Artykuły w czasopismach: „Interplanetary science”

1

DONN, B. "Interplanetary Dust: Properties and Interactions of Interplanetary Dust." Science 233, no. 4764 (1986): 673. http://dx.doi.org/10.1126/science.233.4764.673.

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2

Exarhos, G., and X. Moussas. "On the heliolatitudinal variation of the galactic cosmic-ray intensity. Comparison with Ulysses measurements." Annales Geophysicae 21, no. 6 (2003): 1341–45. http://dx.doi.org/10.5194/angeo-21-1341-2003.

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Abstract. We study the dependence of cosmic rays with heliolatitude using a simple method and compare the results with the actual data from Ulysses and IMP spacecraft. We reproduce the galactic cosmic-ray heliographic latitudinal intensity variations, applying a semi-empirical, 2-D diffusion-convection model for the cosmic-ray transport in the interplanetary space. This model is a modification of our previous 1-D model (Exarhos and Moussas, 2001) and includes not only the radial diffusion of the cosmic-ray particles but also the latitudinal diffusion. Dividing the interplanetary region into "spherical magnetic sectors" (a small heliolatitudinal extension of a spherical magnetized solar wind plasma shell) that travel into the interplanetary space at the solar wind velocity, we calculate the cosmic-ray intensity for different heliographic latitudes as a series of successive intensity drops that all these "spherical magnetic sectors" between the Sun and the heliospheric termination shock cause the unmodulated galactic cosmic-ray intensity. Our results are compared with the Ulysses cosmic-ray measurements obtained during the first pole-to-pole passage from mid-1994 to mid-1995.Key words. Interplanetary physics (cosmic rays; interplanetray magnetic fields; solar wind plasma)

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3

Martin-Mur, T. J., G. L. Kruizinga, P. D. Burkhart, F. Abilleira, M. C. Wong, and J. A. Kangas. "Mars Science Laboratory Interplanetary Navigation." Journal of Spacecraft and Rockets 51, no. 4 (2014): 1014–28. http://dx.doi.org/10.2514/1.a32631.

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4

Martin-Mur, Tomas J., Gerard L. Kruizinga, and Mau C. Wong. "Mars science laboratory interplanetary navigaton analysis." Journal of Aerospace Engineering, Sciences and Applications 4, no. 2 (2012): 107–20. http://dx.doi.org/10.7446/jaesa.0402.10.

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5

Zweibel, E. G. "The Solar Wind: Interplanetary Magnetohydrodynamics." Science 272, no. 5261 (1996): 495b—496b. http://dx.doi.org/10.1126/science.272.5261.495b.

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6

CHRISTOFFERSEN, R., and P. R. BUSECK. "Refractory Minerals in Interplanetary Dust." Science 234, no. 4776 (1986): 590–92. http://dx.doi.org/10.1126/science.234.4776.590.

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7

ZOLENSKY, M. E. "Reports Refractory Interplanetary Dust Particles." Science 237, no. 4821 (1987): 1466–68. http://dx.doi.org/10.1126/science.237.4821.1466.

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8

Hand, Eric. "Interplanetary small satellites come of age." Science 361, no. 6404 (2018): 736–37. http://dx.doi.org/10.1126/science.361.6404.736.

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9

Watari, S., M. Vandas, and T. Watanabe. "Formation of a strong southward IMF near the solar maximum of cycle 23." Annales Geophysicae 22, no. 2 (2004): 673–87. http://dx.doi.org/10.5194/angeo-22-673-2004.

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Abstract. We analyzed observations of the solar activities and the solar wind parameters associated with large geomagnetic storms near the maximum of solar cycle 23. This analysis showed that strong southward interplanetary magnetic fields (IMFs), formed through interaction between an interplanetary disturbance, and background solar wind or between interplanetary disturbances are an important factor in the occurrence of intense geomagnetic storms. Based on our analysis, we seek to improve our understanding of the physical processes in which large negative Bz's are created which will lead to improving predictions of space weather. Key words. Interplanetary physics (Flare and stream dynamics; Interplanetary magnetic fields; Interplanetary shocks)

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10

Smith, D. E. "Two-Way Laser Link over Interplanetary Distance." Science 311, no. 5757 (2006): 53. http://dx.doi.org/10.1126/science.1120091.

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11

Hooke, Adrian. "The interplanetary Internet." Communications of the ACM 44, no. 9 (2001): 38–40. http://dx.doi.org/10.1145/383694.383703.

