Showing papers on "Solar eclipse published in 2015"
TL;DR: In this article, the authors revisited all existing evidence and datasets, both direct and indirect, to assess the level of solar activity during the Maunder minimum, and concluded that solar activity was indeed at an exceptionally low level during this period.
Abstract: Aims. Although the time of the Maunder minimum (1645–1715) is widely known as a period of extremely low solar activity, it is still being debated whether solar activity during that period might have been moderate or even higher than the current solar cycle #24. We have revisited all existing evidence and datasets, both direct and indirect, to assess the level of solar activity during the Maunder minimum. Methods. We discuss the East Asian naked-eye sunspot observations, the telescopic solar observations, the fraction of sunspot active days, the latitudinal extent of sunspot positions, auroral sightings at high latitudes, cosmogenic radionuclide data as well as solar eclipse observations for that period. We also consider peculiar features of the Sun (very strong hemispheric asymmetry of the sunspot location, unusual differential rotation and the lack of the K-corona) that imply a special mode of solar activity during the Maunder minimum. Results. The level of solar activity during the Maunder minimum is reassessed on the basis of all available datasets. Conclusions. We conclude that solar activity was indeed at an exceptionally low level during the Maunder minimum. Although the exact level is still unclear, it was definitely lower than during the Dalton minimum of around 1800 and significantly below that of the current solar cycle #24. Claims of a moderate-to-high level of solar activity during the Maunder minimum are rejected with a high confidence level.
198 citations
TL;DR: In this article, the authors revisited all the existing pieces of evidence and datasets, both direct and indirect, to assess the level of solar activity during the Maunder minimum, and concluded that solar activity was indeed at an exceptionally low level during this period.
Abstract: Aims: Although the time of the Maunder minimum (1645--1715) is widely known as a period of extremely low solar activity, claims are still debated that solar activity during that period might still have been moderate, even higher than the current solar cycle #24. We have revisited all the existing pieces of evidence and datasets, both direct and indirect, to assess the level of solar activity during the Maunder minimum.
Methods: We discuss the East Asian naked-eye sunspot observations, the telescopic solar observations, the fraction of sunspot active days, the latitudinal extent of sunspot positions, auroral sightings at high latitudes, cosmogenic radionuclide data as well as solar eclipse observations for that period. We also consider peculiar features of the Sun (very strong hemispheric asymmetry of sunspot location, unusual differential rotation and the lack of the K-corona) that imply a special mode of solar activity during the Maunder minimum.
Results: The level of solar activity during the Maunder minimum is reassessed on the basis of all available data sets.
Conclusions: We conclude that solar activity was indeed at an exceptionally low level during the Maunder minimum. Although the exact level is still unclear, it was definitely below that during the Dalton minimum around 1800 and significantly below that of the current solar cycle #24. Claims of a moderate-to-high level of solar activity during the Maunder minimum are rejected at a high confidence level.
130 citations
TL;DR: The measurement of the deflection of starlight during a total solar eclipse on 29 May 1919 was the first verification of general relativity by an external team of scientists, brought Einstein and his theory to the attention of the general public, and left a legacy of experimental testing as mentioned in this paper.
Abstract: The measurement of the deflection of starlight during a total solar eclipse on 29 May 1919 was the first verification of general relativity by an external team of scientists, brought Einstein and his theory to the attention of the general public, and left a legacy of experimental testing that continues today. The discovery of gravitational lenses turned Einstein's deflection into an important tool for astronomy and cosmology. This article reviews the history of the 1919 measurement and other eclipse measurements, describes modern measurements of the effect using radio astronomy, and of its cousin, the Shapiro time delay, and discusses the discovery and impact of gravitational lenses.
57 citations
TL;DR: The ASPIICS (Association of Spacecraft for Polarimetric and Imaging Investigation of the Corona of the Sun) as mentioned in this paper is the first space coronagraph to cover the range of radial distances between 1.08 and 3 solar radii where the magnetic field plays a crucial role in the coronal dynamics, thus providing continuous observational conditions very close to those during a total solar eclipse.
