Higher‐energy plasma ions found near the termination shock: Analyses of Voyager 2 data in the heliosheath and in the outer heliosphere

Intriligator, D. S.; Intriligator, James; Miller, Warren D.; Webber, W. R.; Decker, R. B.

doi:10.1029/2009ja014967

Cited by 4 publications

(6 citation statements)

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“…This December, 2006 event has also been propagated through the heliosphere by (Intriligator, et al, 2010b), the 2 nd time was between days 333-348 (2007.91-2007.95). Large transient energetic plasma, TSP and ACR intensity changes were seen near these times in later 2007 by the LECP and CRS instruments on V2 (Decker, et al, 2009;Intriligator, et al, 2010a). Large magnetic field enhancements were also seen near the times of the particle intensity changes (Burlaga, et al, 2008).…”

Section: Variations Of the Hts Distance At V1 And V2 During The 2002-...mentioning

confidence: 88%

“…We note that Intriligator et al [2010a] have observed high‐energy solar wind ions at roughly twice the average solar wind speed at V2 two times in 2007. The first time was on days 242–243 in conjunction with the HTS crossings [ Intriligator et al , 2010b], the second time was between days 333 and 348 (2007.91 and 2007.95). Large transient energetic plasma, termination shock particle (TSP), and anomalous cosmic ray (ACR) intensity changes were seen near these times in later 2007 by the low‐energy charged particle (LECP) and cosmic ray subsystem (CRS) instruments on V2 [ Decker et al , 2009; Intriligator et al , 2010a].…”

Section: Variations Of the Hts Distance At V1 And V2 During The 2002–mentioning

confidence: 99%

“…s -1 ). The HAFSS model used (as discussed inIntriligator, et al, 2010a) does not take into account the fact that the December, 2006 IP shock is propagating beyond the HTS. HAFSS assumes the IP shock is always in the solar wind.…”

mentioning

confidence: 99%

“…HAFSS assumes the IP shock is always in the solar wind. Also including the effects of slowing down, we estimate the interplanetary shock as calculated byIntriligator, et al, 2010a, arrived at V2 in the 26 day time interval centered on 2007.86 one 26 day interval, with a shock pressure increase of 1.3 times.An enlarged profile of the HTS behavior in the year 2007 for these different possibilities is shown in Figure6. Instead of a rapidly decreasing HTS distance at the time of the V2 HTS crossing, we now find that the HTS distance is almost constant throughout the period before and after the shock crossing for all three possibilities.…”

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confidence: 99%

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Voyagers 1 and 2 in a shrunken and squashed heliosphere

Webber

Intriligator

2011

J. Geophys. Res.

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[1] We have extended our earlier calculations of the distance to the heliospheric termination shock (HTS), which covered the period from the launch of V1 and V2 in 1977 to 2005, to the period from 2006 to 2011. During this latter period, the solar wind speed, ram pressure, and magnetic field decreased to the lowest levels in recent history, related to the sunspot minimum in [2008][2009]. The HTS distance has decreased correspondingly so that V1, which was crossed by the HTS at 94 AU in late 2004, would now, in early 2011, be expected to reach the HTS at a distance of ∼80 AU, when the HTS distance would be expected to be at its minimum. Similarly, V2, which was crossed by the HTS at 84 AU in mid-2007, would, in early 2011, reach the HTS at a distance of only 74 AU. These distances, in early 2011, are ∼15% less than those at which V1 and V2 initially reached the HTS. The distance to the heliopause (HP) is more uncertain, but recent calculations place its equilibrium distance at between 1.4 and 1.6 times the HTS distance. Allowing for an additional 1 year for the HP to reach its equilibrium minimum distance relative to the HTS would mean that, assuming this distance remains a constant fraction larger than the HTS distance, the HP distance would be at its minimum distance of (1.4-1.6) × 80 AU = 112-128 AU in the direction of V1 in early 2012. At this time, V1 will be at a distance of ∼120 AU so that there is a possibility that V1 could cross the HP and enter interstellar space at the time 2012.0 ± 1 year. If the crossing does not happen during this time period, then it is unlikely that V1 will reach this defining boundary before about 2016 because of the expected outward motion of the HTS and the HP toward their more normal distances of 85-96 and ∼120-140 AU, coincident with the maximum of the new sunspot cycle.

