Meteor Showers Research Articles

Asteroid break-ups and meteorite delivery to Earth the past 500 million years

The meteoritic material falling on Earth is believed to derive from large break-up or cratering events in the asteroid belt. The flux of extraterrestrial material would then vary in accordance with the timing of such asteroid family-forming events. In order to validate this, we investigated marine sediments representing 15 time-windows in the Phanerozoic for content of micrometeoritic relict chrome-spinel grains (>32 μm). We compare these data with the timing of the 15 largest break-up events involving chrome-spinel-bearing asteroids (S- and V-types). Unexpectedly, our Phanerozoic time windows show a stable flux dominated by ordinary chondrites similar to today's flux. Only in the mid-Ordovician, in connection with the break-up of the L-chondrite parent body, do we observe an anomalous micrometeorite regime with a two to three orders-of-magnitude increase in the flux of L-chondritic chrome-spinel grains to Earth. This corresponds to a one order-of-magnitude excess in the number of impact craters in the mid-Ordovician following the L-chondrite break-up, the only resolvable peak in Phanerozoic cratering rates indicative of an asteroid shower. We argue that meteorites and small (<1-km-sized) asteroids impacting Earth mainly sample a very small region of orbital space in the asteroid belt. This selectiveness has been remarkably stable over the past 500 Ma.

Modeling the meteoroid streams of comet C/1861 G1 (Thatcher), Lyrids

The meteoroid stream of long-period comet C/1861 G1 (Thatcher) is modeled in course to reveal the details of its structure. Specifically, we modeled several parts of the comet's theoretical stream, which were characterized by various values of evolutionary times and various strengths of the Poynting-Robertson effect. The dynamical behaviour of 10 ​000 test particles in each model from the time of their ejection up to the present was followed via a numerical integration of their orbits. The characteristics of the particles that moved on orbits approaching the Earth's orbit were used to predict a shower. Primarily, we wanted to find whether C/1861 G1 is the parent body of other meteor showers than the April Lyrids. However, we confirm that the orbit of this parent and its meteoroid stream is relatively stable during a long time and the meteoroids can collide with our planet only in the pre-perihelion orbital arc corresponding to the April Lyrids, No. 6, code LYR. Our modeling did not show any clustering of the meteoroids in the stream due to the gravitational perturbations that could explain the observed outbursts. The observed semi-major axes are, in general, smaller than those of the modeled particles and the parent comet because of a selection effect. Namely, the meteoroids in orbits with smaller semi-major axes pass the Earth's orbit more frequently. They are then observed and recorded in the data more often than the meteors with the larger axes.

Return and volatility spillovers to African currencies markets

Using daily exchange rate data from February 02, 2000 to September 25, 2019, this paper examines the world connectedness of African currencies markets by analyzing return and volatility spillovers from the currencies of developed and emerging markets to African currencies. The study also investigates spillovers among African currencies. The empirical findings reveal that African currencies are more responsive to their own-.variable market than to regional and/or global return and volatility spillovers. The only exceptions are BWP, MAD, TND, and ZAR that are found to be integrated with other currencies, with significant meteor showers for both return and volatility.

The Use of Photometric Structural Analysis and Digitized Positional Observation Data to Study Small Celestial Bodies

The problems of the study of small celestial bodies are an important component of modern space research. This applies both to the study of physicochemical and evolutionary parameters and the search for the genetic relationships between meteor showers and their parent bodies. An important area of research is the structural analysis of comets and asteroids. The relevance of the study of comet bodies lies in the fact that comets contain information about the protosolar molecular cloud. Comet nuclei are solid bodies that consist of dust (silicates, polymers, polycyclic aromatic hydrocarbons, etc.) and ice of various compositions (water, carbon dioxide, carbon monoxide, methane, ammonia, etc.). Comet nuclei are fragile and have an irregular shape due to their low density, mass, and gravity. The study of the structural and physicochemical characteristics of comets is a relevant and important task for the development of an evolutionary theory. Using the developed method and special software for brightness analysis of digital images, we created structural models of comets and obtained brightness isophotes of their nuclei, heads, and tails. Since comet nuclei are elements of dynamic evolution and processes in the protodisk of the Solar System, study of the digital structure of comets will help improve the theory of the formation and evolution of the Solar System.

