Relevant bibliographies by topics / Planetary science (excl. solar system and planetary geology)

Academic literature on the topic 'Planetary science (excl. solar system and planetary geology)'

Author: Grafiati
Published: 10 December 2022
Last updated: 28 January 2023

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Consult the lists of relevant articles, books, theses, conference reports, and other scholarly sources on the topic 'Planetary science (excl. solar system and planetary geology).'

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Journal articles on the topic "Planetary science (excl. solar system and planetary geology)"

1

Sun, Wei, Jian Wang, JinRu Chen, Ying Wang, GuangMing Yu, and XianHai Xu. "Contrast analysis between the trajectory of the planetary system and the periodicity of solar activity." Annales Geophysicae 35, no. 3 (May 17, 2017): 659–69. http://dx.doi.org/10.5194/angeo-35-659-2017.

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Abstract. The relationship between the periodic movement of the planetary system and its influence on solar activity is currently a serious topic in research. The kinematic index of the planet juncture index has been developed to find the track and variation of the Sun around the centroid of the solar system and the periodicity of solar activity. In the present study, the kinematic index of the planetary system's heliocentric longitude, developed based on the orbital elements of planets in the solar system, and it is used to investigate the periodic movement of the planetary system. The kinematic index of the planetary system's heliocentric longitude and that of the planet juncture index are simulated and analyzed. The numerical simulation of the two kinematic indexes shows orderly orbits and disorderly orbits of 49.9 and 129.6 years, respectively. Two orderly orbits or two disorderly orbits show a period change rule of 179.5 years. The contrast analysis between the periodic movement of the planetary system and the periodicity of solar activity shows that the two phenomena exhibit a period change rule of 179.5 years. Moreover, orderly orbits correspond to high periods of solar activity and disorderly orbits correspond to low periods of solar activity. Therefore, the relative movement of the planetary system affects solar activity to some extent. The relationship provides a basis for discussing the movement of the planetary system and solar activity.
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Kobayashi, Hiroshi, Hiroshi Kimura, Satoru Yamamoto, Sei-ichiro Watanabe, and Tetsuo Yamamoto. "Ice sublimation of dust particles and their detection in the outer solar system." Earth, Planets and Space 62, no. 1 (January 2010): 57–61. http://dx.doi.org/10.5047/eps.2009.03.001.

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Uchida, Tomohisa, Hiroyuki K. M. Tanaka, and Manobu Tanaka. "Development of a muon radiographic imaging electronic board system for a stable solar power operation." Earth, Planets and Space 62, no. 2 (February 2010): 167–72. http://dx.doi.org/10.5047/eps.2009.03.002.

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Yeghikyan, A. G., and H. J. Fahr. "Consequences of the Solar System passage through dense interstellar clouds." Annales Geophysicae 21, no. 6 (June 30, 2003): 1263–73. http://dx.doi.org/10.5194/angeo-21-1263-2003.

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Abstract. Several consequences of the passage of the solar system through dense interstellar molecular clouds are discussed. These clouds, dense (more than 100 cm-3), cold (10–50 K) and extended (larger than 1 pc), are characterized by a gas-to-dust mass ratio of about 100, by a specific power grain size spectrum (grain radii usually cover the range 0.001–3 micron) and by an average dust-to-gas number density ratio of about 10-12. Frequently these clouds contain small-scale (10–100 AU) condensations with gas concentrations ranging up to 10 5 cm-3. At their casual passage over the solar system they exert pressures very much enhanced with respect to today’s standards. Under these conditions it will occur that the Earth is exposed directly to the interstellar flow. It is shown first that even close to the Sun, at 1 AU, the cloud’s matter is only partly ionized and should mainly interact with the solar wind by charge exchange processes. Dust particles of the cloud serve as a source of neutrals, generated by the solar UV irradiation of dust grains, causing the evaporation of icy materials. The release of neutral atoms from dust grains is then followed by strong influences on the solar wind plasma flow. The behavior of the neutral gas inflow parameters is investigated by a 2-D hydrodynamic approach to model the interaction processes. Because of a reduction of the heliospheric dimension down to 1 AU, direct influence of the cloud’s matter to the terrestrial environment and atmosphere could be envisaged.Key words. Interplanetary physics (heliopause and solar wind termination; interplanetary dust; interstellar gas)
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Tveito, Torbjørn, Juha Vierinen, Björn Gustavsson, and Viswanathan Lakshmi Narayanan. "Planetary radar science case for EISCAT 3D." Annales Geophysicae 39, no. 3 (May 12, 2021): 427–38. http://dx.doi.org/10.5194/angeo-39-427-2021.