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12

Kalinichenko, M. M., N. V. Kuhai, O. O. Konovalenko, et al. "INVESTIGATIONS OF COSMIC SOURCES RADIOEMISSION SCINTILLATIONS DUE TO INTERPLANETARY PLASMA IRREGULARITIES AT THE INSTITUTE OF RADIO ASTRONOMY, NAS UKRAINE." Radio physics and radio astronomy 26, no. 2 (2021): 148–64. http://dx.doi.org/10.15407/rpra26.02.148.

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Purpose: Review of investigations of cosmic sources radioemission scintillations due to interplanetary plasma irregularities made at the Institute of Radio Astronomy of the National Academy of Sciences of Ukraine, from the first observations in the mid-70s until now. Design/methodology/approach: In the course of preparation of this paper, the authors have reviewed, analyzed and summarized the information being published in the home and foreign publications, and reported at scientific conferences. Findings: The investigations of the interplanetary scintillations carried out at the Institute of Radio Astronomy, NAS Ukraine have been reviewed. A retrospective discussion has been made on how in the course of these researches the knowledge about the basic parameters of interplanetary scintillations in the decameter wavelength range, as well as that on the important parameters of the solar wind and its structure, have been obtained. Also, various methods of processing and analysis of experimental data were offered, and new means for receiving cosmic radiation were created. The place and importance of the discussed researches for the world science are shown. Conclusions: Over the years since the beginning of the research, the think tank of the Department of Low-Frequency Radio Astronomy of the Institute of Radio Astronomy, NAS Ukraine has obtained a number of new relevant results, which bring Ukraine into the cohort of world centers of interplanetary scintillation researches. The construction of a new GURT radio telescope, among other things, creates new prospects for the development of this relevant line of investigation. Key words: interplanetary scintillations; decameter wavelength range; solar wind; solar wind stream structure; coronal mass ejection

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13

Craig, H. "Retention of Helium in Subducted Interplanetary Dust Particles." Science 265, no. 5180 (1994): 1892–93. http://dx.doi.org/10.1126/science.265.5180.1892.

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14

JOKIPII, J. R. "Cosmic Rays: Cosmic Rays In Interplanetary Magnetic Fields." Science 233, no. 4762 (1986): 483. http://dx.doi.org/10.1126/science.233.4762.483.

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15

Rossi, Bruno. "The Interplanetary Plasma." Annual Review of Astronomy and Astrophysics 29, no. 1 (1991): 1–9. http://dx.doi.org/10.1146/annurev.aa.29.090191.000245.

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16

Ballatore, P., J. P. Villain, N. Vilmer, and M. Pick. "The influence of the interplanetary medium on SuperDARN radar scattering occurrence." Annales Geophysicae 18, no. 12 (2000): 1576–83. http://dx.doi.org/10.1007/s00585-001-1576-2.

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Abstract. The effects of the characteristics of the interplanetary medium on the radar scattering occurrence, related to the whole array of SuperDARN radars installed in the Northern Hemisphere, have been studied over a two-year period. Statistically significant correlations of the variation of the scattering occurrence are found with the merging electric field and with the negative Bz component of the interplanetary magnetic field, independent of the seasonal period considered. This result demonstrates that the merging rate (and in particular the reconnection process) between the interplanetary magnetic field and the magnetosphere is a relevant factor affecting the occurrence of scattering. For comparison, we note that no statistically significant correlations are obtained when the interplanetary ion density or the solar wind speed are considered, although also these variables affect to a small degree the scattering occurrence variation. The study of the latitudinal and magnetic local time dependence of the observations shows an association between the considered correlation and the location of the auroral oval and the cusp/cleft region.Key words: Ionosphere (ionospheric irregularities) · Magnetospheric physics (solar wind-magnetosphere interactions) · Radio science (ionospheric physics)

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17

Janardhan, P., V. Balasubramanian, S. Ananthakrishnan, M. Dryer, A. Bhatnagar, and P. S. McIntosh. "Travelling interplanetary disturbances detected using interplanetary scintillation at 327 MHz." Solar Physics 166, no. 2 (1996): 379–401. http://dx.doi.org/10.1007/bf00149405.

