Interplanetary Shock Parameters Near Jupiter's Orbit

Echer, E.

doi:10.1029/2019gl082126

Cited by 8 publications

(4 citation statements)

References 49 publications

(131 reference statements)

Supporting

Mentioning

Contrasting

Order By: Relevance

“…Interplanetary (IP) shocks are solar wind structures commonly observed in the heliosphere (Echer, 2019; Harada et al., 2017; Mihalov et al., 1987; Richardson & Wang, 2005; Winslow et al., 2015). IP shocks arise when the ratio of the relative speed (between the ambient solar wind and the shock itself) to the local magnetosonic speed, defined as the magnetosonic Mach number, is greater than 1 (Jeffrey & Taniuti, 1964; Priest, 1981).…”

Section: Introductionmentioning

confidence: 99%

Impact Angle Control of Local Intense dB/dt Variations During Shock‐Induced Substorms

et al. 2021

View full text Add to dashboard Cite

show abstract

Section: Introductionmentioning

confidence: 99%

Impact Angle Control of Local Intense dB/dt Variations During Shock‐Induced Substorms

et al. 2021

View full text Add to dashboard Cite

show abstract

“…These results can be compared with the radial variations of shock parameters in the outer heliosphere, beyond ∼1.0 au from the Sun. The shock occurrence is found to peak at ∼5.0 au (e.g., Hoang et al 1995;González-Esparza et al 1998;Richardson & Wang 2005;Neugebauer 2013;Echer 2019), beyond which it decreases linearly (Hajra 2021). In addition, Hajra (2021) reported that the radial variation of the shock M ms between ∼1.0 and ∼15.0 au is slower and less correlated to r h .…”

Section: Summary and Discussionmentioning

confidence: 99%

Interplanetary Shocks between 0.3 and 1.0 au: Helios 1 and 2 Observations

Hajra

Tsurutani²,

Lakhina

et al. 2023

ApJ

View full text Add to dashboard Cite

The Helios 1 (H1) and Helios 2 (H2) spacecraft measured the solar winds at a distance between ∼0.3 and 1.0 au from the Sun. With increasing heliocentric distance (r h), the plasma speed is found to increase at ∼34–40 km s−1 au−1 and the density exhibits a sharper fall ( r h − 2 ) compared to the magnetic field magnitude ( r h − 1.5 ) and the temperature ( r h − 0.8 ). Using all available solar wind plasma and magnetic field measurements, we identified 68 and 39 fast interplanetary shocks encountered by H1 and H2, respectively. The overwhelming majority (85%) of the shocks are found to be driven by interplanetary coronal mass ejections (ICMEs). While the two spacecraft encountered more than 73 solar wind high-speed streams (HSSs), only ∼22% had shocks at the boundaries of corotating interaction regions (CIRs) formed by the HSSs. All of the ICME shocks were found to be fast forward (FF) shocks; only four of the CIR shocks were fast reverse shocks. Among all ICME FF shocks (CIR FF shocks), 60% (75%) are quasi-perpendicular with shock normal angles (θ Bn) ≥ 45° relative to the upstream ambient magnetic field, and 40% (25%) are quasi-parallel (θ Bn < 45°). No radial dependences were found in FF shock normal angle and speed. The FF shock Mach number (M ms), magnetic field, and plasma compression ratios are found to increase with increasing r h at the rates of 0.72, 0.89, and 0.98 au−1, respectively. On average, ICME FF shocks are found to be considerably faster (∼20%) and stronger (with ∼28% higher M ms) than CIR FF shocks.

show abstract

“…The interplanetary fast shocks were identified on mSWim data using the characteristics described by Echer et al 2010 [13] and Echer 2019 [20]. Those shocks are described as follows:…”

Section: Interplanetary Fast Shocksmentioning

confidence: 99%

Solar Wind Interaction with Jupiter’s Magnetosphere

Rodríguez-Gómez

2023

AAST

View full text Add to dashboard Cite

This paper studies the effects of the solar wind on Jupiter's magnetosphere. The solar wind parameters are characterized using the Michigan Solar Wind Model (mSWiM) solar wind data propagated to Jupiter from 1997 to 2016. This analysis covers almost solar cycles 23 and 24. Interplanetary fast shocks: Forward shocks (FS), Reverse shocks (RS), and solar wind dynamic pressure were obtained and analyzed during the apparent opposition periods. The fast forward (FS) shocks were predominant during this period. Generally, the solar wind dynamic pressure from FS and RS shocks follows the solar cycles 23 and 24.

show abstract

Interplanetary Shock Parameters Near Jupiter's Orbit

Cited by 8 publications

References 49 publications

Impact Angle Control of Local Intense dB/dt Variations During Shock‐Induced Substorms

Impact Angle Control of Local Intense dB/dt Variations During Shock‐Induced Substorms

Interplanetary Shocks between 0.3 and 1.0 au: Helios 1 and 2 Observations

Solar Wind Interaction with Jupiter’s Magnetosphere

Contact Info

Product

Resources

About