Velocity observations at high latitude and the acceleration phenomena

Kojima, M.; Asai, Kikuo; Kozuka, Y.; Misawa, Hiroaki; Watanabe, Hironori; Yamauchi, Y.

doi:10.1016/0273-1177(95)00320-e

Cited by 5 publications

(4 citation statements)

References 16 publications

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“…Kojima and Kakinuma (1990) analyzed the radial distance dependence of the IPS speed and found that both of a low-speed wind and a high-speed wind show large speed increase at distance range of 0.1-0.3 AU and become stable flow beyond 0.3 AU ( Figure 1). Misawa and Kojima (1992) and Kojima et al (1995) investigated when in solar activity phase many of the streams with the large speed increase tend to be observed and where they have source regions on the Sun. Major of them were observed in the minimum phase of solar activity and at high latitudes from the magnetic neutral line.…”

Section: Radial Distance Dependence Of Ips Speedmentioning

confidence: 99%

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Acceleration Phenomena Observed by Interplanetary Scintillation at 0.1–0.3 AU

Kojima

Misawa

Watanabe

et al. 1996

International Astronomical Union Colloquium

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Interplanetary scintillation has observed high-latitude streams which show low speeds (≤400 km/s) within 0.3 AU and high speeds (≥700 km/s) beyond 0.3 AU. The foot points of these streams were located in the Hel coronal holes or at their boundaries. Since the IPS measurement is biased by one or several mechanisms, we investigated whether this acceleration phenomena could be caused by bias effects or not. Speed increase of more than 100 km/s is left without being explained by the bias effects.

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Section: Radial Distance Dependence Of Ips Speedmentioning

confidence: 99%

“…Since scattering at 327 MHz is strong at distances within about 0.2 AU, biases in a strong scattering region have to be examined. Kojima et al (1995) examined strong scattering effects on the IPS speed measurements using the IPS data measured at frequencies of 69 MHz and 74 MHz (VHF) by the STE Lab. and UCSD.…”

Section: Bias In Strong Scatteringmentioning

confidence: 99%

Acceleration Phenomena Observed by Interplanetary Scintillation at 0.1–0.3 AU

Kojima

Misawa

Watanabe

et al. 1996

International Astronomical Union Colloquium

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“…Observations of IPS, usually at a frequency of 327 MHz, have been carried out since 1970s in the world. Observations of IPS are extremely useful in determining the physical parameters and structure of the solar wind throughout the inner heliosphere (e.g., Manoharan 1993, Kojima et al 1995, Breen et al 2002, Manoharan & Agalya 2011, Bisi et al 2007, Chang et al 2016, and Morgan et al 2018.…”

Section: Introductionmentioning

confidence: 99%

New Interplanetary Scintillation Telescope Array in China for Space Weather

Yan¹,

Wang²,

Chen³

et al. 2018

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Interplanetary Scintillation (IPS) is a useful ground-based method to investigate solar wind structure and its parameters through the scintillation of distant, compact radio sources at radio wavelengths. Current worldwide IPS facilities include both single-site systems (which are typically a large telescope or array), and multi-site systems (which are typically more varied telescope/array sizes). To combine the advantages of both of these system types, we propose a new design for the IPS telescope in China, implementing a large collecting area at one main site, with smaller collecting areas at the other sites. This new IPS telescope concept is a part of the Phase-II Meridian Space Weather Monitoring Project under the 2016-2020 National Infrastructure Program in China to be constructed in near future. Some specifications and basic considerations of this telescope are described in this paper.

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“…One can use the power spectral fitting method to obtain the solar wind speed. The multi-station method, as used in Japan, is a three-station system (Kojima et al 1995) where one can measure the projected solar wind speed directly. China began IPS studies in the 1990s with the phased array mode of the Miyun Synthesis Radio Telescope (MSRT) at 232 MHz.…”

Section: Introductionmentioning

confidence: 99%

Observations of interplanetary scintillation with a single-station mode at Urumqi

Liu¹,

Zhang²,

Li³

et al. 2010

Res. Astron. Astrophys.

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The Sun affects the Earth's physical phenomena in multiple ways, in particular the material in interplanetary space comes from coronal expansion in the form of inhomogeneous plasma flow (solar wind), which is the primary source of the interplanetary medium. Ground-based Interplanetary Scintillation (IPS) observations are an important and effective method for measuring solar wind speed and the structures of small diameter radio sources. We discuss one mode of ground-based single-station observations: Single-Station Single-Frequency (SSSF) mode. To realize the SSSF mode, a new system has been established at Urumqi Astronomical Observatory (UAO), China, and a series of experimental observations were carried out successfully from May to December, 2008.Abstract The Sun affects the Earth's physical phenomena in multiple ways, in particular the material in interplanetary space comes from coronal expansion in the form of inhomogeneous plasma flow (solar wind), which is the primary source of the interplanetary medium. Ground-based Interplanetary Scintillation (IPS) observations are an important and effective method for measuring solar wind speed and the structures of small diameter radio sources. We discuss one mode of ground-based single-station observations: Single-Station Single-Frequency (SSSF) mode. To realize the SSSF mode, a new system has been established at Urumqi Astronomical Observatory (UAO), China, and a series of experimental observations were carried out successfully from May to December, 2008.

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Velocity observations at high latitude and the acceleration phenomena

Cited by 5 publications

References 16 publications

Acceleration Phenomena Observed by Interplanetary Scintillation at 0.1–0.3 AU

Acceleration Phenomena Observed by Interplanetary Scintillation at 0.1–0.3 AU

New Interplanetary Scintillation Telescope Array in China for Space Weather

Observations of interplanetary scintillation with a single-station mode at Urumqi

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