start by validating our semi-analytical approach via a comparison to a fully numerical model. Our model nicely reproduces the AMS-02 measurements and we find the strength of diffusion and drifts to be strongly correlated with the heliospheric tilt angle and magnitude of the magnetic field. We are able to predict the electron and positron fluxes beyond the range for which measurements by AMS-02 have been presented.

show abstract

Breaks in interstellar spectra of positrons and electrons derived from time-dependent AMS data

Cited by 43 publications

References 66 publications

Galactic halo size in the light of recent AMS-02 data

Galactic halo size in the light of recent AMS-02 data

Can the Local Bubble explain the radio background?

Solar modulation of cosmic rays in a semi-analytical framework

Contact Info

Product

Resources

About