Abstract: The “sonic region” of the Sun corona remains extremely difficult to observe with spatial resolution and sensitivity sufficient to understand the fine scale phenomena that govern the quiescent solar corona, as well as phenomena that lead to coronal mass ejections (CMEs), which influence space weather. Improvement on this front requires eclipse-like conditions over long observation times. The space-borne coronagraphs flown so far provided a continuous coverage of the external parts of the corona but their over-occulting system did not permit to analyse the part of the white-light corona where the main coronal mass is concentrated. The proposed PROBA-3 Coronagraph System, also known as ASPIICS (Association of Spacecraft for Polarimetric and Imaging Investigation of the Corona of the Sun), with its novel design, will be the first space coronagraph to cover the range of radial distances between ~1.08 and 3 solar radii where the magnetic field plays a crucial role in the coronal dynamics, thus providing continuous observational conditions very close to those during a total solar eclipse. PROBA-3 is first a mission devoted to the in-orbit demonstration of precise formation flying techniques and technologies for future European missions, which will fly ASPIICS as primary payload. The instrument is distributed over two satellites flying in formation (approx. 150m apart) to form a giant coronagraph capable of producing a nearly perfect eclipse allowing observing the sun corona closer to the rim than ever before. The coronagraph instrument is developed by a large European consortium including about 20 partners from 7 countries under the auspices of the European Space Agency. This paper is reviewing the recent improvements and design updates of the ASPIICS instrument as it is stepping into the detailed design phase.
37 citations
TL;DR: In this paper, five ionosondes in the Northeast Asia were used to record the midlatitude ionospheric responses to the solar eclipse of 20 May 2012, and the latitude dependence of the eclipse lag was studied first.
Abstract: The solar eclipse effects on the ionosphere are very complex. Except for the ionization decay due to the decrease of the photochemical process, the couplings of matter and energy between the ionosphere and the regions above and below will introduce much more disturbances. Five ionosondes in the Northeast Asia were used to record the midlatitude ionospheric responses to the solar eclipse of 20 May 2012. The latitude dependence of the eclipse lag was studied first. The foF2 response to the eclipse became slower with increased latitude. The response of the ionosphere at the different latitudes with the same eclipse obscuration differed from each other greatly. The plasma flux from the protonsphere was possibly produced by the rapid temperature drop in the lunar shadow to make up the ionization loss. The greater downward plasma flux was generated at higher latitude with larger dip angle and delayed the ionospheric response later. The waves in the foEs and the plasma frequency at the fixed height in the F layer are studied by the time period analytic method. The gravity waves of 43–51 min center period during and after the solar eclipse were found over Jeju and I-Cheon. The northward group velocity component of the gravity waves was estimated as ~108.7 m/s. The vertical group velocities between 100 and 150 km height over the two stations were calculated as ~5 and ~4.3 m/s upward respectively, indicating that the eclipse-induced gravity waves propagated from below the ionosphere.
31 citations
TL;DR: In this article, the authors observed from sites in Queensland, Australia, during the 2012 November 13 (UT)/14 (local time) total solar eclipse, and analyzed its dynamics.