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18

Vilmer, N., M. Pick, R. Schwenn, P. Ballatore, and J. P. Villain. "On the solar origin of interplanetary disturbances observed in the vicinity of the Earth." Annales Geophysicae 21, no. 4 (2003): 847–62. http://dx.doi.org/10.5194/angeo-21-847-2003.

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Abstract. The solar origin of 40 interplanetary disturbances observed in the vicinity of the Earth between January 1997 and June 1998 is investigated in this paper. Analysis starts with the establishment of a list of Interplanetary Mass Ejections or ICMEs (magnetic clouds, flux ropes and ejecta) and of Interplanetary Shocks measured at WIND for the period for which we had previously investigated the coupling of the interplanetary medium with the terrestrial ionospheric response. A search for associated coronal mass ejections (CMEs) observed by LASCO/SOHO is then performed, starting from an estimation of the transit time of the inter-planetary perturbation from the Sun to the Earth, assumed to be achieved at a constant speed (i.e. the speed measured at 1 AU). EIT/SOHO and Nançay Radioheliograph (NRH) observations are also used as proxies in this identification for the cases when LASCO observations do not allow one to firmly establish the association. The last part of the analysis concerns the identification of the solar source of the CMEs, performed using a large set of solar observations from X-ray to radio wavelengths. In the present study, this association is based on a careful examination of many data sets (EIT, NRH and H images and not on the use of catalogs and of Solar Geophysical Data reports). An association between inter-planetary disturbances and LASCO/CMEs or proxies on the disk is found for 36 interplanetary events. For 32 events, the solar source of activity can also be identified. A large proportion of cases is found to be associated with a flare signature in an active region, not excluding of course the involvement of a filament. Conclusions are finally drawn on the propagation of the disturbances in the interplanetary medium, the preferential association of disturbances detected close to the Earth’s orbit with halos or wide CMEs and the location on the solar disk of solar sources of the interplanetary disturbances during that period.Key words. Interplanetary physics (interplanetary shocks); solar physics, astrophysics and astronomy (flares and mass ejections)

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19

Lam, H. L., D. H. Boteler, and L. Trichtchenko. "Case studies of space weather events from their launching on the Sun to their impacts on power systems on the Earth." Annales Geophysicae 20, no. 7 (2002): 1073–79. http://dx.doi.org/10.5194/angeo-20-1073-2002.

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Abstract. Active geomagnetic conditions on 12–13, 15–16, and 22–23 September 1999 resulted in geomagnetically induced currents (GIC) measurable in power systems in Canada and the United States. Different solar origins for these three events gave rise to dissimilar interplanetary signatures. We used these events to present three case studies, each tracing an entire space weather episode from its inception on the Sun, propagation through the interplanetary medium, manifestation on the ground as intense magnetic and electric fluctuations, and its eventual impact on technological systems.Key words. Geomagnetism and paleomagnetism (rapid time variations) – Interplanetary physics (interplanetary magnetic fields) – Solar physics, astrophysics, and astronomy (flares and mass ejections)

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20

Bravo, S., and X. Blanco-Cano. "Signatures of interplanetary transients behind shocks and their associated near-surface solar activity." Annales Geophysicae 16, no. 4 (1998): 359–69. http://dx.doi.org/10.1007/s00585-998-0359-4.

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Abstract. Interplanetary transients with particular signatures different from the normal solar wind have been observed behind interplanetary shocks and also without shocks. In this paper we have selected four well-known transient interplanetary signatures, namely: magnetic clouds, helium enhancements and bidirectional electron and ion fluxes, found in the solar wind behind shocks, and undertaken a correlative study between them and the corresponding solar observations. We found that although commonly different signatures appear in a single interplanetary transient event, they are not necessarily simultaneous, that is, they may belong to different plasma regions within the ejecta, which suggests that they may be generated by complex processes involving the ejection of plasma from different solar regions. We also found that more than 90% of these signatures correspond to cases when an Hα flare and/or the eruption of a filament occurred near solar central meridian between 1 and 4 days before the observation of the disturbance at 1 AU, the highest association being with flares taking place between 2 and 3 days before. The majority of the Hα flares were also accompanied by soft X-ray events. We also studied the longitudinal distribution of the associated solar events and found that between 80% and 90% of the interplanetary ejecta were associated with solar events within a longitudinal band of ±30° from the solar central meridian. An east-west asymmetry in the associated solar events seems to exist for some of the signatures. We also look for coronal holes adjacent to the site of the explosive event and find that they were present almost in every case.Key words. Interplanetary physics · Interplanetary shocks · Solar wind plasma · Solar physics · Flares and mass ejections

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21

Bradley, J. "An Astronomical 2175 A Feature in Interplanetary Dust Particles." Science 307, no. 5707 (2005): 244–47. http://dx.doi.org/10.1126/science.1106717.

