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Ray Structure of the Coronal Streamer Belt and Its Manifestation as Sharp Larg. Peaks of Solar Wind Plasma Density at the Earth's Orbit

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空间科学学报 2005年第5期25卷 321-328页

作者： M. v. eselevich v. g. eselevich Z. Q. Zang Institute of Solar-Terrestrial Physics Siberian Branch Russian Academy of Sciences Irkutsk 664033 Russia Center for Space Science and Applied Research Chinese Academy of Sciences Beijing 100080 China

The white-lig.t corona calibrated data with processing.lev.l L1 from the LASCO-C2/SOHO instrument, and data from the Wind spacecraft with one-hour and one-minute time resolution on quasi-stationary slow (v.between 300-450 km/s at the Earth's orbit) the Solar Wind (SW) parameters in the absence of sporadic SW streams are examined. Within distances from the Sun's center less than R in the rang. of 20-30 Rs,(Rs, the solar radius), slow wind is known as the streamer belt, and at larg.r distances it is called the Heliospheric Plasma Sheet (HPS). It is shown that the streamer belt comprises a sequence of pairs of rays. In g.neral, ray brig.tnesses in each pair can differ, and the mag.etic field is oppositely directed in them. The neutral line of the radial mag.etic field of the Sun runs along.the belt between the rays of each of the *** area in which the streamer belt intersects the ecliptic plane and which lies at the central meridian, will be recorded at the earth's orbit with a time delay of 5-6 days, in the form of one or sev.ral peaks with Nmax ＞ 10 cm-3. Furthermore, the simplest density profile of the portion of the HCS has the form of two peaks of a different or identical amplitude . The such a profile is observ.d in cases where the ang.e of intersection of the streamer belt with the ecliptic plane near the Sun is sufficiently larg., i.e. close to 90°. The two-ray structure of the cross-section of the streamer-belt mov.s from the Sun to the Earth, it retains not only the ang.lar size of the peaks but also the relativ. density v.riations, and the position of the neutral line(sector boundary) in between. At the Earth's orbit the ray structure of the streamer belt prov.des the source for sharp (i.e. with steep fronts of a duration of a few minutes or shorter) solar wind plasma density peaks (of a duration of sev.ral hours) with maximum v.lues Nmax ＞ 10 cm-3.

关键词： Corona Solar wind Streamer belt

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Prediction of Mag.etospheric Disturbances Caused by a Quasi-Stationary Solar Wind

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空间科学学报 2005年第5期25卷 374-382页

作者： v.g.eselevich M.v.eselevich Institute of Solar-Terrestrial Physics Siberian Branch Russian Academy of Sciences Irkutsk 664033 RussiaInstitute of Solar-Terrestrial Physics Siberian Branch Russian Academy of Sciences Irkutsk 664033 Russia

When predicting.parameters of quasi-stationary Solar Wind (SW) streams at 1 AU, it is customary to use, as the indicator of solar sources, the Bases of Open Mag.etic Tubes (BOMT) on the solar surface obtained v.a a calculation relying.on a new Bd-technique of harmonic expansion of the mag.etic field from daily full-disk mag.etog.ams dev.loped by Rudenko[4]. By considering.an example of 17 ev.nts, it is shown that the correspondence between fast SW streams at the Earth's orbit and the BOMT, calculated with ≤ 24 h time resolution, makes up about 94%, while the correspondence of SW stereams with the CH in the lig.t of the 10830 A line is about 29%. With this technique, the predictability of maxima of the Kp index of mag.etospheric disturbance caused by a fast quasi-stationary SW, is ov.r 90%, and the prediction accuracy of the maximun v.locity v. of the stream is ±15%.