Abstract: Continuing our series of observations of coronal motion and dynamics over the solar-activity cycle, we observed from sites in Queensland, Australia, during the 2012 November 13 (UT)/14 (local time) total solar eclipse. The corona took the low-ellipticity shape typical of solar maximum (flattening index e = 0.01), a change from the composite coronal images we observed and analyzed in this journal and elsewhere for the 2006 and 2008-2010 eclipses. After crossing the northeast Australian coast, the path of totality was over the ocean, so further totality was seen only by shipborne observers. Our results include velocities of a coronal mass ejection (CME; during the 36 minutes of passage from the Queensland coast to a ship north of New Zealand, we measured 413 km s6(–1)) and we analyze its dynamics. We discuss the shapes and positions of several types of coronal features seen on our higher-resolution composite Queensland coronal images, including many helmet streamers, very faint bright and dark loops at the bases of helmet streamers, voids, and radially oriented thin streamers. We compare our eclipse observations with models of the magnetic field, confirming the validity of the predictions, and relate the eclipse phenomenology seen with the near-simultaneous images from NASA's Solar Dynamics Observatory (SDO/AIA), NASA's Extreme Ultraviolet Imager on Solar Terrestrial Relations Observatory, ESA/Royal Observatory of Belgium's Sun Watcher with Active Pixels and Image Processing (SWAP) on PROBA2, and Naval Research Laboratory's Large Angle and Spectrometric Coronagraph Experiment on ESA's Solar and Heliospheric Observatory. For example, the southeastern CME is related to the solar flare whose origin we trace with a SWAP series of images.
23 citations
TL;DR: In this paper, the authors studied the effect of the solar eclipse on the low-latitude ionosphere using a multi-instrument network consisting of magnetometer, ionosonde and GPS receivers.
20 citations
TL;DR: In this article, the authors present the use of very low frequency (VLF) radio data to study short-period (∼min-hrs) atmospheric gravity waves and long-period(∼days) planetary waves.
17 citations
TL;DR: In this article, the authors show how the solar eclipse occurred on 20 March 2015 influenced the sporadic E (Es) layer as recorded by the Advanced Ionospheric Sounder by Istituto Nazionale di Geofisica e Vulcanologia (AIS-INGV) ionosondes installed at Rome (41.8°N, 12.5°E) and Gibilmanna (37.9°N 14.0°E), Italy.
17 citations
TL;DR: In this article, the response of the vertical plasma drift and the electron density (NmF2) during different solar eclipses was investigated, and the diurnal values of the direct scaled measurement of F2 peak height and the one derived from M(3000) F2 data, acquired over an equatorial/low-latitude stations, have been used to determine the vertical plasminar drift.
Abstract: The response of the vertical plasma drift (Vz) and the electron density (NmF2) during different solar eclipses was investigated. The diurnal values of the direct scaled measurement of F2 peak height and the one derived from M(3000) F2 data, acquired over an equatorial/low-latitude stations, have been used to determine the vertical plasma drift. The ionosphere during a solar eclipse is significantly affected by the E × B vertical drift; the large depletion of electron density at low altitudes can be transported to high altitudes through the plasma vertical drift. The loss in ionization density during the eclipse phase decreases the electron density, which was accompanied by rapid increase in hmF2. This deviation in the NmF2 during eclipse compared to control days can be related to the increase in the loss rate due to recombination, as a result of reduction in thermal energy. However, the maximum reduction in NmF2 is not synchronous with the time of maximum totality but some minutes later. The differences in the solar epochs may contribute to the observed relative changes in the ionospheric F2 region behavior during the eclipse window. Lastly, it is very difficult to separate the influence of magnetic disturbances from solar eclipse. The deviation in NmF2 is higher during magnetic disturbed days than the quiet day. The reverse is the case for hmF2 observation. However, the NmF2 variation increases with an increase in solar activity.
16 citations
TL;DR: In this paper, the authors analyse des planifications de telles expeditions dans le contexte d'une culture coloniale and compare them with the planifications of telles explorations in Indochina.
Abstract: Entre 1860 et 1914, plusieurs expeditions ont ete realisees par les astronomes britanniques pour etudier l'eclipse du soleil en Inde. Analyse des planifications de telles expeditions dans le contexte d'une culture coloniale
TL;DR: In this article, the authors analyzed air temperature measurements made near the ground by the Williams College expedition to observe the first total occultation of the Sun [TOS (commonly known as a total solar eclipse)] of the 21st century in Lusaka, Zambia, in the afternoon of June 21, 2001.