Meteor showers from known long-period comets

What long-period comets with orbital periods >250 years cause detectable meteor showers on Earth? Low-light video cameras are used to track the motion of +4 to −5 magnitude meteors in our atmosphere by triangulation and calculate the meteoroid orbit in space. In recent years, the CAMS (Cameras for Allsky Meteor Surveillance) low-light video camera network was greatly expanded and, together with other video networks, now has increased the total video meteoroid orbit database to over 2.2 million orbits. Here, we searched this database for meteor showers associated with known long-period comets. Previously, five associations were known. Now, we find 14, as well as six uncertain but likely associations. These showers show a change of longitude of perihelion with node that is a strong function of inclination. Showers of longer duration show a steeper magnitude distribution index, presumably due to aging of the meteoroid population. Showers are generally detected only if the orbital period of the comet is less than 4000 years and the Earth-Comet orbital miss distance is ≤0.10 AU. The lack of an associated meteor shower sets lower limits on the orbital period of poorly observed comets.

Modelling cometary meteoroid stream traverses of the Martian Moons eXploration (MMX) spacecraft en route to Phobos

The Martian Moons Exploration (MMX) spacecraft is a JAXA mission to Mars and its moons Phobos and Deimos. MMX will be equipped with the Circum-Martian Dust Monitor (CMDM) which is a newly developed light-weight (mathrm {650,g}) large area (1,mathrm {m}^{2}) dust impact detector. Cometary meteoroid streams (also referred to as trails) exist along the orbits of comets, forming fine structures of the interplanetary dust cloud. The streams consist predominantly of the largest cometary particles (with sizes of approximately 100,mu mathrm { m} to 1 cm) which are ejected at low speeds and remain very close to the comet orbit for several revolutions around the Sun. The Interplanetary Meteoroid Environment for eXploration (IMEX) dust streams in space model is a new and recently published universal model for cometary meteoroid streams in the inner Solar System. We use IMEX to study the detection conditions of cometary dust stream particles with CMDM during the MMX mission in the time period 2024 to 2028. The model predicts traverses of 12 cometary meteoroid streams with fluxes of 100,mu mathrm { m} and bigger particles of at least 10^{-3},mathrm {m}^{-2},mathrm {day}^{-1} during a total time period of approximately 90 days. The highest flux of 0.15,mathrm {m}^{-2},mathrm {day}^{-1} is predicted for comet 114P/Wiseman-Skiff in October 2026. With its large detection area and high sensitivity CMDM will be able to detect cometary meteoroid streams en route to Phobos. Our simulation results for the Mars orbital phase of MMX also predict the occurrence of meteor showers in the Martian atmosphere which may be observable from the Martian surface with cameras on board landers or rovers. Finally, the IMEX model can be used to study the impact hazards imposed by meteoroid impacts onto large-area spacecraft structures that will be particularly necessary for crewed deep space missions.

Monitoring observations of meteor echo at the EKB ISTP SB RAS radar: algorithms, validation, statistics

The paper considers the implementation of algorithms for automatic search for signals scattered by meteor trails according to EKB ISTP SB RAS radar data. In general, the algorithm is similar to the algorithms adopted in specialized meteor systems. The algorithm is divided into two stages: detecting a meteor echo and determining its parameters. We show that on the day of the maximum Geminid shower, December 13, 2016, the scattered signals detected by the algorithm are foreshortening and correspond to scattering by irregularities extended in the direction of the meteor shower radiant. This confirms that the source of the signals detected by the algorithm is meteor trails. We implement an additional program for indirect trail height determination. It uses a decay time of echo and the NRLMSIS-00 atmosphere model to estimate the trail height. The dataset from 2017 to 2019 is used for further testing of the algorithm. We demonstrate a correlation in calculated Doppler velocity between the new algorithm and FitACF. We present a solution of the inverse problem of reconstructing the neutral wind velocity vector from the data obtained by the weighted least squares method. We compare calculated speeds and directions of horizontal neutral winds, obtained in the three-dimensional wind model, and the HWM-14 horizontal wind model. The algorithm allows real-time scattered signal processing and has been put into continuous operation at the EKB ISTP SB RAS radar.