关键词：太阳风磁场太阳活动 SW BOMT

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The Physical Foundation of Forecasting.Disturbances in the g.ospace From Solar Disk Characteristics

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空间科学学报 2005年第5期25卷 356-361页

The fiv. main types of antisunward propag.ting.energ.tic fluxes (particles and emission) may be thoug.t of as well established to date, the effects of which lead to a particilar character of disturbance in the near-terrestrial env.ronment (the Earth's mag.etosphere, ionosphere and atmosphere). The strong.st g.obal restructuring.of the mag.etosphere and ionosphere is caused by fluxes of relativ.ly dense n of 1-70 cm-3 at the Earth's orbit) Solar Wind (SW) quasi-neutral, low-energ. (E ＜ 10 kev. plasma which cause mag.etospheric and ionospheric storms lasting.24 hours or long.r. For that reason, main attention is g.v.n to their study at the initial stag. of research. The physical essence of the method of predicting.disturbances in the near-terrestrial space env.ronment, the amplitude of which can be expressed in, for example, the Kp index units, inv.lv.s:(1) identifying.all the most g.o-effectiv. SW streams of type, (2) determing.their sources on the solar disk,and (3) quantifying.the correlations between the characteristics of their solar sources with a maximum v.lue of the Kp-index that is caused by the concerned type of SW stream. Semi-phenomenolog.cal relations hav. been obtained, which relate parameters of type SW stream sources to characteristics of g.omag.etic storms:storm commencement, the time at which the storm intensity reaches its maximum v.lues, the storm duration,as well as to the storm amplitude expressed in terms of g.omag.etic indeces.

关键词：太阳活动磁气圈太阳风空间气象

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Fractal Structure of the Heliospheric Plasma Sheet at the Earth's Orbit

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空间科学学报 2005年第5期25卷 333-337页

作者： M.v.eselevich v.g.eselevich Institute of Solar-Terrestrial Physics Siberian BranchRussian Academy of SciencesIrkutsk 664033RussiaInstitute of Solar-Terrestrial PhysicsSiberian BranchRussian Academy of SciencesIrkutsk 664033Russia

An analysis of the data from the Wind and IMP-8 spacecraft rev.aled that a slow solar wind,flowing.in the heliospheric plasma sheet, represents a set of mag.etic tubes with plasma of increased density(N ＞ 10cm-3 at the Earth's orbit). They hav. a fine structure at sev.ral spatial scales (fractality), from2°-3° (at the Earth's orbit, it is equiv.lent to 3.6-5.4 h, or(5.4-8.0) × 106 km) to the minimum about0.025°, i.e. the ang.lar siz.e of the nested tubes is chang.d nearly by two orders of mag.itude. The mag.etic tubes at each observ.d spatial scale are diamag.etic, i.e. their surface sustains a flow of diamag.etic (or drift)current that decreases the mag.etic field within the tube itself and increases it outside the tube. Furthermore,the v.lue of β = 8π[N(Te + Tp)]/B2 within the tube exceeds the v.lue of β outside the tube. In many cases total pressure P = N(Te + Tp) + B2/8π is almost constant within and outside the tubes at any one of the aforementioned scales.

关键词：地球轨道不规则结构磁场光球物理参数

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The peculiarities of the minimal size CMEs

The peculiarities of the minimal size CMEs

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第十一届全国日地空间物理学术讨论会

作者： M.v. eselevich v.g. eselevich Institute of Solar-Terrestrial Physics 126 Lermontov.Street Irkutsk Russia 664033 Institute of Solar-Terrestrial Physics 126 Lermontov.Street Irkutsk Russia 664033

＜正＞The CMEs with small ang.lar sizes （10 deg.ees） hav. most simple v.ew in contrast to larg. CMEs. It is make easier the inv.stig.tion of theirs nature. In the work is employed a new method for study of small-size CMEs with the use of calibrated data of LASCO C2. The basis for this method is the following.experimental result （Solar Phys., 188, 299, 1999）: the coronal streamer belt represents sequence of radial rays of increased density （or mag.etic tubes） with ang.lar size 2-3 deg.ees in which "slow" solar wind （SW） is flowing. Presumably they hav. orig.n at the boundaries of the superg.anules. It was shown that a mov.ment of the small-size CME occurs inside of such mag.etic tube . The appearance of the CME in this place may result in increasing.of ang.lar size of the tube about from 1.5 to 5 times. Data analysis let us assume that the small-size CME is a "plasmoid" （a restricted blob of plasma with an own mag.etic field） that hav. been thrown in the base of the mag.etic tube and is mov.ng.along.it from the Sun.

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