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22

von Hegner, Ian. "Interplanetary transmissions of life in an evolutionary context." International Journal of Astrobiology 19, no. 4 (2020): 335–48. http://dx.doi.org/10.1017/s1473550420000099.

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AbstractThe theory of lithopanspermia proposes the natural exchange of organisms between solar system bodies through meteorites. The focus of this theory comprises three distinct stages: planetary ejection, interplanetary transit and planetary entry. However, it is debatable whether organisms transported within the ejecta can survive all three stages. If the conjecture is granted, that life can indeed be safely transmitted from one world to another, then it is not only a topic pertaining to planetary science but also biological sciences. Hence, these stages are only the first three factors of the equation. The other factors for successful lithopanspermia are the quality, quantity and evolutionary strategy of the transmitted organisms. When expanding into new environments, invading organisms often do not survive in the first attempt and usually require several attempts through propagule pressure to obtain a foothold. There is a crucial difference between this terrestrial situation and the one brought about by lithopanspermia. While invasive species on Earth repeatedly enters a new habitat, a species pragmatically arrives on another solar system body only once; thus, an all-or-nothing response will be in effect. The species must survive in the first attempt, which limits the probability of survival. In addition, evolution sets a boundary through the existence of an inverse proportionality between the exchanges of life between two worlds, thus further restricting the probability of survival. However, terrestrial populations often encounter unpredictable and variable environmental conditions, which in turn necessitates an evolutionary response. Thus, one evolutionary mode in particular, bet hedging, is the evolutionary strategy that best smooth out this inverse proportionality. This is achieved by generating diversity even among a colony of genetically identical organisms. This variability in individual risk-taking increases the probability of survival and allows organisms to colonize more diverse environments. The present analysis to understand conditions relevant to a bacterial colony arriving in a new planetary environment provides a bridge between the theory of bet hedging, invasive range expansion and planetary science.

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23

Anttila, A., L. G. Kocharov, J. Torsti, and R. Vainio. "Long-duration high-energy proton events observed by GOES in October 1989." Annales Geophysicae 16, no. 8 (1998): 921–30. http://dx.doi.org/10.1007/s00585-998-0921-0.

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Abstract. We consider the prolonged injection of the high-energy (>10 MeV) protons during the three successive events observed by GOES in October 1989. We apply a solar-rotation-stereoscopy approach to study the injection of the accelerated particles from the CME-driven interplanetary shock waves in order to find out how the effectiveness of the particle acceleration and/or escape depends on the angular distance from the shock axis. We use an empirical model for the proton injection at the shock and a standard model of the interplanetary transport. The model can reproduce rather well the observed intensity–time profiles of the October 1989 events. The deduced proton injection rate is highest at the nose of the shock; the injection spectrum is always harder near the Sun. The results seem to be consistent with the scheme that the CME-driven interplanetary shock waves accelerate a seed particle population of coronal origin.Key words. Interplanetary physics · Energetic particles · Solar physics · astrophysics and astronomy · Flares and mass ejections

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24

Malandraki, O. E., E. T. Sarris, and G. Tsiropoula. "Magnetic topology of coronal mass ejection events out of the ecliptic: Ulysses/HI-SCALE energetic particle observations." Annales Geophysicae 21, no. 6 (2003): 1249–56. http://dx.doi.org/10.5194/angeo-21-1249-2003.

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Abstract. Solar energetic particle fluxes (Ee > 38 keV) observed by the ULYSSES/HI-SCALE experiment are utilized as diagnostic tracers of the large-scale structure and topology of the Interplanetary Magnetic Field (IMF) embedded within two well-identified Interplanetary Coronal Mass Ejections (ICMEs) detected at 56° and 62° south heliolatitudes by ULYSSES during the solar maximum southern high-latitude pass. On the basis of the energetic solar particle observations it is concluded that: (A) the high-latitude ICME magnetic structure observed in May 2000 causes a depression in the solar energetic electron intensities which can be accounted for by either a detached or an attached magnetic field topology for the ICME; (B) during the traversal of the out-of-ecliptic ICME event observed in July 2000 energetic electrons injected at the Sun are channeled by the ICME and propagate freely along the ICME magnetic field lines to 62° S heliolatitude.Key words. Interplanetary physics (energetic particles; interplanetary magnetic fields)

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25

Lanzerotti, L., T. Armstrong, R. Gold, et al. "Over the southern solar pole: low-energy interplanetary charged particles." Science 268, no. 5213 (1995): 1010–13. http://dx.doi.org/10.1126/science.7754378.

