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  • 1
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    Online Resource
    Wave properties near the subsolar magnetopause: Pc 3–4 energy coupling for northward interplanetary magnetic field
    American Geophysical Union (AGU) ; 1993
    In:  Journal of Geophysical Research: Space Physics Vol. 98, No. A1 ( 1993-01), p. 187-196
    Details
    In: Journal of Geophysical Research: Space Physics, American Geophysical Union (AGU), Vol. 98, No. A1 ( 1993-01), p. 187-196
    Abstract: Strong slow mode waves in the Pc 3–4 frequency range are found in the magnetosheath close to the magnetopause. We have studied these waves at one of the ISEE subsolar magnetopause crossings using the magnetic field, electric field, and plasma measurements. We use the pressure balance at the magnetopause to calibrate the Fast Plasma Experiment data versus the magnetometer data. When we perform such a calibration and renonnalization, we find that the slow mode structures are not in pressure balance and small scale fluctuations in the total pressure still remain in the Pc 3–4 range. Energy in the total pressure fluctuations can be transmitted through the magnetopause by boundary motions. The Poynting flux calculated from the electric and magnetic field measurements suggests that a net Poynting flux is transmitted into the magnetopause. The two independent measurements show a similar energy transmission coefficient. The transmitted energy flux is about 18% of the magnetic energy flux of the waves in the magnetosheath. Part of this transmitted energy is lost in the sheath transition layer before it enters the closed field line region. The waves reaching the boundary layer decay rapidly. Little wave power is transmitted into the magnetosphere.
    Type of Medium: Online Resource
    ISSN: 0148-0227
    URL: Article
    DOI: 10.1029/92JA01534
    Language: English
    Publisher: American Geophysical Union (AGU)
    Publication Date: 1993
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  • 2
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    Particle and field characteristics of the high‐latitude plasma sheet boundary layer
    American Geophysical Union (AGU) ; 1984
    In:  Journal of Geophysical Research: Space Physics Vol. 89, No. A10 ( 1984-10), p. 8885-8906
    Details
    In: Journal of Geophysical Research: Space Physics, American Geophysical Union (AGU), Vol. 89, No. A10 ( 1984-10), p. 8885-8906
    Abstract: Particle and field data obtained by eight ISEE spacecraft experiments are used to define more precisely the characteristics of the high‐latitude boundary region of the plasma sheet. We find that there is a region immediately adjacent to the high‐latitude plasma sheet boundary whose particle and field characteristics are distinctly different from its neighbors, the lobe and the plasma sheet. This region supports intense ion flows, field‐aligned currents, large amplitude electric fields, and enhanced broad band electrostatic noise. A detailed analysis of events detected on April 19, 1978, shows that the plasma distributions in the region are unstable. For instance, bidirectional field‐aligned electron distributions are observed at nearly all energies (a few electron volts to a few hundred keV). Both the differential energy spectra and the reduced distribution function F (υ ∥ ) = 2π∫υ ⊥ f (υ ∥ , υ ⊥ ) d υ ⊥ show significant peaks at 100‐400 eV. These peaks comprise electrons coming from the earthward direction. Ions below a few keV are convected in the direction perpendicular to B , whereas the higher energy ions ( 〉 30 keV) are field‐aligned and travelling mainly toward the earth. The electric field in the region is intense, spiky, and possibly time varying. The magnetic B y component increases dramatically from a few nanoteslas to more than 20 nT, indicating presence of a field‐aligned current. These features are in contrast with the plasma characteristics outside the region. In the adjacent regions (closer to the lobe and the inner plasma sheet regions), the electron distributions are nearly isotropic. Ion flow is virtually at a standstill. The high‐energy ions ( 〉 30 keV) are anisotropic and field‐aligned but bidirectional.
