Kinetic-Gasdynamic Modeling of the Heliospheric Interface

Izmodenov, Vladislav; Malama, Yu. G.; Chalov, S. V.; Alexashov, D. B.; Katushkina, Olga; Provornikova, Elena

doi:10.1007/978-1-4419-1448-4_14

Cited by 17 publications

(33 citation statements)

References 40 publications

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“…In Section 5 we will discuss separately constraining d TS and l IHS , but for this work, we adopt the values for the au in the direction of the south ecliptic pole. The derived north pole IHS thickness value of l IHS ∼210 au is within the range predicted by asymmetric heliosphere models, although there is considerable variation, from 100 au (Pogorelov et al 2013) to 240 au (Izmodenov et al 2009). The derived IHS thickness in the south is less than inthe north pole, presumably due to compression of the heliosheath along the southern leading edge by the interstellar magnetic field.…”

Section: Correlation Of 1 Au Dynamic Pressure With Ena-derived Plasmasupporting

confidence: 74%

“…Based on a survey of outer heliospheric models (e.g., Pogorelov et al 2007Pogorelov et al , 2013Izmodenov et al 2009;Opher et al 2009Opher et al , 2015, a proton outbound along the heliographic equator will travel roughly an additional 200 au through the IHS to the pole as compared to a proton traveling directly poleward. For a flow speed in the IHS of ∼150 km s −1 (based on Voyager 2 observations; Burlaga et al 2009), this corresponds to a travel time difference of ∼6.5 years, or more than half a solar cycle.…”

Section: Propagation Of Variations Along Streamlinesmentioning

confidence: 99%

“…The values for d TS can be reasonably estimated by considering the Voyager 1 and 2 TS crossing distances of 94 au and 84 au, respectively (Burlaga et al 2005;Stone et al 2008), and using the results of heliospheric models to scale these distances to the poles. Based on a survey of asymmetric heliosphere models (e.g., Pogorelov et al 2007Pogorelov et al , 2013Opher et al 2009Opher et al , 2015Izmodenov et al 2009 at the south pole. Then, the values for l IHS are varied until the best correlation between P 1au and P L s · is found.…”

Section: Trace-back Timementioning

confidence: 99%

See 2 more Smart Citations

Tracking the Solar Cycle Through Ibex Observations of Energetic Neutral Atom Flux Variations at the Heliospheric Poles

Reisenfeld

Bzowski

Funsten

et al. 2016

ApJ

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With seven years of Interstellar Boundary Explorer (IBEX) observations, from 2009 to 2015, we can now trace the time evolution of heliospheric energetic neutral atoms (ENAs) through over half a solar cycle. At the north and south ecliptic poles, the spacecraft attitude allows for continuous coverage of the ENA flux; thus, signal from these regions has much higher statistical accuracy and time resolution than anywhere else in the sky. By comparing the solar wind dynamic pressure measured at 1 au with the heliosheath plasma pressure derived from the observed ENA fluxes, we show that the heliosheath pressure measured at the poles correlates well with the solar cycle. The analysis requires time-shifting the ENA measurements to account for the travel time out and back from the heliosheath, which allows us to estimate the scale size of the heliosphere in the polar directions. We arrive at an estimated distance to the center of the ENA source region in the north of 220 auand in the southa distance of 190 au. We also find a good correlation between the solar cycle and the ENA energy spectra at the poles. In particular, the ENA flux for the highest IBEX energy channel (4.3 keV) is quite closely correlated with the areas of the polar coronal holes, in both the north and south, consistent with the notion that polar ENAs at this energy originate from pickup ions of the very high speed wind (∼700 km s −1 ) that emanates from polar coronal holes.

