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"Solar eclipses"
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Eclipses : what everyone needs to know
\"Helps explain the profound differences between a 99.99% partial eclipse and true totality, and inform readers how to experience this most beautiful natural phenomenon successfully. It covers eclipses of sun, moon, and other astronomical objects, and their applications in science, as well as their role in history, literature, and myth. It describes the phenomena to expect at a solar eclipse and the best ways to record them--by camera, video, or by simple handmade experiments. The book covers the timetable of upcoming eclipses, where the best locations will be to see them, and the opportunities for using them as vehicles for inspiration and education. \"--Back cover.
Book
Eclipse : journeys to the dark side of the moon
Explains why eclipses happen, reveals their role in history, literature and myth, and introduces us to eclipse chasers, who travel with ecstatic fervor to some of the most inaccessible places on the globe. The book also includes the author's quest to solve a 3000-year-old mystery: how did the moon move backward during a total solar eclipse, as claimed in the Book of Joshua?
Book
Substorms and Solar Eclipses: A Mutual Information Based Study
Solar eclipses present a rare glimpse into the impact of ionospheric electrodynamics on the magnetosphere independent of other well studied seasonal influences. Despite decades of study, we still do not have a complete description of the conditions for geomagnetic substorm onset. We present herein a mutual information based study of previously published substorm onsets and the past two decades of eclipses which indicates the likelihood of co‐occurrence is greater than random chance. A plausible interpretation for this relation suggests that the abrupt fluctuations in ionospheric conductivity during an eclipse may influence the magnetospheric preconditions of substorm initiation. While the mechanism remains unclear, this study presents strong evidence of a link between substorm onset and solar eclipses. Plain Language Summary Geomagnetic substorms are a long‐studied phenomenon with significant potential for impact on human infrastructure and activities. Despite decades of research, a comprehensive description of what causes these violent eruptions of space plasma near earth has yet to be agreed upon. Although their evolution is well documented, the precise conditions required for substorms to manifest appear to be more complex than previously understood. We present evidence in this manuscript of a mutual dependence between solar eclipses and substorms, which suggests that changes to the upper atmosphere like those occurring during an eclipse may influence substorm development. Key Points In a given 2 hr window between 2001 and 2021, a substorm occurs roughly 40% of the time, increasing to 67% during windows including an eclipse Conditional Point‐wise Mutual Information analysis suggests the probability of eclipse‐substorm co‐occurrence is higher than random chance The mutual dependence between eclipses and substorms is likely the result of ionospheric conductivity feedback into the magnetosphere
Journal Article
The Responses of Ozone to the Solar Eclipse on the 21st of June 2020 in the Mesosphere and Upper Stratosphere
Microwave Limb Sounder (MLS) observations showed an obvious variation of ozone concentration during the annular solar eclipse on 21 June 2020 in the mesosphere and upper stratosphere. Ozone concentration slightly reduced near 40 km in the regions of 24°N–36°N, and increased in low latitudes at 40 km. In the heights of 45–60 km, the increase in ozone concentration in most of the regions was obvious. The ozone increases and decreases were more obvious between 60–65 km, where enhancement took the leading role. The nighttime ozone variation was weaker than the daytime in most of the heights of 30–65 km. The variation of HO2 and CO is investigated to study the photochemical and dynamical causes of ozone variation. As HO2 decreased at 1 hPa and increased at 60–65 km, ozone variation shows a mostly reversed relationship to HO2 variation. CO increased at 32–39 km and decreased at 52–60 km, which was related to the upwelling at these heights. The dynamic processes also contributed to the decrease in ozone concentration at 40 km and increase at 50–60 km.
Journal Article
Sun, moon, Earth : the history of solar eclipses, from omens of doom to Einstein and exoplanets
\"On August 21, 2017, more than ten million Americans will experience an awe-inspiring phenomenon: the first total eclipse of the sun in America in almost forty years. In [this book], astronomer Tyler Nordgren illustrates how this most seemingly unnatural of natural phenomena was transformed from a fearsome omen to a tourist attraction. From the astrologers of ancient China and Babylon to the high priests of the Maya, [we're taken] around the world to show how different cultures interpreted these dramatic events\"--Amazon.com.
Book
A Comparative Study of VLF Transmitter Signal Measurements and Simulations during Two Solar Eclipse Events
To monitor the Very-Low-Frequency (VLF) environment, a VLF detection system has been installed in Suizhou, China, a location with the longitude almost identical to that of the NWC transmitter in Australia. In the years 2019 and 2020, two solar eclipses crossed the NWC–Suizhou path at different locations. Each solar eclipse event represents a naturally occurring controlled experiment, but these two events are unique in that similar levels of electron density variation occurred at different locations along the VLF propagation path. Therefore, we conducted a comparative study using the VLF measurements during these two eclipses. Previous studies mostly estimated a pair of the reflection height (h′) and sharpness parameter (β) using the Long Wavelength Propagation Capability code, whereas, in this study, we use the VLF amplitude and phase as constraints in order to find the electron density change that best explains the VLF measurements. The eclipse measurements could be best explained if the path-averaged β value was 0.56 and 0.62 km−1 for the 2019 and 2020 eclipse, respectively. The VLF reflection height increased from 71.5 to 73.3 km for the 2019 eclipse and from 71.1 to 72.8 km for the 2020 eclipse. The best-fit β values were consistent with the Faraday International Reference Ionosphere model and statistical studies, and the h′ change was also consistent with previous studies and theoretical calculations. Moreover, present results suggested that VLF signals collected by a single receiver were not sensitive to where the electron density change occurs along the propagation path but reflected the average path condition. Therefore, a network of VLF receivers is required in order to monitor in real time the spatial extent of the space weather events that disturb the lower ionosphere.
Journal Article
In the shadow of the moon : the science, magic, and mystery of solar eclipses
In anticipation of the solar eclipses visible in 2017 and 2024, an exploration of the scientific and cultural significance of this mesmerizing cosmic display.-- Source other than the Library of Congress.
Book
Multi-Instrument Observations of the Ionospheric Response Caused by the 8 April 2024 Total Solar Eclipse
This paper investigates ionospheric response characteristics from multiple perspectives based on globally distributed GNSS data and products, ionosonde data, FORMOSAT-7/COSMIC-2 occultation data, and Swarm satellite observations caused by the total solar eclipse of 8 April 2024 across North and Central America. The results show that both GNSS-derived TEC products have detected the ionospheric TEC degradation triggered by the total solar eclipse, with the maximum degradation exceeding 10 TECU. The TEC data from nine GNSS stations in the path of the maximum eclipse reveal that the intensity of ionospheric TEC degradation is related to the spatial location, with the maximum degradation value of the ionospheric TEC being about 14~23 min behind the moment of the maximum eclipse. Additionally, a negative anomaly of foF2 with a maximum of more than 2.7 MHz is detected by ionosonde. In the eclipse region, NmF2 and hmF2 show trends of decrease and increase, with percentages of variation of 40~70% and 4~16%, respectively. The Ne profile of the Swarm-A satellite is significantly lower than the reference value during the eclipse period, with the maximum negative anomaly value reaching 11.2 × 105 el/cm3, and it failed to show the equatorial ionization anomaly.
Journal Article