    Type of Medium: Online Resource
    ISSN: 0148-0227
    URL: Article
    DOI: 10.1029/JA089iA10p08885
    Language: English
    Publisher: American Geophysical Union (AGU)
    Publication Date: 1984
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  • 3
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    A magnetic cloud containing prominence material: January 1997
    American Geophysical Union (AGU) ; 1998
    In:  Journal of Geophysical Research: Space Physics Vol. 103, No. A1 ( 1998-01), p. 277-285
    Details
    In: Journal of Geophysical Research: Space Physics, American Geophysical Union (AGU), Vol. 103, No. A1 ( 1998-01), p. 277-285
    Abstract: This work discusses the relations among (1) an interplanetary force‐free magnetic cloud containing a plug of cold high‐density material with unusual composition, (2) a coronal mass ejection (CME), (3) an eruptive prominence, and (4) a model of prominence material supported by a force‐free magnetic flux rope in a coronal streamer. The magnetic cloud moved past the Wind spacecraft located in the solar wind upstream of Earth on January 10 and 11, 1997. The magnetic field configuration in the magnetic cloud was approximately a constant‐α, force‐free flux rope. The 4 He ++ /H + abundance in the most of the magnetic cloud was similar to that of the streamer belt material, suggesting an association between the magnetic cloud and a helmet streamer. A very cold region of exceptionally high density was detected at the rear of the magnetic cloud. This dense region had an unusual composition, including (1) a relatively high (10%) 4 He ++ /He + abundance (indicating a source near the photosphere), and (2) 4 He + , with an abundance relative to 4 He ++ of ∼1%, and the unusual charge states of O 5+ and Fe 5+ (indicating a freezing‐in temperature of (1.6–4.0) × 10 5 °K, which is unusually low, but consistent with that expected for prominence material). Thus we suggest that the high‐density region might be prominence material. The CME was seen in the solar corona on January 6, 1997, by the large angle and spectrometric coronagraph (LASCO) instrument on SOHO shortly after an eruptive prominence. A helmet streamer was observed near the latitude of the eruptive prominence a quarter of a solar rotation before and after the eruptive prominence. These observations are consistent with recent models, including the conceptual model of Low and Hundhausen [1995] for a quasi‐static helmet streamer containing a force‐free flux rope which supports prominence material and the dynamical model of Wu et al. [1997] for CMEs produced by the disruption of such a configuration.
    Type of Medium: Online Resource
    ISSN: 0148-0227
    URL: Article
    DOI: 10.1029/97JA02768
    Language: English
    Publisher: American Geophysical Union (AGU)
    Publication Date: 1998
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  • 4
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    Counterstreaming ion events in the magnetosphere
    American Geophysical Union (AGU) ; 1987
    In:  Journal of Geophysical Research: Space Physics Vol. 92, No. A12 ( 1987-12), p. 13523-13536
    Details
    In: Journal of Geophysical Research: Space Physics, American Geophysical Union (AGU), Vol. 92, No. A12 ( 1987-12), p. 13523-13536
    Abstract: Counterstreaming ions or ions traveling simultaneously both parallel and antiparallel to the magnetic field direction have been briefly noted in the literature but have not been studied previously in depth. We have studied over 60 counterstreaming ion (CSI) events observed on the ISEE 1 satellite. Often, both oxygen and hydrogen ions at a number of energy levels are Counterstreaming, but some events show only either oxygen or hydrogen ions at one or more energy levels involved. One particularly interesting event shows only counterstreaming oxygen ions with 417 eV energy; oxygen ions of lower energy (215 eV) and higher energy (630–17,000 eV) and all the hydrogen ions between 215 and 17,000 eV energy have lower fluxes and/or nearly isotropic pitch angle distributions. This event correlates well with wave activity in the 17‐ to 100‐Hz band and is also accompanied by 200‐eV downgoing and 400‐eV upgoing electrons. Details of this and some other CSI events are presented. The CSI events were found to occur at altitudes of about 2–8 R E on L shells of about 5–12 in the evening‐to‐morning sector from about 1700 to 0900 LT; the majority of the CSI events at altitudes between 2 and 5 R E and L values from 5 to 8 involve oxygen ions, while at higher altitudes from about 5 to 8 R E and higher L values from about 8 to 12 the majority involve hydrogen ions. Some features suggest wave‐particle interaction may be involved in some CSI events.
