Galactic and heliotail‐in anisotropies of cosmic rays as the origin of sidereal daily variation in the energy region &lt; 10<sup>4</sup> GeV

Nagashima, K.; Fujimoto, K.; Jacklyn, R. M.

doi:10.1029/98ja01105

Cited by 94 publications

(100 citation statements)

References 21 publications

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“…Large-scale anisotropies and smaller scale excess regions have been detected in the distribution of CRs in this energy range (Nagashima et al 1998;Hall et al 1999;Abdo et al 2008;Abbasi et al 2011;Surdo & Argo-Ybj Collaboration 2011). It has been suggested that the Sun is located in a magnetic flux tube in the ISM, and that such a structure would be a conduit for GCRs (Frisch 1997).…”

Section: Galactic Cosmic Rays and The Local Ismfmentioning

confidence: 99%

“…The blue open circle gives the ISMF direction derived from the center of the IBEX Ribbon arc. The large blue circular region (light gray) shows the location of the tail-in anisotropy for ∼500 GeV GCRs modeled by Hall et al (1999), with the extent defined by the 68 • width from Nagashima et al (1998). The regions outlined by thick black lines show the observed heliotail that is deflected ∼44 • to the west of the downwind gas direction (red triangle) and is prominent in maps of the globally distributed ENAs (Schwadron et al 2011).…”

Section: Cmb Dipole Anisotropy and The Local Ismfmentioning

confidence: 99%

“…Using cosmic-ray fluxes in the northern and southern hemispheres, Nagashima et al (1998) described two anisotropies in terms of a broad sidereal galactic anisotropy and a narrow anisotropy, the "tail-in" anisotropy, described by a maximum toward the anti-apex direction of the solar motion. 20 The galactic anisotropy arrives from the direction α, δ = 0 H , −20 • ( , b ∼ 61 • , −76 • ).…”

Section: Galactic Cosmic Rays and The Local Ismfmentioning

confidence: 99%

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The Interstellar Magnetic Field Close to the Sun. Ii.

Frisch

Andersson

Berdyugin

et al. 2012

ApJ

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The magnetic field in the local interstellar medium (ISM) provides a key indicator of the galactic environment of the Sun and influences the shape of the heliosphere. We have studied the interstellar magnetic field (ISMF) in the solar vicinity using polarized starlight for stars within 40 pc of the Sun and 90 • of the heliosphere nose. In Frisch et al. (Paper I), we developed a method for determining the local ISMF direction by finding the best match to a group of interstellar polarization position angles obtained toward nearby stars, based on the assumption that the polarization is parallel to the ISMF. In this paper, we extend the analysis by utilizing weighted fits to the position angles and by including new observations acquired for this study. We find that the local ISMF is pointed toward the • 25 pc −1 . This conclusion is conditioned on the small sample of stars available for defining this rotation. Variations from the ordered component suggest a turbulent component of ∼23 • . The ordered component and standard relations between polarization, color excess, and H o column density predict a reasonable increase of N(H) with distance in the local ISM. The similarity of the ISMF directions traced by the polarizations, the IBEX Ribbon, and pulsars inside the Local Bubble in the third galactic quadrant suggest that the ISMF is relatively uniform over spatial scales of 8-200 pc and is more similar to interarm than spiral-arm magnetic fields. The ISMF direction from the polarization data is also consistent with small-scale spatial asymmetries detected in GeV-TeV cosmic rays with a galactic origin. The peculiar geometrical relation found earlier between the cosmic microwave background dipole moment, the heliosphere nose, and the ISMF direction is supported by this study. The interstellar radiation field at ∼975 Å does not appear to play a role in grain alignment for the low-density ISM studied here.

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Section: Galactic Cosmic Rays and The Local Ismfmentioning

confidence: 99%

Section: Cmb Dipole Anisotropy and The Local Ismfmentioning

confidence: 99%

Section: Galactic Cosmic Rays and The Local Ismfmentioning

confidence: 99%

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The Interstellar Magnetic Field Close to the Sun. Ii.

