Solar wind heavy ion abundances

Bame, S. J.; Asbridge, J. R.; Feldman, W. C.; Montgomery, M. D.; Kearney, P. D.

doi:10.1007/bf00152368

Cited by 103 publications

(52 citation statements)

References 31 publications

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“…The E/q spectra in Fig. 13 are of typical O-Si-Fe type and in good agreement with the spectra for the cold, low speed, solar wind given by BAME et al (1970, 1974, 1975, 1979), and ZASTENKER and YERMOLAEv (1981. In our experiments, ions heavier than He++ are also found in the E/q spectra in low speed regions, as indicated by the arrows in Fig.…”

Section: Heavy Ionssupporting

confidence: 79%

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Observations of solar wind ions by the interplanetary spacecraft Suisei (PLANET-A).

Mukai¹,

Miyake²,

Terasawa³

et al. 1987

J. geomagn. geoelec

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Overview of the solar wind ion measurements which were carried out by the Japanese interplanetary spacecraft Suisei (PLANET-A) is presented. The instrumentation and results obtained from the initial two-month observations are described.(1) The experiment has been successful in resolving solar wind ions into H+, He++, and, sometimes, other minor constituents, such as 0+6, Si+' , Si+8, and iron groups. These heavy ions, which are considered to contain information on the solar corona, have been identified clearly in the low-speed region. (2) The typical corotating structure is observed during two solar rotations near the sunspot minimum . (3) Velocity fluctuations which are interpreted to be Alfvenic fluctuations are observed in high speed streams. (4) It is also found that the flow vector of the solar wind is significantly deflected westwards in the region of increasing velocity, as a result of pressure gradient caused by stream interaction. (5) Anisotropic distributions of protons which may be related to the local magnetic field are also observed.

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Section: Heavy Ionssupporting

confidence: 79%

“…The shaded region in each spectrum abundance of various elements in the solar corona, we attribute the observed peaks to oxygen ion Oi, silicon ions Si28, Sias, and whole group of iron ions. There is also a of 3.2 to 4.0 (BAME et al, 1975). The E/q spectra in Fig.…”

Section: Heavy Ionsmentioning

confidence: 86%

Observations of solar wind ions by the interplanetary spacecraft Suisei (PLANET-A).

Mukai¹,

Miyake²,

Terasawa³

et al. 1987

J. geomagn. geoelec

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“…[32] The ionosphere is known to be the source of the large abundances of O + ions found within the magnetosphere, since the solar wind contains insufficient oxygen of any charge state [Bame et al, 1975], even if sufficient entry and charge exchange mechanisms are active [Johnson, 1979]. How can the ions escape from the Earth's ionosphere?…”

Section: Discussion: Ionospheric Outflow and Interplanetary Shockmentioning

confidence: 99%

Cluster observations of O⁺ escape in the magnetotail due to shock compression effects during the initial phase of the magnetic storm on 17 August 2001

et al. 2008

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We study the O+ outflow into the magnetotail during the initial phase of the 17 August 2001 magnetic storm. Solar wind and magnetospheric data are used from instruments onboard ACE, WIND, and Cluster spacecraft. The interplanetary shock arrival at Earth caused a large compression of the magnetosphere. During this event, the Cluster spacecraft were crossing the plasma sheet boundary layer of the magnetotail. Thus this case study constitutes a unique opportunity to observe the magnetotail response to a shock driven storm with multiple S/C data. We observed a field aligned oxygen (O+) outflow in the plasma sheet boundary layer and a bidirectional O+ flux in the central plasma sheet. Using the Cluster multiple spacecraft data, we derived the O+ gradient and the escape rate into the magnetotail during the initial phase of the magnetic storm. We found an escape rate of 4.0 × 1024 O+ ions s−1 in the plasma sheet boundary layer of the magnetotail, which is about 20 times the O+ inflow into the ring current during an intense magnetic storm.

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“…In the lateral branches of the streamers the abundance decreases monotonically with heliodistance from 3.5×10 −4 (8.54) to 2.2×10 −4 (8.34), that is, oxygen is depleted by a factor of 2 and 3 at 1.5 R and 2.2 R , respectively. The oxygen abundance of streamers can be compared with the value observed in the slow solar wind in the ecliptic plane by Bame et al (1975) (von Steiger et al, 1997) during a period of declining activity, between mid-1992 and mid-1993. In this period the solar wind speed was observed to vary periodically between 400 km s −1 and 800 km s −1 .…”

Section: Discussionmentioning

confidence: 99%

Oxygen abundance in coronal streamers during solar minimum

2001

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Abstract. We present a study of the oxygen abundance relative to hydrogen in the equatorial streamer belt of the solar corona during the recent period of activity minimum. The oxygen abundance is derived from the spectroscopic observations of the outer corona performed during 1996 with the Ultraviolet Coronagraph Spectrometer (SOHO) in the ultraviolet region. This study shows that the depletion of oxygen, by almost one order of magnitude with respect to the photospheric values, found in the inner part of streamers by Raymond et al. (1997a) is a common feature of the solar minimum streamer belt, which exhibits an abundance structure with the following characteristics. In the core of streamers the oxygen abundance is 1.3×10 −4 at 1.5 R , then it drops to 0.8×10 −4 at 1.7 R , value which remains almost constant out to 2.2 R . In the lateral bright structures that are observed to surround the core of streamers in the oxygen emission, the oxygen abundance drops monotonically with heliodistance, from 3.5×10 −4 at 1.5 R to 2.2×10 −4 at 2.2 R . The oxygen abundance structure found in the streamer belt is consistent with the model of magnetic topology of streamers proposed by Noci et al. (1997). The composition of the plasma contained in streamers is not the same as observed in the slow solar wind. Even in the lateral branches, richer in oxygen, at 2.2 R the abundance drops by a factor 2 with respect to the slow wind plasma observed with Ulysses during the declining phase of the solar cycle. Hence the slow wind does not appear to originate primarily from streamers, with the exception perhaps of the plasma flowing along the heliospheric current sheet.

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Solar wind heavy ion abundances

Cited by 103 publications

References 31 publications

Observations of solar wind ions by the interplanetary spacecraft Suisei (PLANET-A).

Observations of solar wind ions by the interplanetary spacecraft Suisei (PLANET-A).

Cluster observations of O⁺ escape in the magnetotail due to shock compression effects during the initial phase of the magnetic storm on 17 August 2001

Oxygen abundance in coronal streamers during solar minimum

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Solar wind heavy ion abundances

Cited by 103 publications

References 31 publications

Observations of solar wind ions by the interplanetary spacecraft Suisei (PLANET-A).

Observations of solar wind ions by the interplanetary spacecraft Suisei (PLANET-A).

Cluster observations of O+ escape in the magnetotail due to shock compression effects during the initial phase of the magnetic storm on 17 August 2001

Oxygen abundance in coronal streamers during solar minimum

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Cluster observations of O⁺ escape in the magnetotail due to shock compression effects during the initial phase of the magnetic storm on 17 August 2001