TL;DR: In this paper, the authors used a projection map approach and a line of intersection method by extending the Earth shadow eclipse models described by Srivastava et al. for the Earth orbiting spacecraft.
Posted Content•
TL;DR: In this article, the authors theoretically predict the normal characteristics of very low frequency (3~30 kHz) radio wave propagation through Earth-ionosphere waveguide corresponding to normal behavior of the D-region ionosphere.
Abstract: In this thesis, we theoretically predict the normal characteristics of Very Low Frequency (3~30 kHz) radio wave propagation through Earth-ionosphere waveguide corresponding to normal behavior of the D-region ionosphere. We took the VLF narrow band data from the receivers of Indian Centre for Space Physics (ICSP) to validate our models. Detection of sudden ionospheric disturbances (SIDs) are common to all the measurements. We apply our theoretical models to infer the D-region characteristics and to reproduce the observed VLF signal behavior corresponding to such SIDs.
We develop a code based on ray theory to simulate the diurnal behavior of VLF signals over short propagation paths (2000~3000 km). The diurnal variation from this code are comparable to the variation obtained from a more general Long Wave Propagation Capability (LWPC) code which is based on mode theory approach. We simulate the observational results obtained during the Total Solar Eclipse of July 22, 2009 in India. We also report and simulate a historic event, namely, the lunar occultation of a solar flare during the annular solar eclipse of 15th January, 2010 and find the effects on the D-region electron density profiles.
01 Apr 2015
TL;DR: In this article, the angular distance between the Sun and the Moon is used to develop a method to instantaneously monitor the partial or total solar eclipse occurrence for solar energy applications, which can be used in many other applications for observers of the sun and the moon positions for applications limited to the stated uncertainty.
Abstract: In recent years, the interest in using solar energy as a major contributor to renewable energy applications has increased, and the focus to optimize the use of electrical energy based on demand and resources from different locations has strengthened. This article includes a procedure for implementing an algorithm to calculate the Moon’s zenith angle with uncertainty of ±0.001° and azimuth angle with uncertainty of ±0.003°. In conjunction with Solar Position Algorithm, the angular distance between the Sun and the Moon is used to develop a method to instantaneously monitor the partial or total solar eclipse occurrence for solar energy applications. This method can be used in many other applications for observers of the Sun and the Moon positions for applications limited to the stated uncertainty.
TL;DR: In this paper, the angular distance between the Sun and the Moon is used to develop a method to instantaneously monitor the partial or total solar eclipse occurrence for solar energy applications, which can be used in many other applications for observers of the sun and the moon positions for applications limited to the stated uncertainty.
TL;DR: In this paper, the conditions under which eclipse induced stresses are safe for E-sail tethers were analyzed by numerical simulation, and the closest safe approach distances for Earth, Moon, Venus, Mars, Jupiter, Ceres and an exemplary 300 km main belt asteroid Interamnia for circular, parabolic and hyperbolic orbits.
TL;DR: In this article, the geomagnetic field data sets indicated that there was a characteristic decrease at the beginning of the solar eclipse and this decrease can be well-correlated with previous measurements taken during the total solar eclipse that was observed in Turkey on 2006 March 29.
Abstract: Some geophysical parameters, such as those related to gravitation and the geomagnetic field, could change during solar eclipses. In order to observe geomagnetic fluctuations, geomagnetic measurements were carried out in a limited time frame during the partial solar eclipse that occurred on 2011 January 4 and was observed in Canakkale and Ankara, Turkey. Additionally, records of the geomagnetic field spanning 24 hours, obtained from another observatory (in Iznik, Turkey), were also analyzed to check for any peculiar variations. In the data processing stage, a polynomial fit, following the application of a running average routine, was applied to the geomagnetic field data sets. Geomagnetic field data sets indicated there was a characteristic decrease at the beginning of the solar eclipse and this decrease can be well-correlated with previous geomagnetic field measurements that were taken during the total solar eclipse that was observed in Turkey on 2006 March 29. The behavior of the geomagnetic field is also consistent with previous observations in the literature. As a result of these analyses, it can be suggested that eclipses can cause a shielding effect on the geomagnetic field of the Earth.