    Type of Medium: Online Resource
    ISSN: 0148-0227
    URL: Article
    DOI: 10.1029/JA092iA12p13523
    Language: English
    Publisher: American Geophysical Union (AGU)
    Publication Date: 1987
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  • 5
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    Widely spaced wave‐particle observations during GEOTAIL and Wind magnetic conjunctions in the Earth's ion foreshock with near‐radial interplanetary magnetic field
    American Geophysical Union (AGU) ; 1999
    In:  Journal of Geophysical Research: Space Physics Vol. 104, No. A1 ( 1999-01), p. 463-482
    Details
    In: Journal of Geophysical Research: Space Physics, American Geophysical Union (AGU), Vol. 104, No. A1 ( 1999-01), p. 463-482
    Abstract: Several events have been identified of an ion foreshock extending up to 250 RE upstream of the Earth. These events occur mostly during periods of slowly drifting radial interplanetary magnetic field (IMF) when the 1‐min average values of the strengths of the IMF and the solar wind (SW) speeds are mostly steady. For their analysis an analytical solution to the problem of the closest approach of an IMF line to two spacecraft is given. We used this method to find intervals of magnetic conjunction between the bow shock and the upstream regions at GEOTAIL and Wind. This solution is obtained by determining the minimum angle θ (as a function of time) between the mean direction of the IMF (measured at Wind) and the vector‐difference (rWI‐r) of the locations of Wind and the point (attached on the field line) which went earlier by GEOTAIL. Here we take into account the mean drift of the flux lines with the SW, by assuming that the spacecraft were located in the same heliospheric magnetic domain. We have tested this method against a set of selected cases which show a steady presence of the ion foreshock close to the bow shock (GEOTAIL) and its sporadic presence far upstream (Wind). We have found our method to be accurate within a few Earth radii (RE). We have identified an outstanding candidate for the bow shock, GEOTAIL, and Wind sequential magnetic conjunction, which occurred on June 11, 1995. Additionally, this diagnostic technique has been applied to nine more intervals of simultaneous occurrences of intensity enhancements of broadband ultralow‐frequency (ULF) waves, and fluctuating fluxes of scattered energetic ions (40–140 keV). Very broad ion foreshock regions ( 〉 40 RE) are commonly observed during the subset of events characterized by a high‐speed SW. The observed frequencies of the ULF waves are basically enhanced transversal modes in the range from ∼ 1/10 to 2/3 of proton cyclotron frequency, f cp . Fluctuations in the energetic ion fluxes were also observed in this frequency range for all the cases. Therefore we argue that the nature of the coupling between ULF waves and energetic ions is similar both in the near as well as far upstream regions of the Earth's bow shock.
    Type of Medium: Online Resource
    ISSN: 0148-0227
    URL: Article
    DOI: 10.1029/1998JA900018
    Language: English
    Publisher: American Geophysical Union (AGU)
    Publication Date: 1999
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  • 6
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    Reconnection remnants in the magnetic cloud of October 18–19, 1995: A shock, monochromatic wave, heat flux dropout, and energetic ion beam
    American Geophysical Union (AGU) ; 2001
    In:  Journal of Geophysical Research: Space Physics Vol. 106, No. A8 ( 2001-08), p. 15985-16000
    Details
    In: Journal of Geophysical Research: Space Physics, American Geophysical Union (AGU), Vol. 106, No. A8 ( 2001-08), p. 15985-16000
    Abstract: Evidence is presented that the Wind spacecraft observed particle and field signatures on October 18–19, 1995, due to reconnection near the foot points of a magnetic cloud (i.e., between 1 and 5 solar radii). These signatures include (1) an internal shock traveling approximately along the axis of the magnetic cloud, (2) a simple compression of the magnetic field consistent with the foot point magnetic fields being thrust outward at speeds much greater than the solar wind speed, (3) an electron heat flux dropout occurring within minutes of the shock, indicating a topological change resulting from disconnection from the solar surface, (4) a very cold 5 keV proton beam, and (5) an associated monochromatic wave. We expect that given observations of enough magnetic clouds, Wind and other spacecraft will see signatures similar to the ones reported here indicating reconnection. However, these observations require the spacecraft to be fortuitously positioned to observe the passing shock and other signatures and will therefore be associated with only a small fraction of magnetic clouds. Consistent with this, a few magnetic clouds observed by Wind have been found to possess internal shock waves.
