Modeling Drift Along the Heliospheric Wavy Neutral Sheet

Burger, R. A.

doi:10.1088/0004-637x/760/1/60

Cited by 33 publications

(22 citation statements)

References 25 publications

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“…PROPAGATION IN THE GALAXY The GALPROP model for CR propagation is being continuously developed in order to provide a framework for theoretical studies of CR propagation in the Galaxy and interpretation of relevant observations (for more details see , 2000, Moskalenko et al 2002, 2003, Ptuskin et al 2006, Strong et al 2007, Trotta et al 2011, Vladimirov et al 2011, 2012, Jóhannesson et al 2016. GALPROP numerically solves the system of time-dependent partial differential equations describing the particle transport with a given source distribution and boundary conditions for all CR species.…”

Section: Galprop Model For Cr Production Andmentioning

confidence: 99%

“…With the development of sophisticated Galactic propagation models, the force-field approximation became the Achilles' hill of CR astrophysics. More advanced mod-els did exist -including those accounting for the so-called "charge drift effect" (e.g., Jokipii et al 1977;Burger 2012), whose experimental evidence was provided, for instance, by Garcia-Munoz et al (1986) and Boella et al (2001), -but they were not as "user friendly" and their wide practical application was suppressed by the high "threshold" demand of an expertise in the heliospheric physics.…”

mentioning

confidence: 99%

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Solution of Heliospheric Propagation: Unveiling the Local Interstellar Spectra of Cosmic-ray Species

Boschini

Torre

Gervasi

et al. 2017

ApJ

149

181

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Local interstellar spectra (LIS) for protons, helium and antiprotons are built using the most recent experimental results combined with the state-of-the-art models for propagation in the Galaxy and heliosphere. Two propagation packages, GALPROP and HelMod, are combined to provide a single framework that is run to reproduce direct measurements of cosmic ray (CR) species at different modulation levels and at both polarities of the solar magnetic field. To do so in a self-consistent way, an iterative procedure was developed, where the GALPROP LIS output is fed into HelMod that provides modulated spectra for specific time periods of selected experiments to compare with the data; the HelMod parameters optimization is performed at this stage and looped back to adjust the LIS using the new GALPROP run. The parameters were tuned with the maximum likelihood procedure using an extensive data set of proton spectra from 1997-2015. The proposed LIS accommodate both the low energy interstellar CR spectra measured by Voyager 1 and the high energy observations by BESS, Pamela, AMS-01, and AMS-02 made from the balloons and near-Earth payloads; it also accounts for Ulysses counting rate features measured out of the ecliptic plane. The found solution is in a good agreement with proton, helium, and antiproton data by AMS-02, BESS, and PAMELA in the whole energy range.

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Section: Galprop Model For Cr Production Andmentioning

confidence: 99%

mentioning

confidence: 99%

Solution of Heliospheric Propagation: Unveiling the Local Interstellar Spectra of Cosmic-ray Species

Boschini

Torre

Gervasi

et al. 2017

ApJ

149

181

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“…This electric field causes particles to experienceÉ B drift, analogous with corotation of field lines. In the case of a wavy HCS (see, e.g., Burger 2012;Pei et al 2012;Strauss et al 2012), especially with greater heliocentric distance, an assumed radial solar wind flow will no longer be wholly in the current sheet plane, requiring more detailed analysis of possible reconnection. Observations estimate the HCS thickness to be in the region of between 5000 and 40,000 km at 1 au (see, e.g., Winterhalter et al 1994;Eastwood et al 2002).…”

Section: Hcs Modelmentioning

confidence: 99%

Solar Energetic Particle Transport Near a Heliospheric Current Sheet

Battarbee

Dalla

Marsh

2017

ApJ

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Solar energetic particles (SEPs), a major component of space weather, propagate through the interplanetary medium strongly guided by the interplanetary magnetic field (IMF). In this work, we analyze the implications that a flat Heliospheric Current Sheet (HCS) has on proton propagation from SEP release sites to the Earth. We simulate proton propagation by integrating fully 3D trajectories near an analytically defined flat current sheet, collecting comprehensive statistics into histograms, fluence maps, and virtual observer time profiles within an energy range of 1-800 MeV. We show that protons experience significant current sheet drift to distant longitudes, causing time profiles to exhibit multiple components, which are a potential source of confusing interpretations of observations. We find that variation of the current sheet thickness within a realistic parameter range has little effect on particle propagation. We show that the IMF configuration strongly affects the deceleration of protons. We show that in our model, the presence of a flat equatorial HCS in the inner heliosphere limits the crossing of protons into the opposite hemisphere.

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“…Version "Strauss2" (st2) is essentially the same, but uses the angles defined by Burger (2012) and takes into account the r-dependency of the solar wind (see,e.g., Raath 2015). The second possibility is to smooth out the HCS (Burger 2012) and to compute the drift contributions analytically as given in Equation (13) of Burger (2012). Version "Burger1" (bg1) omits the last contribution of this equation, while "Burger2" (bg2) uses the full equation.…”

Section: The Transport Coefficientsmentioning

confidence: 99%

Cosmic-Ray Transport in Heliospheric Magnetic Structures. II. Modeling Particle Transport through Corotating Interaction Regions

Kopp

Wiengarten

Fichtner

et al. 2017

ApJ

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The transport of cosmic rays (CRs) in the heliosphere is determined by the properties of the solar wind plasma. The heliospheric plasma environment has been probed by spacecraft for decades and provides a unique opportunity for testing transport theories. Of particular interest for the three-dimensional (3D) heliospheric CR transport are structures such as corotating interaction regions (CIRs), which, due to the enhancement of the magnetic field strength and magnetic fluctuations within and due to the associated shocks as well as stream interfaces, do influence the CR diffusion and drift. In a three-fold series of papers, we investigate these effects by modeling innerheliospheric solar wind conditions with the numerical magnetohydrodynamic (MHD) framework CRONOS (Wiengarten et al., referred as Paper I), andthe results serve as input to a transport code employing a stochastic differential equation approach (this paper). While, in Paper I, we presented results from 3D simulations with CRONOS, the MHD output is now taken as an input to the CR transport modeling. We discuss the diffusion and drift behavior of Galactic cosmic rays using the example of different theories, andstudy the effects of CIRs on these transport processes. In particular, we point out the wide range of possible particle fluxes at a given point in space resulting from these different theories. The restriction of this variety by fitting the numerical results to spacecraft data will be the subject of the third paper of this series.

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Modeling Drift Along the Heliospheric Wavy Neutral Sheet

Cited by 33 publications

References 25 publications

Solution of Heliospheric Propagation: Unveiling the Local Interstellar Spectra of Cosmic-ray Species

Solution of Heliospheric Propagation: Unveiling the Local Interstellar Spectra of Cosmic-ray Species

Solar Energetic Particle Transport Near a Heliospheric Current Sheet

Cosmic-Ray Transport in Heliospheric Magnetic Structures. II. Modeling Particle Transport through Corotating Interaction Regions

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