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Gurnett, D. A., W. S. Kurth, S. C. Allendorf, and R. L. Poynter. "Radio Emission from the Heliopause Triggered by an Interplanetary Shock." Science 262, no. 5131 (1993): 199–203. http://dx.doi.org/10.1126/science.262.5131.199.

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Clemett, S. J., C. R. Maechling, R. N. Zare, P. D. Swan, and R. M. Walker. "Identification of Complex Aromatic Molecules in Individual Interplanetary Dust Particles." Science 262, no. 5134 (1993): 721–25. http://dx.doi.org/10.1126/science.262.5134.721.

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Bradley, J. P. "Chemically Anomalous, Preaccretionally Irradiated Grains in Interplanetary Dust from Comets." Science 265, no. 5174 (1994): 925–29. http://dx.doi.org/10.1126/science.265.5174.925.

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29

HORD, C. W., C. A. BARTH, L. W. ESPOSITO, et al. "Galileo Ultraviolet Spectrometer Experiment: Initial Venus and Interplanetary Cruise Results." Science 253, no. 5027 (1991): 1548–50. http://dx.doi.org/10.1126/science.253.5027.1548.

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30

Colwell, J. E. "Capture of Interplanetary and Interstellar Dust by the Jovian Magnetosphere." Science 280, no. 5360 (1998): 88–91. http://dx.doi.org/10.1126/science.280.5360.88.

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31

Baxter, Stepen. "Fast Interplanetary Travel: a Literature Review." Journal of the British Interplanetary Society 76, no. 5 (2023): 163–69. http://dx.doi.org/10.59332/jbis-076-05-163.

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The project to which this paper is a contribution is a prospectus for the integrated industrial development of the Solar System. Fast transit on an interplanetary scale is a prerequisite before such a development can be established. To facilitate this freedom of movement, this study has defined a suite of fast, large-scale interplanetary ships, achievable in the relatively near term. As background, the present paper is a review of the literature on the feasibility of fast, large-scale, nuclear-powered, cargo carrying and/or crewed interplanetary craft, as explored historically from the development of atomic theory itself through to the application of modern fusion-technology high-performance propulsion systems. The study is part of the BIS SPACE (Study Project Advancing Colony Engineering) technical initiative. Keywords: BIS SPACE Project, Nuclear Powered Spaceship, Fast Interplanetary Ship, Project Daedalus, Project Icarus

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Baxter, Stephen. "Fast Interplanetary Travel: a Literature Review." Journal of the British Interplanetary Society 76, no. 5 (2023): 163–69. http://dx.doi.org/10.59332/jbis-076-05-0163.

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The project to which this paper is a contribution is a prospectus for the integrated industrial development of the Solar System. Fast transit on an interplanetary scale is a prerequisite before such a development can be established. To facilitate this freedom of movement, this study has defined a suite of fast, large-scale interplanetary ships, achievable in the relatively near term. As background, the present paper is a review of the literature on the feasibility of fast, large-scale, nuclear-powered, cargo-carrying and/or crewed interplanetary craft, as explored historically from the development of atomic theory itself through to the application of modern fusion-technology high-performance propulsion systems. The study is part of the BIS SPACE (Study Project Advancing Colony Engineering) technical initiative. Keywords: BIS SPACE Project, Nuclear Powered Spaceship, Fast Interplanetary Ship, Project Daedalus, Project Icarus

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33

Divine, Neil. "Five populations of interplanetary meteoroids." Journal of Geophysical Research 98, E9 (1993): 17029. http://dx.doi.org/10.1029/93je01203.

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Whang, Y. C. "Evolution of interplanetary slow shocks." Journal of Geophysical Research 93, A1 (1988): 251. http://dx.doi.org/10.1029/ja093ia01p00251.

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Cane, H. V. "The evolution of interplanetary shocks." Journal of Geophysical Research: Space Physics 90, A1 (1985): 191–97. http://dx.doi.org/10.1029/ja090ia01p00191.

