THREE-DIMENSIONAL FEATURES OF THE OUTER HELIOSPHERE DUE TO COUPLING BETWEEN THE INTERSTELLAR AND INTERPLANETARY MAGNETIC FIELDS. IV. SOLAR CYCLE MODEL BASED ON<i>ULYSSES</i>OBSERVATIONS

Pogorelov, N. V.; Suess, S. T.; Borovikov, S. N.; Ebert, R. W.; McComas, D. J.; Zank, G. P.

doi:10.1088/0004-637x/772/1/2

Cited by 108 publications

(94 citation statements)

References 86 publications

Supporting

Mentioning

Contrasting

Unclassified

Order By: Relevance

“…With time-dependent boundary conditions derived from Ulysses data, Pogorelov et al (2013) analyzed the solar-cycle (SC) influence on the three-dimensional (3-D) structure of the outer heliosphere.…”

Section: Modelmentioning

confidence: 99%

See 1 more Smart Citation

Modeling the Solar Wind at the Ulysses, Voyager, and New Horizons Spacecraft

Kim

Pogorelov

Zank

et al. 2016

ApJ

Self Cite

View full text Add to dashboard Cite

The outer heliosphere is a dynamic region shaped largely by the interaction between the solar wind and the interstellar medium. While interplanetary magnetic field and plasma observations by the Voyager spacecraft have significantly improved our understanding of this vast region, modeling the outer heliosphere still remains a challenge. We simulate the three-dimensional, time-dependent solar wind flow from 1 to 80 astronomical units (AU), where the solar wind is assumed to be supersonic, using a two-fluid model in which protons and interstellar neutral hydrogen atoms are treated as separate fluids. We use 1-day averages of the solar wind parameters from the OMNI data set as inner boundary conditions to reproduce time-dependent effects in a simplified manner which involves interpolation in both space and time. Our model generally agrees with Ulysses data in the inner heliosphere and Voyager data in the outer heliosphere. Ultimately, we present the model solar wind parameters extracted along the trajectory of New Horizons spacecraft. We compare our results with in situ plasma data taken between 11 and 33 AU and at the closest approach to Pluto on July 14, 2015.

show abstract

Section: Modelmentioning

confidence: 99%

“…At the inner boundary, the solar wind velocity changes from 800 km s −1 at the center (poles) to ∼700 km s −1 at the edges of PCHs. Empirical correlations from Ulysses data are used to estimate the PCH density and temperature as a function of solar wind radial velocity (Ebert et al 2009;Pogorelov et al 2013) using the following formulae:…”

Section: Modelmentioning

confidence: 99%

Modeling the Solar Wind at the Ulysses, Voyager, and New Horizons Spacecraft

Kim

Pogorelov

Zank

et al. 2016

ApJ

Self Cite

View full text Add to dashboard Cite

show abstract

“…The passage of the supersonic solar wind to the subsonic heliosheath by means of a TS was modeled by Borovikov et al (2011). A variety of models (e.g., Pogorelov et al 2009Pogorelov et al , 2012Pogorelov et al , 2013Opher et al 2011Opher et al , 2012Opher & Drake 2013;Washimi et al 2011;Borovikov et al 2012;Fisk & Gloeckler 2013) describe the structure and dynamics in the heliosheath. Recent models by Provornikova et al (2013Provornikova et al ( , 2014 and by Michael et al (2015) predict the observed B and radial speeds at V1 and V2.…”

Section: Structure and Formation Of The Interaction Regionmentioning

confidence: 99%

Heliosheath Magnetic Field and Plasma Observed by Voyager 2 During 2012 in the Rising Phase of Solar Cycle 24

Burlaga

Ness

Richardson

et al. 2016

ApJ

View full text Add to dashboard Cite

We discuss magnetic field and plasma observations of the heliosheath made by Voyager 2 (V2) during 2012, when V2 was observing the effects of increasing solar activity following the solar minimum in 2009. The average magnetic field strength B was 0.14 nT and B reached 0.29 nT on day 249. V2 was in a unipolar region in which the magnetic polarity was directed away from the Sun along the Parker spiral 88% of the time, indicating that V2 was poleward of the heliospheric current sheet throughout most of 2012. The magnetic flux at V2 during 2012 was constant. A merged interaction region (MIR) was observed, and the flow speed increased as the MIR moved past V2. The MIR caused a decrease in the >70 MeV nuc −1 cosmic-ray intensity. The increments of B can be described by a q-Gaussian distribution with q=1.2±0.1 for daily averages and q=1.82±0.03 for hour averages. Eight isolated current sheets ("PBLs") and four closely spaced pairs of current sheets were observed. The average change of B across the current sheets was a factor of ≈2, and B increased or decreased with equal probability. Magnetic holes and magnetic humps were also observed. The characteristic size of the PBLs was ≈6 R L , where R L is the Larmor radius of protons, and the characteristic sizes of the magnetic holes and humps were ≈38 R L and ≈11 R L , respectively.

show abstract

“…Such processes create instabilities on the heliopause in the upstream direction, that propagate along the flanks and that can reach spatial scales of 10-100 AU (Borovikov, 2008). Another source of instabilities on the heliopause is the solar cycles affecting the heliospheric magnetic field pressure that determines the location of the heliopause (Pogorelov et al, 2013). The magnetic field polarity inversions due to solar cycles, also produce unipolar regions of magnetic fields that, dragged by the solar wind, drift along the heliotail ).…”

Section: The Heliospherementioning

confidence: 99%

TeV Cosmic Ray Anisotropy and the Heliospheric Magnetic Field

Desiati

Lazarían

2014

ASTRA Proc.

View full text Add to dashboard Cite

Abstract. Cosmic rays are observed to possess a small non uniform distribution in arrival direction. Such anisotropy appears to have a roughly consistent topology between tens of GeV and hundreds of TeV, with a smooth energy dependency on phase and amplitude. Above a few hundreds of TeV a sudden change in the topology of the anisotropy is observed. The distribution of cosmic ray sources in the Milky Way is expected to inject anisotropy on the cosmic ray flux. The nearest and most recent sources, in particular, are expected to contribute more significantly than others. Moreover the interstellar medium is expected to have different characteristics throughout the Galaxy, with different turbulent properties and injection scales. Propagation effects in the interstellar magnetic field can shape the cosmic ray particle distribution as well. In particular, in the 1-10 TeV energy range, they have a gyroradius comparable to the size of the Heliosphere, assuming a typical interstellar magnetic field strength of 3 µG. Therefore they are expected to be strongly affected by the Heliosphere in a manner ordered by the direction of the local interstellar magnetic field and of the heliotail. In this paper we discuss on the possibility that TeV cosmic rays arrival distribution might be significantly redistributed as they propagate through the Heliosphere.

show abstract

THREE-DIMENSIONAL FEATURES OF THE OUTER HELIOSPHERE DUE TO COUPLING BETWEEN THE INTERSTELLAR AND INTERPLANETARY MAGNETIC FIELDS. IV. SOLAR CYCLE MODEL BASED ONULYSSESOBSERVATIONS

Cited by 108 publications

References 86 publications

Modeling the Solar Wind at the Ulysses, Voyager, and New Horizons Spacecraft

Modeling the Solar Wind at the Ulysses, Voyager, and New Horizons Spacecraft

Heliosheath Magnetic Field and Plasma Observed by Voyager 2 During 2012 in the Rising Phase of Solar Cycle 24

TeV Cosmic Ray Anisotropy and the Heliospheric Magnetic Field

Contact Info

Product

Resources

About