Posted Content•
TL;DR: The failure of the laser-interferometer gravitational wave antennas to measure the tiny changes of lengths many orders of magnitude smaller than the diameter of a proton raises the question of whether the reason for this failure is a large gravitational wave background noise, and if so, where this background noise is coming from.
Abstract: The failure of the laser-interferometer gravitational wave antennas to measure the tiny changes of lengths many orders of magnitude smaller than the diameter of a proton raises the question of whether the reason for this failure is a large gravitational wave background noise, and if so, where this background noise is coming from. It is conjectured that it comes from gravitational waves emitted from a magnetohydrodynamic dynamo in the center of the sun, with the large magnetic field from this dynamo shielded by thermomagnetic currents in the tachocline. Using the moon as a large Weber bar, these gravitational waves could possibly be detected by the Poisson diffraction into the center of the lunar shadow during a total solar eclipse.
TL;DR: In this paper, the authors used wavelet analysis to study the periodic variations in the intensity, Doppler velocity and line width of the solar corona during the 2010 total solar eclipse.
Abstract: During the total solar eclipse of 11 July 2010, multi-slit spectroscopic observations of the solar corona were performed from Easter Island, Chile. To search for high-frequency waves, observations were taken at a high cadence in the green line at 5303 A due to [Fe xiv] and the red line at 6374 A due to [Fe x]. The data are analyzed to study the periodic variations in the intensity, Doppler velocity and line width using wavelet analysis. The data with high spectral and temporal resolution enabled us to study the rapid dynamical changes within coronal structures. We find that at certain locations each parameter shows significant oscillation with periods ranging from 6 - 25 s. For the first time, we could detect damping of high-frequency oscillations with periods of the order of 10 s. If the observed damped oscillations are due to magnetohydrodynamic (MHD) waves then they can contribute significantly in the heating of the corona. From a statistical study we try to characterize the nature of the observed oscillations while looking at the distribution of power in different line parameters.
10 Dec 2015
TL;DR: In this paper, the authors evaluated the performance of three models, namely Klobuchar, NeQuick-G and Global ionospheric Maps (GIMs), for non-nominal ionosphere conditions, such as the geomagnetic storm on March 17, 2015 followed by a Solar Eclipse on March 20.
Abstract: Global Navigation Satellite System (GNSS)-based navigation is usually carried out in open sky conditions, where one of the main error sources is introduced by the ionosphere. Ionospheric effect can be mitigated by combining two GNSS signals at different frequencies exploiting the dispersive behavior of the ionosphere. Unfortunately, most of the mass-market receivers do not benefit from this cancellation since they are single frequency receivers, hence they have to apply a model to reduce the ionospehric effects. In this work three models are considered, specifically Klobuchar, NeQuick-G and Global ionospheric Maps (GIMs). In this context, it is important to evaluate the response of these models to non-nominal ionospheric conditions, such as the geomagnetic storm on March 17, 2015 followed by a Solar Eclipse on March 20. The combination of these phenomena generates a unique scenario to test the discrepancies of the broadcast ionosphere with the real one. The performance is evaluated in the measurement domain computing the delay by the above mentioned models and comparing it with respect to the reference delay computed using post-processed Vertical Total Electron Content (VTEC) maps provided by the International GNSS Service (IGS). In order to analyze the impact of the Coronal Mass Ejection (CME) and the Eclipse, a performance analysis is carried out also in the position domain, applying different ionospheric algorithms. In this work, experiments to compare the performance of different ionospheric modelling methods, and to evaluate their robustness in non-nominal conditions, are conducted. The performance is evaluated using data from three different IGS stations.