    Type of Medium: Online Resource
    ISSN: 0148-0227
    URL: Article
    DOI: 10.1029/2000JA000101
    Language: English
    Publisher: American Geophysical Union (AGU)
    Publication Date: 2001
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  • 7
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    Radio observations of interplanetary magnetic field structures out of the ecliptic
    Springer Science and Business Media LLC ; 1977
    In:  Solar Physics Vol. 52, No. 2 ( 1977-5), p. 477-484
    Details
    In: Solar Physics, Springer Science and Business Media LLC, Vol. 52, No. 2 ( 1977-5), p. 477-484
    Type of Medium: Online Resource
    ISSN: 0038-0938 , 1573-093X
    URL: Article
    DOI: 10.1007/BF00149662
    Language: English
    Publisher: Springer Science and Business Media LLC
    Publication Date: 1977
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  • 8
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    Interplanetary baseline observations of type III solar radio bursts
    Springer Science and Business Media LLC ; 1977
    In:  Solar Physics Vol. 54, No. 2 ( 1977-10), p. 431-439
    Details
    In: Solar Physics, Springer Science and Business Media LLC, Vol. 54, No. 2 ( 1977-10), p. 431-439
    Type of Medium: Online Resource
    ISSN: 0038-0938 , 1573-093X
    URL: Article
    DOI: 10.1007/BF00159934
    Language: English
    Publisher: Springer Science and Business Media LLC
    Publication Date: 1977
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  • 9
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    Structure and properties of the subsolar magnetopause for northward interplanetary magnetic field: Multiple‐instrument particle observations
    American Geophysical Union (AGU) ; 1993
    In:  Journal of Geophysical Research: Space Physics Vol. 98, No. A7 ( 1993-07), p. 11319-11337
    Details
    In: Journal of Geophysical Research: Space Physics, American Geophysical Union (AGU), Vol. 98, No. A7 ( 1993-07), p. 11319-11337
    Abstract: The structure and properties of the subsolar magnetopause for northward interplanetary magnetic feild (IMF) are studied with measurements from 10 different instruments for three ISEE crossings. Data show that the overall structure and properties are similar for the three crossings, indicating the magnetopause is relatively well determined in the subsolar region for strongly northward IMF. The measurements from different instruments are consistent with each other and complementary based on the current knowledge of space plasma physics. The combined data set suggests that the magnetopause region is best organized by defining a sheath transition layer and steplike boundary layers. The sheath transition layer contains mostly magnetosheath particles. The magnetosheath, magnetospheric, and ionospheric populations are mixed in the interior boundary layers. This result, which is consistent with previous studies, is now supported by observations of a much broader spectrum of measurements including three‐dimensional electron, energetic particle, heavy ion and plasma wave. Some new features are also found: even for quiet subsolar magnetopause crossings, transient or small‐scale structures still occur sporadically; slight heating may occur in the boundary layers. Some outstanding issues are clarified by this study: the electron flux enhancements in the lowest energies in the boundary layers and magnetosphere are ionospheric electrons and not photoelectrons from the spacecraft; for northward IMF, they are photoelectrons, but for southward IMF they may be secondary electrons; and the density measurements from differential and integral techniques are similar, leaving no room for a significant “invisible” population.
    Type of Medium: Online Resource
    ISSN: 0148-0227
    URL: Article
    DOI: 10.1029/93JA00606
    Language: English
    Publisher: American Geophysical Union (AGU)
    Publication Date: 1993
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  • 10
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    Sector boundary transformation by an open magnetic cloud
    American Geophysical Union (AGU) ; 1998
    In:  Journal of Geophysical Research: Space Physics Vol. 103, No. A11 ( 1998-11), p. 26859-26868
    Details
    In: Journal of Geophysical Research: Space Physics, American Geophysical Union (AGU), Vol. 103, No. A11 ( 1998-11), p. 26859-26868
    Abstract: A magnetic cloud observed by the Wind spacecraft on February 8, 1995, was remarkable for its impact on the interplanetary sector structure. The magnetic field data imply that the cloud occurred in the middle of a sector and that the arrival of the following sector boundary on February 10 coincided with the arrival time predicted from the corresponding source surface map. The electron heat flux data, however, give incontrovertible evidence that instead the cloud brought the sector boundary, well ahead of the predicted arrival time. The electron heat flux data show little counterstreaming within the cloud, indicating predominantly open helical field lines. Under the assumption that the cloud originally had the form of a closed flux rope loop with legs rooted to the Sun, observational constraints dictate that the sector boundary was displaced not because it was pushed aside by the cloud but because reconnection in the leading leg opened field lines there, creating a topological change spanning 45° of heliographic longitude. The solar source of the cloud was deduced from an associated eruptive arcade event extending northeastward from an active region in Yohkoh soft X ray data on February 4. On February 8, the same active region was the source of impulsive energetic electron events observed at Wind during a brief counterstreaming interval, consistent with magnetic connection in the leading leg at that time. The cloud's helicity matches that predicted from the skew of the arcade fields in the February 4 X ray event, but the predicted alignment of the arcade and cloud axes was off by 35°. We use an MHD model with boundary conditions derived from solar magnetograms to illustrate the tilted arcade configuration in the corona that gave rise to the magnetic cloud and the lesser tilt of the heliospheric current sheet stemming from it.
    Type of Medium: Online Resource
    ISSN: 0148-0227
    URL: Article
    DOI: 10.1029/98JA02391
    Language: English
    Publisher: American Geophysical Union (AGU)
    Publication Date: 1998
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