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Abstract. Ground-based inverse synthetic aperture radar is a tool that can provide insights into the early history and formative processes of planetary bodies in the inner solar system. This information is gathered by measuring the scattering matrix of the target body, providing composite information about the physical structure and chemical makeup of its surface and subsurface down to the penetration depth of the radio wave. This work describes the technical capabilities of the upcoming 233 MHz European Incoherent Scatter Scientific Association (EISCAT) 3D radar facility for measuring planetary surfaces. Estimates of the achievable signal-to-noise ratios for terrestrial target bodies are provided. While Venus and Mars can possibly be detected, only the Moon is found to have sufficient signal-to-noise ratio to allow high-resolution mapping to be performed. The performance of the EISCAT 3D antenna layout is evaluated for interferometric range–Doppler disambiguation, and it is found to be well suited for this task, providing up to 20 dB of separation between Doppler northern and southern hemispheres in our case study. The low frequency used by EISCAT 3D is more affected by the ionosphere than higher-frequency radars. The magnitude of the Doppler broadening due to ionospheric propagation effects associated with traveling ionospheric disturbances has been estimated. The effect is found to be significant but not severe enough to prevent high-resolution imaging. A survey of lunar observing opportunities between 2022 and 2040 is evaluated by investigating the path of the sub-radar point when the Moon is above the local radar horizon. During this time, a good variety of look directions and Doppler equator directions are found, with observations opportunities available for approximately 10 d every lunar month. EISCAT 3D will be able to provide new, high-quality polarimetric scattering maps of the nearside of the Moon with the previously unused wavelength of 1.3 m, which provides a good compromise between radio wave penetration depth and Doppler resolution.
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Jakowski, N., and H. D. Bettac. "Proposal for an ionosphere/plasmasphere monitoring system." Annales Geophysicae 12, no. 5 (April 30, 1994): 431–37. http://dx.doi.org/10.1007/s00585-994-0431-7.

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Abstract. A space-based satellite system suited for long-term monitoring of the Earth's ionosphere/plasmasphere systems is proposed. The monitoring system consists of a network of radio beacon satellites capable of measuring the ionospheric and plasmaspheric electron content on a continuous base with high time resolution. It takes advantage of the geometrical relationship between the orbit of geostationary satellites and the position of the plasmapause region characterized by a steep electron density gradient. A combination of geostationary and nongeostationary satellites may explore the three-dimensional structure of the plasmasphere. Taking into account plasmaspheric characteristics some criteria for an effective arrangement of the satellites are derived and discussed. Since the plasmapause position is very sensitive to changes or distortions in the solar wind and the related geomagnetic activity, a continuous monitoring of the position of the plasmapause would be helpful in understanding solar-terrestrial relationships.
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Prikryl, Paul, Vojto Rušin, Emil A. Prikryl, Pavel Šťastný, Maroš Turňa, and Martina Zeleňáková. "Heavy rainfall, floods, and flash floods influenced by high-speed solar wind coupling to the magnetosphere–ionosphere–atmosphere system." Annales Geophysicae 39, no. 4 (August 27, 2021): 769–93. http://dx.doi.org/10.5194/angeo-39-769-2021.