Мониторинговые наблюдения метеорного эха на радаре EKB ИСЗФ СО РАН: алгоритмы, валидация, статистика

The paper considers the implementation of algorithms for automatic search for signals scattered by meteor trails according to EKB ISTP SB RAS radar data. In general, the algorithm is similar to the algorithms adopted in specialized meteor systems. The algorithm is divided into two stages: detecting a meteor echo and determining its parameters. We show that on the day of the maximum Geminid shower, December 13, 2016, the scattered signals detected by the algorithm are foreshortening and correspond to scattering by irregularities extended in the direction of the meteor shower radiant. This confirms that the source of the signals detected by the algorithm is meteor trails. We implement an additional program for indirect trail height determination. It uses a decay time of echo and the NRLMSIS-00 atmosphere model to estimate the trail height. The dataset from 2017 to 2019 is used for further testing of the algorithm. We demonstrate a correlation in calculated Doppler velocity between the new algorithm and FitACF. We present a solution of the inverse problem of reconstructing the neutral wind velocity vector from the data obtained by the weighted least squares method. We compare calculated speeds and directions of horizontal neutral winds, obtained in the three-dimensional wind model, and the HWM-14 horizontal wind model. The algorithm allows real-time scattered signal processing and has been put into continuous operation at the EKB ISTP SB RAS radar.

Observation of the A Carinid Meteor Shower 2020 Unexpected Outburst

Abstract We present observations of the sudden outburst of the A Carinid meteor shower recorded with the Southern Argentina Agile MEteor Radar Orbital System (SAAMER-OS) near the south toroidal sporadic region. The outburst peaked between 21 UT and 22 UT on 2020 October 14 and lasted 7 days (199° ≤ λ ⊙ ≤ 205°), with a mean Sun-centered geocentric ecliptic radiant of λ g − λ ⊙ = 271.°04, β g = −76.°4, and a geocentric speed of 33.3 km s−1. Assuming a mass index value of s = 2.0, we compute a peak 24 hr average flux of 0.029 meteoroids km−2 hr−1 to a limit of 9th magnitude, which is equivalent to a zenithal hourly rate (ZHR) of 5.7 and comparable to other established showers with similar mass indices. By further estimating the peak fluxes for other typical mass index values, we find that the outburst likely never exceeded a maximum ZHR of ∼44, well below the activity of other strong showers. The mean orbital elements resemble those of a short-period object, a = 3.5 ± 0.1 au, q ≃ 1 au, e = 0.72 ± 0.02, i = 55.°8 ± 0.°3, ω = 1° ± 173°, and Ω = 21.°7, and are similar to those derived for two previous shower outbursts observed with SAAMER-OS at high southern ecliptic latitudes. Using the D ′ criterion did not reveal a parent object associated with this shower in the known object catalogs.

Surfaces of (Nearly) Dormant Comets and the Recent History of the Quadrantid Meteor Shower

Abstract The parent of the Quadrantid meteor shower is the inactive solar system small body (196256) 2003 EH1. EH1 has likely only gone dormant in the past few hundred years, and may be related to the bright comet C/1490 Y1. Compared with the other best-studied inactive meteor shower parent (3200) Phaethon, EH1 has received comparatively minimal characterization of its surface properties. We present the first reflectance spectrum and additional photometry of EH1, as well as new spectra of the nuclei of three nearly dormant comets P/2006 HR30 (Siding Spring), 364P/Pan-STARRS, and 249P/LINEAR for comparison. We also present new short-term high-resolution orbital integrations of these bodies for context. EH1s spectrum is red in color below 0.8 μm in between C and D types, consistent with previous photometric measurements, but is blue beyond 0.8 μm until at least 1.02 μm. 249P and 364P have both red slopes consistent with C taxonomic types and HR30 has a classic comet nucleus D-type slope. If the downturn in EH1’s spectrum is due to an absorption feature, magnetite and olivine are plausible candidates, but more data are needed. 249P and 364P have similar recent and historical dynamical evolutions in addition to their similar surface properties. We discuss the interrelation between the dynamical histories and modern surfaces of these four objects and suggest avenues for further study to better constrain how the Quadrantids and Geminids were created.