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TL;DR: In this article, the anomalous behavior of pendulums during a total solar eclipse was explained by Poisson diffraction of gravitational waves into the lunar shadow, with the waves emitted through large mass motion in the center of the sun by a thermonuclear fusion reaction driven magnetohydrodynamic dynamo.
Abstract: An attempt is made to explain the Allais effect, the anomalous behavior of pendulums during a total solar eclipse, by Poisson diffraction of gravitational waves into the lunar shadow, with the waves emitted through large mass motion in the center of the sun by a thermonuclear fusion reaction driven magnetohydrodynamic dynamo. Thermomagnetic currents in the tachocline shield the strong magnetic field in the solar core.
TL;DR: The Cretan Bronze Age Minoan Kernos as discussed by the authors was designed specifically to predict the occurrence of the 9th. January 1860 BCE total solar eclipse and a prototype magnetic compass was centrally facilitated in a non-magnetic marble structure, whose geomagnetic declination angle appeared to coincide with the Kernos' eclipse prediction-axis orientation.
Abstract: Archaeometry is the application of scientific techniques used to analyze archaeological materials. The Cretan Bronze Age Minoan Kernos, has hitherto, been regarded as a gaming board or for religious purposes. Here, it is shown, that, it was designed, specifically, to predict the occurrence of the 9th. January 1860 BCE Total Solar Eclipse. A prototype magnetic compass was centrally facilitated in a non-magnetic marble structure, whose geomagnetic declination angle, appears to coincide with the Kernos’ eclipse prediction-axis orientation. Comparisons of eclipse constructions taken from Kernos measurements, with those of Hipparchus (2nd. c. BCE), appear to be similar, suggesting a common origin. Evidence obtained using a multidisciplinary approach, is testament to the sophistication of Middle Bronze Age science and technology and the ability to create a mathematically-based eclipse predictor and magnetic compass, 3800 years ago and 1700 years before the advent of the Antikythera Mechanism.
01 Jan 2015
TL;DR: In this article, the angular diameters of the Sun and Moon in ancient and medieval astronomy and their role in predicting the existence of annular eclipses are discussed. But since the Ptolemaic context, there was no justifiable basis for annular eclipse.
Abstract: This study deals with considerations on the angular diameters of the Sun and Moon in ancient and medieval astronomy and focuses on their role in predicting the existence of annular eclipses. Historical reports of annular eclipses probably date back to the ancient Greeks. From that period there are some documented theoretical considerations about the angular diameters of the Sun and Moon, implying the possible existence of annular eclipses. Nevertheless, according to the Ptolemaic context, since the minimum angular diameters of the Sun and Moon were considered to be equal, there was no justifiable basis for annular eclipses. During the medieval Islamic period, some observational evidence, including annular eclipses in AD 873 and 1283, and a total solar eclipse in AD 876 in which the Sun was completely covered for an unusually long interval, led to attempts by the astronomers of the time to revise Ptolemaic ideas, and come up with acceptable alternatives. Accordingly, non-Ptolemaic ideas concerning the angular diameters of the Sun and Moon were adopted from Indian astronomy, inserted into the Ptolemaic model, and eventually transferred to European astronomy. Finally, by the late medieval period a ‘bright ring eclipse’ had become an accepted term for one of the three types of solar eclipses––the others being total and partial. With the progress of astronomy, the discussion of annular eclipses was back on the agenda whenever the idea of homocentric models arose, and were used to reveal their glaring deficiencies.
Journal Article•
TL;DR: In this paper, two Burmese eclipse calculations, one lunar and one solar, were analyzed using examples from a Burmeese manuscript, with some important exceptions the same as in the Suryasiddhanta, but the handling of, for instance, parallax in the solar eclipse is different and much simplified.
Abstract: Two Burmese eclipse calculations, one lunar and one solar, are analysed using examples from a Burmese manuscript. The fundamental parameters are with some important exceptions the same as in the Suryasiddhanta, but the handling of, for instance, parallax in the solar eclipse is different and much simplified. Specific to Burma are also the shadow calculations.