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Abstract. Heavy rainfall events causing floods and flash floods are examined in the context of solar wind coupling to the magnetosphere–ionosphere–atmosphere system. The superposed epoch (SPE) analyses of solar wind variables have shown the tendency of severe weather to follow arrivals of high-speed streams from solar coronal holes. Precipitation data sets based on rain gauge and satellite sensor measurements are used to examine the relationship between the solar wind high-speed streams and daily precipitation rates over several midlatitude regions. The SPE analysis results show an increase in the occurrence of high precipitation rates following arrivals of high-speed streams, including recurrence with a solar rotation period of 27 d. The cross-correlation analysis applied to the SPE averages of the green (Fe XIV; 530.3 nm) corona intensity observed by ground-based coronagraphs, solar wind parameters, and daily precipitation rates show correlation peaks at lags spaced by solar rotation period. When the SPE analysis is limited to years around the solar minimum (2008–2009), which was dominated by recurrent coronal holes separated by ∼ 120∘ in heliographic longitude, significant cross-correlation peaks are found at lags spaced by 9 d. These results are further demonstrated by cases of heavy rainfall, floods and flash floods in Europe, Japan, and the USA, highlighting the role of solar wind coupling to the magnetosphere–ionosphere–atmosphere system in severe weather, mediated by aurorally excited atmospheric gravity waves.
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Gallagher, P. T., C. Denker, V. Yurchyshyn, T. Spirock, J. Qiu, H. Wang, and P. R. Goode. "Solar activity monitoring and forecasting capabilities at Big Bear Solar Observatory." Annales Geophysicae 20, no. 7 (July 31, 2002): 1105–15. http://dx.doi.org/10.5194/angeo-20-1105-2002.

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Abstract. The availability of full-disk, high-resolution Ha images from Big Bear Solar Observatory (USA), Kanzelhöhe Solar Observatory (Austria), and Yunnan Astronomical Observatory (China) allows for the continual monitoring of solar activity with unprecedented spatial and temporal resolution. Typically, this Global Ha Network (GHN) provides almost uninterrupted Ha images with a cadence of 1 min and an image scale of 1'' per pixel. Every hour, GHN images are transferred to the web-based BBSO Active Region Monitor (ARM; www.bbso.njit.edu/arm), which includes the most recent EUV, continuum, and magnetogram data from the Solar and Heliospheric Observatory, together with magnetograms from the Global Oscillation Network Group. ARM also includes a variety of active region properties from the National Oceanic and Atmospheric Administration’s Space Environment Center, such as up-to-date active region positions, GOES 5-min X-ray data, and flare identification. Stokes I, V, Q, and U images are available from the recently operational BBSO Digital Vector Magnetograph and the Vector Magnetograph at the Huairou Solar Observing Station of Beijing Observatory. Vector magnetograms provide complete information on the photospheric magnetic field, and allow for magnetic flux gradients, electric currents, and shear forces to be calculated: these measurements are extremely sensitive to conditions resulting in flaring activity. Furthermore, we have developed a Flare Prediction System which estimates the probability for each region to produce C-, M-, or X-class flares based on nearly eight years of NOAA data from cycle 22. This, in addition to BBSO’s daily solar activity reports, has proven a useful resource for activity forecasting.Key words. Solar physics, astronomy and astrophysics (flares and mass ejections; instruments and techniques; photosphere and chromosphere)
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TSUCHIYAMA, Akira, and Junya MATSUNO. "Using Mineral Science to Elucidate Mysteries of the Early Solar System." Journal of Geography (Chigaku Zasshi) 131, no. 2 (April 25, 2022): 193–211. http://dx.doi.org/10.5026/jgeography.131.193.

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Lopez, R. E., V. G. Merkin, and J. G. Lyon. "The role of the bow shock in solar wind-magnetosphere coupling." Annales Geophysicae 29, no. 6 (June 25, 2011): 1129–35. http://dx.doi.org/10.5194/angeo-29-1129-2011.