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Marchese, Mario. "Interplanetary and pervasive communications." IEEE Aerospace and Electronic Systems Magazine 26, no. 2 (2011): 12–18. http://dx.doi.org/10.1109/maes.2011.5739484.

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Xiao, T., Q. Q. Shi, T. L. Zhang, et al. "Cluster-C1 observations on the geometrical structure of linear magnetic holes in the solar wind at 1 AU." Annales Geophysicae 28, no. 9 (2010): 1695–702. http://dx.doi.org/10.5194/angeo-28-1695-2010.

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Abstract. Interplanetary linear magnetic holes (LMHs) are structures in which the magnetic field magnitude decreases with little change in the field direction. They are a 10–30% subset of all interplanetary magnetic holes (MHs). Using magnetic field and plasma measurements obtained by Cluster-C1, we surveyed the LMHs in the solar wind at 1 AU. In total 567 interplanetary LMHs are identified from the magnetic field data when Cluster-C1 was in the solar wind from 2001 to 2004. We studied the relationship between the durations and the magnetic field orientations, as well as that of the scales and the field orientations of LMHs in the solar wind. It is found that the geometrical structure of the LMHs in the solar wind at 1 AU is consistent with rotational ellipsoid and the ratio of scales along and across the magnetic field is about 1.93:1. In other words, the structure is elongated along the magnetic field at 1 AU. The occurrence rate of LMHs in the solar wind at 1 AU is about 3.7 per day. It is shown that not only the occurrence rate but also the geometrical shape of interplanetary LMHs has no significant change from 0.72 AU to 1 AU in comparison with previous studies. It is thus inferred that most of interplanetary LMHs observed at 1 AU are formed and fully developed before 0.72 AU. The present results help us to study the formation mechanism of the LMHs in the solar wind.

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IPATOV, S. I., J. C. MATHER, and P. A. TAYLOR. "Migration of Interplanetary Dust." Annals of the New York Academy of Sciences 1017, no. 1 (2004): 66–80. http://dx.doi.org/10.1196/annals.1311.005.

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Watari, S., and T. Detman. "In situ local shock speed and transit shock speed." Annales Geophysicae 16, no. 4 (1998): 370–75. http://dx.doi.org/10.1007/s00585-998-0370-9.

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Abstract. A useful index for estimating the transit speeds was derived by analyzing interplanetary shock observations. This index is the ratio of the in situ local shock speed and the transit speed; it is 0.6–0.9 for most observed shocks. The local shock speed and the transit speed calculated for the results of the magnetohydrodynamic simulation show good agreement with the observations. The relation expressed by the index is well explained by a simplified propagation model assuming a blast wave. For several shocks the ratio is approximately 1.2, implying that these shocks accelerated during propagation in slow-speed solar wind. This ratio is similar to that for the background solar wind acceleration.Keywords. Interplanetary physics (Flare and stream dynamics; Interplanetary shocks; Solar wind plasma)

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40

Chashei, I. V., S. А. Tyul’bashev, and Yu V. Pisanko. "Monitoring of Interplanetary Scintillation and Potential of Short-time Space Weather Forecasting." Meteorologiya i Gidrologiya 3 (2021): 28–37. http://dx.doi.org/10.52002/0130-2906-2021-3-28-37.

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Observations and initial analysis of interplanetary scintillation data are briefly described in the framework of the program for the solar wind monitoring with the modernized LPI LPA radio telescope that started in 2014. The examples of detecting interplanetary coronal mass injections (ICME) and co-rotating interaction regions (СIR) of different-speed flows are presented. It is shown that in the first case, enhancements in the scintillation level in extended sounded regions of solar wind are observed 20–30 hours before the arrival of the disturbances to the Earth; in the second case, the evening and night scintillation level decrease is observed several days before the compressed region of disturbances comes to the Earth. These features are considered as a base of using interplanetary scintillation monitoring data for short-time space weather forecasting.

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Malandraki, O., E. T. Sarris, and P. Trochoutsos. "Probing the magnetic topology of coronal mass ejections by means of Ulysses/HI-SCALE energetic particle observations." Annales Geophysicae 18, no. 2 (2000): 129–40. http://dx.doi.org/10.1007/s00585-000-0129-4.