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Section: Variations Of the Hts Distance At V1 And V2 During The 2002-...mentioning

confidence: 88%

Section: Variations Of the Hts Distance At V1 And V2 During The 2002–mentioning

confidence: 99%

mentioning

confidence: 99%

mentioning

confidence: 99%

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Voyagers 1 and 2 in a shrunken and squashed heliosphere

Webber

Intriligator

2011

J. Geophys. Res.

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“…Pressure fluctuations in the turbulent solar wind make the location of the termination shock highly dynamic; it moved across Voyager 2 five times Burlaga et al, 2008;Intriligator et al, 2010aIntriligator et al, , 2010b. Pressure variations resulting directly from solar activity include interplanetary shock waves, coronal mass ejections (CMEs), corotating interaction regions (CIRs), and global merged interaction regions (GMIRs).…”

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confidence: 99%

The influence of pickup protons, from interstellar neutral hydrogen, on the propagation of interplanetary shocks from the Halloween 2003 solar events to ACE and Ulysses: A 3-D MHD modeling study

et al. 2011

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[1] We describe our 3-D, time-dependent, MHD solar wind model that we recently modified to include the physics of pickup protons from interstellar neutral hydrogen. The model has a time-dependent lower boundary condition, at 0.1 AU, that is driven by source surface map files through an empirical interface module. We describe the empirical interface and its parameter tuning to maximize model agreement with background (quiet) solar wind observations at ACE. We then give results of a simulation study of the famous Halloween 2003 series of solar events. We began with shock inputs from the Fearless Forecast real-time shock arrival prediction study, and then we iteratively adjusted input shock speeds to obtain agreement between observed and simulated shock arrival times at ACE. We then extended the model grid to 5.5 AU and compared those simulation results with Ulysses observations at 5.2 AU. Next we undertook the more difficult tuning of shock speeds and locations to get matching shock arrival times at both ACE and Ulysses. Then we ran this last case again with neutral hydrogen density set to zero, to identify the effect of pickup ions. We show that the speed of interplanetary shocks propagating from the Sun to Ulysses is reduced by the effects of pickup protons. We plan to make further improvements to the model as we continue our benchmarking process to 10 AU, comparing our results with Cassini observations, and eventually on to 100 AU, comparing our results with Voyager 1 and 2 observations.

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Radiation‐Tolerant Electronic Devices Using Wide Bandgap Semiconductors

Muhammad

Wang

Zhang

et al. 2022

Adv Materials Technologies

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These energetic particles, such as electrons, protons, neutrons, X-rays, or gamma rays, induced damage in materials (used in electronic devices) through total ionization and displacement, [4] which would affect the reliability of the electronic devices. [5][6][7] Electronics failure occurs in harsh and inaccessible environments through various paths, such as electromagnetic waves, nuclear reactions, and high-frequency communications systems. Therefore, the radiationhardened requirements of the deployed electronic technology depend on the specific high-energy photons and particles in the radiation environment. For example, Mars exploration requires a special proton anti-radiation in electronics. At the same time, the safety supervision and inspection of the contaminated nuclear area are suggested to be equipped with high resilience towards the alpha, beta, and gamma rays. The development of radiation-hard electric circuits over the years has led researchers to consider the application of functional anti-irradiation material to devices. The current focus is on developing complementary metal-oxide semiconductors (CMOS) with wide bandgap semiconductors (WBGs), which are well suited to large-area aerospace applications. [8][9][10] As shown in Figure 1, a notable material class of WBGs can be listed as metal oxides (MOS), transition-metal dichalcogenides (TMDs), silicon carbide, gallium nitride, and others. WBGs materials contribute robust properties under harsh conditions due to their strong electronic compliance, high-temperature competence, and strong atomic bond energy. [11][12][13][14][15][16] They have been proposed as favorable materials for aerospace and other radiation-hardened applications. Generally, the bandgap in the semiconductor reflects the extra energy that a valence electron must access to become a free electron. Its large bandgap of more than 3 eV guarantees inherent reliability in the semiconductors, providing transparency for the low-energy photons. The large, spherical nsorbitals in the conduction band (CB) of MOS also play a critical role in high dopability for hosting a high density of electrons, leading to the remarkably tolerance to various radiation fluences. [17][18][19][20][21][22][23][24][25][26][27][28][29][30][31][32][33][34][35] Understanding the apparent immunity of the WBGs to various radiation environments and radiation-hard electronic engineering would be critical for pushing the technology further and understanding its limitations. Efforts to address these issues have been underway over the past two decades. Substantial progress has also been made in designing radiation-hard thin films transistors (TFTs) with ZnO, Ga 2 O 3 , In 2 O 3 , SnO 2 , IGZO, SiC, GaN, and many other WBGs, The aspiration of electronic technologies that are resistant to high-energy cosmic radiation is essential for current harsh radiation environment exploration. Integrated circuits mostly require post-processing after designing, making their structures more complex than the standard systems. Thus, unique de...

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Higher‐energy plasma ions found near the termination shock: Analyses of Voyager 2 data in the heliosheath and in the outer heliosphere

Cited by 4 publications

References 18 publications

Voyagers 1 and 2 in a shrunken and squashed heliosphere

Voyagers 1 and 2 in a shrunken and squashed heliosphere

The influence of pickup protons, from interstellar neutral hydrogen, on the propagation of interplanetary shocks from the Halloween 2003 solar events to ACE and Ulysses: A 3-D MHD modeling study

Radiation‐Tolerant Electronic Devices Using Wide Bandgap Semiconductors

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