Two-Station Interplanetary Scintillation Measurements of Solar Wind Speed near the Sun Using the X-band Radio Signal of the Nozomi Spacecraft

Tokumaru, M.; Fujimaki, Shunsuke; Higashiyama, M.; Yokobe, A.; Ohmi, Tetsuo; Fujiki, K.; Kojima, M.

doi:10.1007/s11207-011-9864-9

Cited by 4 publications

(3 citation statements)

References 37 publications

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“…As result, the solar wind speed is found to rapidly increases up to ≈ 400 km/sat distances between 5-20 Rs. In addition, strong low-frequency acoustic waves, which are regarded as a promising source for coronal heating, are detected at 5-10 Rs from Akaktsuki radio observations (Tokumaru et al (2012b), Imamura et al (2014), Miyamoto et al (2014), Ando et al (2015)). …”

Section: Division E Commission 49mentioning

confidence: 98%

Division E Commission 49: Interplanetary Plasma and Heliosphere

Mann¹,

Manoharan²,

Gopalswamy³

et al. 2015

Proc. IAU

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Abstract. After a little more than forty years of work related to the interplanetary plasma and the heliosphere the IAU's Commission 49 was formally discontinued in 2015. The commission started its work when the first spacecraft were launched to measure the solar wind in-situ away from Earth orbit, both inward and outward from 1 AU. It now hands over its activities to a new commission during an era of space research when Voyager 1 measures in-situ the parameters of the local interstellar medium at the edge of the heliosphere. The commission will be succeeded by C.E3 with a similar area of responsibility but with more focused specific tasks that the community intends to address during the coming several years. This report includes a short description of the motivation for this commission and of the historical context. It then describes work from 2012 to 2015 during the present solar cycle 24 that has been the weakest in the space era so far. It gave rise to a large number of studies on solar energetic particles and cosmic rays. Other studies addressed e.g. the variation of the solar wind structure and energetic particle fluxes on long time scales, the detection of dust in the solar wind and the Voyager measurements at the edge of the heliosphere. The research is based on measurements from spacecraft that are at present operational and motivated by the upcoming Solar Probe + and Solar Orbiter missions to explore the vicinity of the Sun. We also report here the progress on new and planned radio instruments and their importance for heliospheric studies. Contributors to this report are

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Section: Division E Commission 49mentioning

confidence: 98%

Division E Commission 49: Interplanetary Plasma and Heliosphere

Mann¹,

Manoharan²,

Gopalswamy³

et al. 2015

Proc. IAU

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“…Watanabe & Schwenn 1989;Fujiki et al 2005;Tokumaru et al 2006;Tokumaru et al 2010;Tokumaru et al 2011). These studies have formed the foundations for certain 3D reconstruction techniques (Jackson et al 2007;Bisi et al 2010).…”

Section: Introductionmentioning

confidence: 99%

“…For many years, interplanetary scintillation (IPS) has provided scientists with indirect measurements of the changing structure of the solar wind and CMEs between the Sun and terrestrial distances (e.g. Watanabe & Schwenn 1989;Fujiki et al 2005;Tokumaru et al 2006;Tokumaru et al 2010;Tokumaru et al 2011). These studies have formed the foundations for certain 3D reconstruction techniques (Jackson et al 2007;Bisi et al 2010).…”

Section: Introductionmentioning

confidence: 99%

Observational Tracking of the 2D Structure of Coronal Mass Ejections Between the Sun and 1 AU

et al. 2012

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The Solar Terrestrial Relations Observatory (STEREO) provides high cadence and high resolution images of the structure and morphology of coronal mass ejections (CMEs) in the inner heliosphere. CME directions and propagation speeds have often been estimated through the use of time-elongation maps obtained from the STEREO Heliospheric Imager (HI) data.Many of these CMEs have been identified by citizen scientists working within the SolarStormWatch project (www.solarstormwatch.com) as they work towards providing robust real-time identification of Earth-directed CMEs. The wide field of view of HI allows scientists to directly observe the 2-dimensional (2D) structures, while the relative simplicity of time-elongation analysis means that it can be easily applied to many such events, thereby enabling a much deeper understanding of how CMEs evolve between the Sun and the Earth.For events with certain orientations, both the rear and front edge of the CME can be monitored at varying heliocentric distances (R) between the Sun and 1 AU. Here we take four example events with measurable position angle widths and identified by the citizen scientists.These events were chosen for the clarity of their structure within the HI cameras and their long track lengths in the time-elongation maps. We show a linear dependency with R for the growth of the radial width (W) and the 2D aspect ratio (χ) of these CMEs, which are measured out to ~0.7AU. We derived a radial width estimate from a linear best fit for the average of the four CMEs; the equation followed W=0.14R + 0.04.The aspect ratio followed χ=2.5R + 0.86.

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The dispersion analysis of drift velocity in the study of solar wind flows

Olyak

2013

Journal of Atmospheric and Solar-Terrestrial Physics

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Two-Station Interplanetary Scintillation Measurements of Solar Wind Speed near the Sun Using the X-band Radio Signal of the Nozomi Spacecraft

Cited by 4 publications

References 37 publications

Division E Commission 49: Interplanetary Plasma and Heliosphere

Division E Commission 49: Interplanetary Plasma and Heliosphere

Observational Tracking of the 2D Structure of Coronal Mass Ejections Between the Sun and 1 AU

The dispersion analysis of drift velocity in the study of solar wind flows

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