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Abstract. In this work, solar flare energetic particle fluxes (Ee ≥ 42 keV) observed by the HI-SCALE instrument onboard Ulysses, a spacecraft that is probing the heliosphere in 3-D, are utilized as diagnostics of the large-scale structure and topology of the interplanetary magnetic field (IMF) embedded within two well-identified interplanetary coronal mass ejection (ICME) structures. On the basis of the energetic solar flare particle observations firm conclusions are drawn on whether the detected ICMEs have been detached from the solar corona or are still magnetically anchored to it when they arrive at 2.5 AU. From the development of the angular distributions of the particle intensities, we have inferred that portions of the ICMEs studied consisted of both open and closed magnetic field lines. Both ICMEs present a filamentary structure comprising magnetic filaments with distinct electron anisotropy characteristics. Subsequently, we studied the evolution of the anisotropies of the energetic electrons along the magnetic field loop-like structure of one ICME and computed the characteristic decay time of the anisotropy which is a measure of the amount of scattering that the trapped electron population underwent after injection at the Sun.Key words: Interplanetary physics (energetic particles; interplanetary magnetic fields)

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Nielsen, E., and F. Honary. "Observations of ionospheric flows and particle precipitation following a Sudden Commencement." Annales Geophysicae 18, no. 8 (2000): 908–17. http://dx.doi.org/10.1007/s00585-000-0908-y.

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Abstract. On May 4, 1998, at 0227 UT an interplanetary shock crossed the WIND spacecraft, and half an hour later a Sudden Commencement occurred. Coinciding with the Sudden Commencement a rapid intensification of the flux of particle precipitation into the ionosphere was observed. Evidence is presented that the ionospheric electric fields were influenced by the associated dynamic variations of the ionospheric conductivities. Following the initial phase the ionospheric flow speeds increased rapidly over the next 20 min to more than 2000 m/s, in agreement with an increased effective coupling of the solar wind energy to the magnetosphere following the interplanetary shock that caused the Sudden Commencement. These strong flows were meandering in latitude, a type of plasma flow modulation that has been reported before to occur during Omega band events: a string of alternating field-aligned currents propagating eastward. The riometer absorption was found to be at a minimum in regions associated with outward directed field aligned currents. The riometer absorption regions (the regions of particle precipitation) were drifting with E × B drift speed of the ionospheric electrons.Key words: Interplanetary physics (interplanetary shocks) - Ionosphere (electric fields and currents) - Magnetospheric physics (energetic particles, precipitating)

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Feng, HengQiang, GuoQing Zhao, and JieMin Wang. "Small interplanetary magnetic flux rope." Science China Technological Sciences 63, no. 2 (2019): 183–94. http://dx.doi.org/10.1007/s11431-018-9481-1.

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Floss, C. "Carbon and Nitrogen Isotopic Anomalies in an Anhydrous Interplanetary Dust Particle." Science 303, no. 5662 (2004): 1355–58. http://dx.doi.org/10.1126/science.1093283.

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Reiner, M. J., J. Fainberg, and R. G. Stone. "Large-Scale Interplanetary Magnetic Field Configuration Revealed by Solar Radio Bursts." Science 270, no. 5235 (1995): 461–64. http://dx.doi.org/10.1126/science.270.5235.461.

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Kortenkamp, S. J. "A 100,000-Year Periodicity in the Accretion Rate of Interplanetary Dust." Science 280, no. 5365 (1998): 874–76. http://dx.doi.org/10.1126/science.280.5365.874.

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Yamakawa, Hiroshi. "Optimal Radially Accelerated Interplanetary Trajectories." Journal of Spacecraft and Rockets 43, no. 1 (2006): 116–20. http://dx.doi.org/10.2514/1.13317.

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Feynman, Joan, T. P. Armstrong, L. Dao-Gibner, and S. Silverman. "New interplanetary proton fluence model." Journal of Spacecraft and Rockets 27, no. 4 (1990): 403–10. http://dx.doi.org/10.2514/3.26157.

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Zubrin, Robert M., and Dana G. Andrews. "Magnetic sails and interplanetary travel." Journal of Spacecraft and Rockets 28, no. 2 (1991): 197–203. http://dx.doi.org/10.2514/3.26230.

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Garrett, Henry B., S. J. Drouilhet, John P. Oliver, and R. W. Evans. "Interplanetary Meteoroid Environment Model Update." Journal of Spacecraft and Rockets 36, no. 1 (1999): 124–32. http://dx.doi.org/10.2514/2.3424.

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