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Abstract. In this paper we examine the role of the bow shock in coupling solar wind energy to the magnetosphere using global magnetohydrodynamic simulations of the solar wind-magnetosphere interaction with southward IMF. During typical solar wind conditions, there are two significant dynamo currents in the magnetospheric system, one in the high-latitude mantle region tailward of the cusp and the other in the bow shock. As the magnitude of the (southward) IMF increases and the solar wind becomes a low Mach number flow, there is a significant change in solar wind-magnetosphere coupling. The high-latitude magnetopause dynamo becomes insignificant compared to the bow shock and a large load appears right outside the magnetopause. This leaves the bow shock current as the only substantial dynamo current in the system, and the only place where a significant amount of mechanical energy is extracted from the solar wind. That energy appears primarily as electromagnetic energy, and the Poynting flux generated at the bow shock feeds energy back into the plasma, reaccelerating it to solar wind speeds. Some small fraction of that Poynting flux is directed into the magnetosphere, supplying the energy needed for magnetospheric dynamics. Thus during periods when the solar wind flow has a low Mach number, the main dynamo in the solar wind-magnetosphere system is the bow shock.
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Dissertations / Theses on the topic "Planetary science (excl. solar system and planetary geology)"

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"Early Solar System Processes and Parent Body Relationships Recorded by Chromium and Titanium Isotopes in Meteorites." Doctoral diss., 2020. http://hdl.handle.net/2286/R.I.62701.

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abstract: Meteorites and their components can be used to unravel the history of the early Solar System. Carbonaceous chondrites are meteorites that originated from undifferentiated parent bodies that formed within a few million years of the beginning of the Solar System. These meteorites contain calcium-aluminum-rich inclusions (CAIs), which are the oldest dated solids in the Solar System at ~4.567 billion years old and thus preserve a record of the earliest stage of Solar System formation. The isotopic compositions of CAIs and bulk carbonaceous chondrites can be used to identify the sources of material inherited by the protoplanetary disk, assess the degree of mixing in the disk, and evaluate sample origins and potential genetic relationships between parent bodies. In particular, mass-independent Cr and Ti isotopic compositions have proven to be especially useful for these purposes. In this work, I first developed new methods for the chemical separation of Cr and Ti, improving the reliability of existing methods to ensure consistent yields and accurate isotopic measurements. I then measured the Cr and Ti isotopic compositions of CAIs from CV and CK chondrites to determine the extent of isotopic heterogeneity in the CAI-forming region and assess the role of CAIs in the preservation of planetary-scale isotopic anomalies. My results show that all measured CAIs originated from a common isotopic reservoir that incorporated material from at least three distinct nucleosynthetic sources and preserved limited isotopic heterogeneity. These results also suggest that planetary-scale isotopic anomalies cannot be attributed solely to the transport of CAIs from one part of the solar nebula to another. I finally measured the Cr and Ti isotopic compositions of bulk CM, CO, and ungrouped chondrites to evaluate the relationship between CM and CO chondrites, which have been suggested to originate from either distinct but related parent bodies or a common compositionally heterogeneous parent body. My results suggest that CM, CO, and related ungrouped chondrites originated from distinct parent bodies that formed from similar precursor materials in nearby formation regions. These results may have implications for asteroid samples returned by the OSIRIS-REx and Hayabusa2 missions.
Dissertation/Thesis
Doctoral Dissertation Geological Sciences 2020
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Books on the topic "Planetary science (excl. solar system and planetary geology)"

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M, Mensing Teresa, ed. Introduction to planetary science: The geological perspective. Dordrecht: Springer, 2007.

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1961-, Stofan Ellen Renee, ed. Planetology: How Earth is unlocking the secrets of the solar system. Washington, D.C: National Geographic, 2008.

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Mensing, Teresa M., and Gunter Faure. Introduction to Planetary Science. Springer, 2008.

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Mensing, Teresa M., and Gunter Faure. Introduction to Planetary Science: The Geological Perspective. Springer, 2016.

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Mensing, Teresa M., and Gunter Faure. Introduction to Planetary Science: The Geological Perspective. Springer London, Limited, 2007.

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Fundamental Planetary Science Physics Chemistry And Habitability. Cambridge University Press, 2013.

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