Magnetic loop behind an interplanetary shock: Voyager, Helios, and IMP 8 observations

Burlaga, L. F.; Sittler, E. C.; Mariani, F.; Schwenn, R.

doi:10.1029/ja086ia08p06673

Cited by 1,503 publications

(1,263 citation statements)

References 26 publications

(22 reference statements)

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“…One class of ejecta that is particularly e ective in in uencing the magnetic ÿeld and magnetosphere of Earth and presumably of Mercury as well is the set of magnetic clouds. A "magnetic cloud" is deÿned by three properties observed as it moves past a spacecraft at ≈ 1 AU in a day or so: 1) a large, smooth rotation of the magnetic ÿeld direction; 2) higher than average magnetic ÿeld strengths; and 3) lower than average proton temperatures and ÿ (Burlaga et al, 1981). A magnetic cloud observed by Helios 1 on 20 June 1980 at 0:6 AU (Burlaga et al, 1982) is shown in Fig.…”

Section: Magnetic Clouds and Other Ejectamentioning

confidence: 99%

Magnetic fields and plasmas in the inner heliosphere: Helios results

Burlaga

2001

Planetary and Space Science

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The magnetic ÿeld of Mercury and the structure and dynamics of Mercury's magnetosphere, which will be studied by the spacecraft orbiting Mercury, are strongly in uenced by the interaction of the solar wind with Mercury. In order to understand the internal magnetic ÿeld, it will be necessary to correct the observations of the external ÿeld for the distortions produced by the solar wind. Understanding of the solar wind interaction with Mercury is essential for understanding the structure and dynamics of the magnetosphere and phenomena such as magnetic storms. Helios 1 and 2 made a number of passes in the region traversed by the orbit of Mercury, and each pass provided a sample of the solar wind environment of Mercury. This paper reviews the plasma and magnetic ÿeld observations from Helios that provide a general basis for interpreting the observations of Mercury that will be made by orbiting spacecraft. The variables that govern the structure and dynamics of the magnetospheres of Mercury and Earth are approximately 5 -10 times larger at Mercury than at Earth. Thus, the solar wind interaction with Mercury will be much stronger than the interaction with Earth. Moreover, the solar wind at Mercury is probably more variable than that at Earth. There is a clear need for measurements of the solar wind during the approach of spacecraft to Mercury and while they are in orbit around Mercury.

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Section: Magnetic Clouds and Other Ejectamentioning

confidence: 99%

Magnetic fields and plasmas in the inner heliosphere: Helios results

Burlaga

2001

Planetary and Space Science

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“…as defined by Burlaga et al [8], indicated in the column "IP Kind" as "cloud", 2 were interplanetary ejecta without the signature of magnetic cloud, indicated by "eje" in this same column, and the other 2 were only compressed sheath regions, as a consequence of an interplanetary shock passage, indicated by "neje". The column "Bs source" indicates the various sources of southward interplanetary magnetic field responsible for the occurrence of each storm.…”

Section: Discussionmentioning

confidence: 99%

“…** not a clear shock, lack of discontinuity in the parameters. Symbols are: 1 = unequivocal association between a CME and an interplanetary event; 2 = possible association between a CME and an interplanetary event; neje = not an interplanetary ejecta structure of any kind; eje = definitely an interplanetary ejecta but not defined; cloud = interplanetary ejecta of the magnetic cloud type according to Burlaga et al [8].…”

Section: Introductionmentioning

confidence: 99%

“…The second type of interplanetary structure responsible for the storms, also called geoeffective structures, found by Tsurutani et al [7] were interplanetary ejecta, which are believed to be the ejected material from the CMEs observed by coronagraphs, near the Sun. These ejecta can be very well behaved magnetic structures, like interplanetary magnetic clouds [8], modeled by a force-free ( J × B = 0) magnetic flux rope assuming local cylindrical symmetry [9]. Very often, magnetic clouds possess intense magnetic field, with a substantial fraction pointing southward.…”

Section: Introductionmentioning

confidence: 99%

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Great geomagnetic storms in the rise and maximum of solar cycle 23

Lago¹,

Vieira²,

Echer³

et al. 2004

Braz. J. Phys.

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Geomagnetic storms are intervals of time when a sufficiently intense and long-lasting interplanetary convection electric field leads, through a substantial injection of energy into the magnetosphere-ionosphere system, to an intensified ring current, strong enough to exceed some key threshold of the quantifying storm time Dst index. We have studied all the 9 great magnetic storms (peak Dst < -200 nT) observed during the rise and maximum of solar cycle 23 (from 1997 to early 2001), in order to identify their solar and interplanetary causes. Apart of one storm occurred during the period without observations from the Solar and Heliospheric Observatory (SOHO), all of them were related to coronal mass ejections observed by the Large Angle and Spectroscopic Coronagraph (LASCO). The sources of interplanetary southward magnetic field, Bs, responsible for the occurrence of the storms were related to the intensified shock/sheath field, interplanetary magnetic cloud's field, or the combination of sheath-cloud or sheath-ejecta field. It called our attention the fact that one of the events was related to a slow CME, with CME expansion speed not greater than 550 km/s. The purpose of this paper is to address the main sources of large geomagnetic disturbances using the current satellite capability available. As a general conclusion, we found that shock/sheath compressed fields are the most important interplanetary causes of great magnetic storms during this period.

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“…While the first two terms were rather inclusive in their definition, the last one is rather restrictive [Burlaga et al, 1981]. A magnetic cloud has to have a particular duration, a smooth rota tion^ strong magnetic field, and a low proton temperature.…”

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confidence: 99%

In defense of the term ICME

Russell

2001

EoS Transactions

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As Burlaga [2001] correctly points out, the term “cloud” has been used for many years to describe solar wind disturbances. “Plasma cloud,” “magnetized plasma cloud,” and now “magnetic cloud” have all seen use. While the first two terms were rather inclusive in their definition, the last one is rather restrictive [Burlaga et al., 1981]. A magnetic cloud has to have a particular duration, a smooth rotation, strong magnetic field, and a low proton temperature. Thus, we are forced into adopting a separate name for many structures that do not fit this restrictive scheme. The term “ejecta” could be used, but there are two types of ejecta: flare ejecta and coronal mass ejecta. The latter term has been used extensively for the disturbance seen at 1 AU that arises in response to a coronal mass ejection (CME) detected at the Sun. This usage has led to some difficulties, because one line of research in this field is to compare the properties of CMEs in the corona with the disturbance seen later in the interplanetary medium. Both cannot be simply called CMEs, or confusion reigns. Thus arose the practice of using the term ICME for the interplanetary counterpart of a CME; e.g. [Lindsay et al., 1999; Mulligan et al., 1999a, b]. This term includes a wide variety of structures; in particular, structures missing one feature of a magnetic cloud, but clearly being associated with a CME on the Sun. While not every ICME detected has been identified with a specific CME, enough have that we can be confident of the association [e.g. Lindsay et al., 1999].

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Magnetic loop behind an interplanetary shock: Voyager, Helios, and IMP 8 observations

Cited by 1,503 publications

References 26 publications

Magnetic fields and plasmas in the inner heliosphere: Helios results

Magnetic fields and plasmas in the inner heliosphere: Helios results

Great geomagnetic storms in the rise and maximum of solar cycle 23

In defense of the term ICME

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