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Section: Correlation Of 1 Au Dynamic Pressure With Ena-derived Plasmasupporting

confidence: 74%

Section: Propagation Of Variations Along Streamlinesmentioning

confidence: 99%

Section: Trace-back Timementioning

confidence: 99%

See 1 more Smart Citation

Tracking the Solar Cycle Through Ibex Observations of Energetic Neutral Atom Flux Variations at the Heliospheric Poles

Reisenfeld

Bzowski

Funsten

et al. 2016

ApJ

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“…The inclusion of the neutral H atoms tend to symmetrize the solution and quantitatively affect the degree of asymmetry as seen recently by Pogorelov et al (2008aPogorelov et al ( , 2008b) (see also Izmodenov et al 2005b). The asymmetry in respect to the TS distances are recovered when more intense interstellar magnetic field is included (∼4-5 µG) Izmodenov et al 2008b).…”

Section: Discussionmentioning

confidence: 87%

Confronting Observations and Modeling: The Role of the Interstellar Magnetic Field in Voyager 1 and 2 Asymmetries

et al. 2008

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Magnetic effects are ubiquitous and known to be crucial in space physics and astrophysical media. We have now the opportunity to probe these effects in the outer heliosphere with the two spacecraft Voyager 1 and 2. Voyager 1 crossed, in December 2004, the termination shock and is now in the heliosheath. On August 30, 2007 Voyager 2 crossed the termination shock, providing us for the first time in-situ measurements of the subsonic solar wind in the heliosheath. With the recent in-situ data from Voyager 1 and 2 the numerical models are forced to confront their models with observational data. Our recent results indicate that magnetic effects, in particular the interstellar magnetic field, are very important in the interaction between the solar system and the interstellar medium. We summarize here our recent work that shows that the interstellar magnetic field affects the symmetry of the heliosphere that can be detected by different measurements. We combined radio emission and energetic particle streaming measurements from Voyager 1 and 2 with extensive state-of-the art 3D MHD modeling, to constrain the direction of the local interstellar magnetic field. The orientation derived is a plane ∼60°-90°from the galactic plane. This indicates that the field orientation differs from that of a larger scale interstellar magnetic field, thought to parallel the galactic plane. Although it may take 7-12 years for Voyager 2 to leave the heliosheath and enter the pristine interstellar medium, the subsonic flows are immediately sensitive to the shape of the heliopause. The flows measured by Voyager 2 in the heliosheath indicate that the heliopause is being distorted by local interstellar magnetic field with the same orientation as derived previously. As a result of the interstellar magnetic field the solar system is asymmetric being pushed in the southern direction. The presence of hydrogen atoms tend to symmetrize the solutions. We show that with a strong interstellar magnetic field with our M. Opher ( ) M. Opher et al. most current model that includes hydrogen atoms, the asymmetries are recovered. It remains a challenge for future works with a more complete model, to explain all the observed asymmetries by V1 and V2. We comment on these results and implications of other factors not included in our present model.

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“…Component 0 refers to the neutral H atoms that come directly from the LISM, while neutral components 1, 2, and 3 are created in the outer heliosheath, inner heliosheath, and supersonic solar wind, respectively. We refer the reader to several reviews for a detailed description of the heliosphere and various physical processes [1,2,3,4].…”

Section: Introductionmentioning

confidence: 99%

Lyman-alpha Radiation Pressure in the Heliosphere: Results from a 3D Monte Carlo Radiative Transfer Simulation

Fayock

Zank

Heerikhuisen

et al. 2015

J. Phys.: Conf. Ser.

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Kinetic-Gasdynamic Modeling of the Heliospheric Interface

Cited by 17 publications

References 40 publications

Tracking the Solar Cycle Through Ibex Observations of Energetic Neutral Atom Flux Variations at the Heliospheric Poles

Tracking the Solar Cycle Through Ibex Observations of Energetic Neutral Atom Flux Variations at the Heliospheric Poles

Confronting Observations and Modeling: The Role of the Interstellar Magnetic Field in Voyager 1 and 2 Asymmetries

Lyman-alpha Radiation Pressure in the Heliosphere: Results from a 3D Monte Carlo Radiative Transfer Simulation

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