Book Chapter•
01 Nov 2015
TL;DR: In this paper, the authors discuss ongoing plans and discussions for EPO and scientific observing of the 21 August 2017 total solar eclipse and discuss aspects of EPO based on my experiences at the 60 solar eclipses I have seen.
Abstract: I discuss ongoing plans and discussions for EPO and scientific observing of the 21 August 2017 total solar eclipse. I discuss aspects of EPO based on my experiences at the 60 solar eclipses I have seen. I share cloud statistics along the eclipse path compiled by Jay Anderson, the foremost eclipse meteorologist. I show some sample observations of composite imagery, of spectra, and of terrestrial temperature changes based on observations of recent eclipses, including 2012 from Australia and 2013 from Gabon. Links to various mapping sites of totality, partial phases, and other eclipse-related information, including that provided by Michael Zeiler, Fred Espenak (retired from NASA) and Xavier Jubier can be found on the website I run for the International Astronomical Union's Working Group on Eclipses at http://www.eclipses.info.
TL;DR: In this article, the vertical distributions of mesospheric ozone (O3) during a solar eclipse event and analyzes theoretically the eclipse-induced changes were reported. But the authors did not consider the photochemical lifetime of ozone in the mesosphere.
Abstract: The Superconducting Submillimeter-Wave Limb-Emission Sounder (SMILES) successfully observed vertical distributions of ozone (O3) concentration in the middle atmosphere during the annular solar eclipse that occurred on 15 January 2010. In the mesosphere, where the photochemical lifetime of O3 is relatively short (approximately 100 s), altitude-dependent changes in O3 concentration under reduced solar radiation and their temporal variations were clearly observed as a function of the eclipse obscuration. This study reports the vertical distributions of mesospheric O3 during a solar eclipse event and analyzes theoretically the eclipse-induced changes. We show that simple analytical expressions for O3 concentration, which assume that O3 and O are in a photochemically steady state, can be used to describe the O3 concentration under reduced solar radiation. The SMILES data obtained during the eclipse provide a unique opportunity to test our current understanding of mesospheric O3 photochemistry.
16 Mar 2015
TL;DR: The NASA Ames Krex2 rover deployed and operated in the Mojave Volatile Prospector (MVP) field expedition during the partial solar eclipse of 23-26 October 2014.
Abstract: On 23 October a partial solar eclipse occurred across parts of the southwest United States between approximately 21:09 and 23:40 (UT), with maximum obscuration, 36%, occurring at 22:29 (UT). During 21-26 October 2014 the Mojave Volatile Prospector (MVP) field expedition deployed and operated the NASA Ames Krex2 rover in the Mojave desert west of Baker, California (Fig. 1, bottom). The MVP field expedition primary goal was to characterize the surface and sub-surface soil moisture properties within desert alluvial fans, and as a secondary goal to provide mission operations simulations of the Resource Prospector (RP) mission to a Lunar pole. The partial solar eclipse provided an opportunity during MVP operations to address serendipitous science. Science instruments on Krex2 included a neutron spectrometer, a near-infrared spectrometer with associated imaging camera, and an independent camera coupled with software to characterize the surface textures of the areas encountered. All of these devices are focused upon the surface and as a result are downward looking. In addition to these science instruments, two hazard cameras are mounted on Krex2. The chief device used to monitor the partial solar eclipse was the engineering development unit of the Near-Infrared Volatile Spectrometer System (NIRVSS) near-infrared spectrometer. This device uses two separate fiber optic fed Hadamard transform spectrometers. The short-wave and long-wave spectrometers measure the 1600-2400 and 2300-3400 nm wavelength regions with resolutions of 10 and 13 nm, respectively. Data are obtained approximately every 8 seconds. The NIRVSS stares in the opposite direction as the front Krex2.