Frisch

Andersson

Berdyugin

et al. 2012

ApJ

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“…Contrary to this expectation, the C-G effect could not be observed ( Nagashima et al, 1998). The non-existence of the effect is of importance with regard to the interaction between the HMS and the interstellar gaseous matter (IGM), as will be discussed in the next section.…”

Section: Direction Of Nose Head Of the Hms In Spacementioning

confidence: 47%

“…3). Nagashima et al (1998) were indicating that at energies less than 10 4 GeV the amplitude of TA was decreasing with increasing energy, giving strength to the conclusion that TA was of solar origin. Remarkably, since that time it has been reported from a number of advanced experiments that TA continues to exist at energies in the multi-TeV region, raising new questions regarding the evidence for the solar origin of TA.…”

Section: Ga and Ta Of Three Kinds Of Sidereal Anisotropy In The Hmsmentioning

confidence: 88%

The existence of cosmic ray sidereal anisotropies of galactic and solar origins with energies lower than 104 GeV and their modulation caused by the presumed behavior pattern of the heliomagnetosphere and of its neighboring gaseous matter in interstellar magnetic field

et al. 2012

Self Cite

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It is shown that the sidereal anisotropy (S i A) of cosmic rays (CRs) with energies smaller than 10 4 GeV consists of three kinds: one (GA) is of galactic origin from the direction G (α G = 0 hr; δ G = −20• ), and the other two (tail-in TA and nose-in HA) are of solar origin from the respective directions T (α T = 6 hr; δ T ∼ −24• ) and H (α H = 18 hr; δ H > 0• ) and supposed to be produced by the acceleration of CRs on the tail and nose boundaries of the heliomagnetosphere (HMS). This conclusion was arrived at in 1995 after a long-term delay since the beginning of CR observations in the early 20-th century. This delay was mainly due to the inconsistency among observations caused by the belief that the sidereal anisotropy must be unidirectional in space. The inconsistency has been solved at least qualitatively by the discovery of GA and TA. These anisotropies, including also HA, are subject, respectively, to their proper solar modulations in the HMS characterized by a polarity reversal every 11 years of the solar polar magnetic field and solar activity dependence with an 11-year periodicity. By using these modulation patterns, the origins of the three anisotropies have been determined. TA and HA thus determined inversely produce the following kinds of evidence and problems in the HMS: (1) the structure of the HMS, (2) acceleration of CRs on the boundary of the HMS, (3) CR Lens Effect of the HMS for the sharp concentration of TA and HA, (4) the proper motion (V HMS ) of the HMS relative to neighboring stars, (5) the proper motion of interstellar gaseous matter (including the magnetic field) relative to neighboring stars, and (6) the existence of the Subordinate HMS surrounding the HMS for the explanation of the duality of the motion of the HMS and also of the absence of the Compton-Getting (C-G) effect on the HMS. The present paper not only presents a brief summary of the studies of CR sidereal anisotropy made by many researchers during the 20th century leading to the present understanding, but also presents some problems to open up a new vista of the future.

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Turbulence, Magnetic Reconnection in Turbulent Fluids and Energetic Particle Acceleration

Lazarían¹,

Vlahos²,

Kowal³

et al. 2012

Particle Acceleration in Cosmic Plasmas

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Turbulence is ubiquitous in astrophysics. It radically changes many astrophysical phenomena, in particular, the propagation and acceleration of cosmic rays. We present the modern understanding of compressible magnetohydrodynamic (MHD) turbulence, in particular its decomposition into Alfvén, slow and fast modes, discuss the density structure of turbulent subsonic and supersonic media, as well as other relevant regimes of astrophysical turbulence. All this information is essential for understanding the energetic par-A. Lazarian

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Galactic and heliotail‐in anisotropies of cosmic rays as the origin of sidereal daily variation in the energy region < 10⁴ GeV

Cited by 94 publications

References 21 publications

The Interstellar Magnetic Field Close to the Sun. Ii.

The Interstellar Magnetic Field Close to the Sun. Ii.

The existence of cosmic ray sidereal anisotropies of galactic and solar origins with energies lower than 104 GeV and their modulation caused by the presumed behavior pattern of the heliomagnetosphere and of its neighboring gaseous matter in interstellar magnetic field

Turbulence, Magnetic Reconnection in Turbulent Fluids and Energetic Particle Acceleration

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Galactic and heliotail‐in anisotropies of cosmic rays as the origin of sidereal daily variation in the energy region < 104 GeV

Cited by 94 publications

References 21 publications

The Interstellar Magnetic Field Close to the Sun. Ii.

The Interstellar Magnetic Field Close to the Sun. Ii.

The existence of cosmic ray sidereal anisotropies of galactic and solar origins with energies lower than 104 GeV and their modulation caused by the presumed behavior pattern of the heliomagnetosphere and of its neighboring gaseous matter in interstellar magnetic field

Turbulence, Magnetic Reconnection in Turbulent Fluids and Energetic Particle Acceleration

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Galactic and heliotail‐in anisotropies of cosmic rays as the origin of sidereal daily variation in the energy region < 10⁴ GeV