A New Model of the Galactic Magnetic Field

Jansson, Ronnie; Farrar, Glennys R.

doi:10.1088/0004-637x/757/1/14

Cited by 652 publications

(913 citation statements)

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“…Reviewing all of them is a daunting task, so I will very partially choose to describe in some detail only the two latest largescale models of [1] and [2], and mention this year's small-scale effort appeared in [3]; for many more details, a beautiful and very recent review on the GMF is [7].…”

Section: Models Of the Galactic Magnetic Fieldmentioning

confidence: 99%

“…2. The large-scale GMF JF12 model as in [2]. The left panel shows the disk field (top) and halo field (bottom) as they appear at ±10 pc and ±1 kpc, respectively; the right panel depicts the "X-field" strength.…”

Section: Regular Gmf Modelsmentioning

confidence: 99%

“…At this point there are two options: either α and β are both small, or they are not. In the first case, we can kill them from (2), so that the ( δB) 2 is now in common between (2) and (3), and can be simplified as…”

Section: A Gmf Non-modelmentioning

confidence: 99%

“…2.1 succintly review the features of the two largescale GMF models en vogue in 2014, which first appeared in [1] (PTKN11) and in [2] (JF12), and, in sec. 2.2, the small-scale latest model of [3]; to close sec.…”

Section: Introductionmentioning

confidence: 99%

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The Galactic Magnetic Field and Ultra-High Energy Cosmic Rays

Urban¹

2016

Proceedings of International Symposium for Ultra-High Energy Cosmic Rays (UHECR2014)

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The Galactic Magnetic Field is a peeving and importune screen between Ultra-High Energy Cosmic Rays and us cosmologists, engaged in the combat to unveil their properties and origin, as it deviates their paths towards the Earth in unpredictable ways. I will, in this order: briefly review the available field models on the market; explain a little trick which allows one to obtain cosmic rays deflection variances without even knowing what the (random) GMF model is; and argue that there is a lack of anisotropy in the large scales cosmic rays signal, which the Galactic field can do nothing about.

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Section: Models Of the Galactic Magnetic Fieldmentioning

confidence: 99%

Section: Regular Gmf Modelsmentioning

confidence: 99%

Section: A Gmf Non-modelmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

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The Galactic Magnetic Field and Ultra-High Energy Cosmic Rays

Urban¹

2016

Proceedings of International Symposium for Ultra-High Energy Cosmic Rays (UHECR2014)

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“…The Galactic field contains both a regular and a turbulent component. The regular Galactic field can be inferred from Faraday rotation measures [5] in combination with synchrotron polarization measurements [6]. The uncertainties are still significant; typical deflections of a proton of energy E = 100 EeV are 1 • − 6 • depending on the direction, with the median value ∼ 3 • in both models cited above.…”

Section: Introductionmentioning

confidence: 99%

TA Anisotropy Summary

Tinyakov

2018

Proceedings of 2016 International Conference on Ultra-High Energy Cosmic Rays (UHECR2016)

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We analyze the ultra-high energy cosmic ray (UHECR) events collected by the surface detector of the Telescope Array (TA) during 7 years of operation for the presence of anisotropy at small and large angular scales. To minimize the number of trials, we consider three a priori chosen energy thresholds: 10 EeV, 40 EeV and 57 EeV. The two lower-energy sets show no deviation from isotropy neither at small nor at large scales. In the high-energy set E > 57 EeV there is a localized excess, the "hot spot" of the radius ∼ 20 • in the direction R.A. = 148.4 • , Dec. = 44.5 • (equatorial coordinates), reported previously in [1] on the basis of the 5yr of TA data. We present an update of this analysis with 2 additional years of data. We also examine spectral differences between different regions of the sky and, in particular, between the hot spot region and the rest of the sky.

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Probing the universe at the highest energies with the Pierre Auger Observatory

Vícha

2019

Astron Nachr

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The Pierre Auger Observatory is currently the largest detector of cosmic rays of ultrahigh energies (from ∼10 17 to ∼10 20 eV). The size of its accumulated exposure and the hybrid concept of the detector have provided measurements of unprecedented precision on the cosmic ray energy spectrum, mass composition, and anisotropy searches. There is an ankle in the energy spectrum at ∼4 EeV and a steepening at the end of the energy spectrum (above ∼40 EeV). The mass composition around the ankle is mixed and is uncertain at the highest energies due to the lack of statistics and high systematic uncertainties coming from predictions of different models of hadronic interactions. These models have, moreover, serious problems in describing the muon component of air showers. Still, the mean mass number of cosmic rays reaches its lowest value at energy ∼2 EeV and increases gradually above this energy. A dipole in the arrival directions is observed for energies above 8 EeV at more than 5 significance level. It points ∼125 • from the Galactic center, indicating the extra-Galactic origin of these cosmic rays. The correlation of the arrival directions with starburst galaxies disfavors the isotropy hypothesis at energies above ∼40 EeV at the 4 level without penalization for the catalog scan. The Observatory is currently being upgraded to improve its sensitivity to the mass of cosmic rays at the highest energies, which is crucial to constrain their sources. KEYWORDS arrival directions -cosmic rays -extensive air shower -mass composition -models of hadronic interactions 1 PIERRE AUGER OBSERVATORY The Pierre Auger Observatory (PAO; Aab et al. 2015b) is a cosmic ray experiment located in the Argentinian Pampa covering the latitudes 35.0 • S and 35.3 • S and longitudes 69.0 • W and 69.4 • W at around 1,400 m a.s.l. It detects extensive air showers of secondary particles initiated by primary particles of energies above ∼10 18 eV. Two detection techniques are combined and form a hybrid cosmic ray detector. During the propagation of the secondary particles, an isotropic emission of faint fluorescent light (350-400 nm) is produced and collected in fluorescence telescopes with a mirror area of 13 m 2 . These 24 telescopes, making up the fluorescence detector (FD) with a duty cycle ∼13% are built at four sites surrounding the array of ∼1,600 surface detectors. This array forms the surface detector (SD) with a duty cycle of ∼100%,covering an area of ∼3,000 km 2 in total. The SDs collect the Cherenkov light induced by charged particles passing through the water medium (12 m 3 ) inside these detectors spaced in the regular triangular grid of 1,500 m spacing. An illustration of detection of air shower by SD and FD at the PAO is shown in Figure 1. The Observatory has been collecting scientific data since 2004, and the main detector was completed in 2008, providing measurements of unprecedented precision and statistics. Further, low-energy extensions (down to 10 17 eV) have been installed at the Observatory. Three high-elevation telescopes were inst...

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A New Model of the Galactic Magnetic Field

Cited by 652 publications

References 48 publications

The Galactic Magnetic Field and Ultra-High Energy Cosmic Rays

The Galactic Magnetic Field and Ultra-High Energy Cosmic Rays

TA Anisotropy Summary

Probing the universe at the highest energies with the Pierre Auger Observatory

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