The 'Meteor Shower' Effect between Precious Metals in Spot and Futures Markets – The Markov Switching Processes in the Variance and Mean

The 'Meteor Shower' Effect between Precious Metals in Spot and Futures Markets – The Markov Switching Processes in the Variance and Mean

Study of aerosol vertical distribution during meteor showers of January 2009

Atmospheric aerosols are minute particles (1 nm–100 μm) suspended in various layers of the Earth's atmosphere. During meteor showers, huge amount of cosmic debris called meteoroids enters into the Earth's atmosphere. These particles contribute to aerosols in the mesosphere and lower thermosphere. The aerosols emerged from meteor dust particles are having different size. The displacement of the particles through the atmosphere is directly proportional to their size. Therefore, we observed several maxima on the post-shower aerosol vertical profiles. One attempt is made to study correlation between the mesospheric and lower thermospheric Aerosol Number Density per cm3 (AND) and different types of Meteor Showers i.e. strong, medium-level and weak. Another attempt is made to trace the journey of meteor matter through lower atmospheric layers. The changes in AND are studied under this topic by using the data collected during January 2009 at Kolhapur (16°39′42.2″N, 74°14′20.8″E) by using Semiautomatic Twilight Photometer. This instrument provides the qualitative picture of vertical distribution of atmospheric aerosols from about 6 km to 360 km with the height resolution of 30 m at tropospheric levels.

Modeling the meteoroid streams of comets C/1894 G1 (Gale) and C/1936 O1 (Kaho-Kozik-Lis)

We modeled meteoroid streams of two long-period comets, C/1894 G1 (Gale) and C/1936 O1 (Kaho-Kozik-Lis), in order to reveal their possible associations with meteor showers observed in the Earth’s atmosphere. For both comets, we modeled several parts of their theoretical streams, characterized by various values of evolutionary times and various strengths of the Poynting-Robertson effect. We studied the dynamical behaviour of 10000 test particles in each model from the time of their ejection up to the present. The characteristics of the particles that moved on orbits approaching the Earth’s orbit were used to predict showers which are related to the parent comet. We also mapped the impacts of possibly different cometary orbits on our predictions by creating models of the streams based on several cloned orbits.The modeling of the stream of the comet C/1894 G1 led to a prediction of a single shower related to the comet. Its existence was, however, not confirmed by real meteor data. Nevertheless, as a byproduct of our investigation, we found a new meteor shower in three databases of video meteors. In line with our suggestion, the shower was named the December ι-Ursae Majorids, No. 1049 and code DIU. We do not consider it as related to the comet.The stream models of the C/1936 O1 also yielded a single predicted shower. Its identification was, in this case, successful and also supported by the cloned-orbit models. In two datasets, we found a shower with characteristics consistent with the predictions. After our suggestion, the shower was newly added into the IAU MDC list as the January ψ-Scorpiids, No. 1048, code JAS.

The study of near Earth objects and meteor showers

In this work, the physical parameters of near-Earth objects (NEO), i.e. small celestial bodies crossing the Earth’s orbit, are investigated. First of all, the study of NEO, whose number exceeds 15 thousand, is important in terms of asteroid threats. NEO are mainly stony and iron, but also could be comet nuclei that had lost the icy component under the influence of solar radiation. As a result of analyzing 14800 near-Earth asteroids from the Apollo group, in this work near-Earth objects closely genetically related to the existing meteor showers are determined. 2002LV and 2001MG1 asteroids are the closest to the Kappa-Cygnids by orbital elements. 2014RS17, 2006BF56, 2001YB5 asteroids are the closest to the Delta-Cancrids by orbital elements. 2008VL14, 2006UF17, 2010VF, 2000DO1, 2010CF55, 2010TN55, 2007EJ88, 481482 2007CA19 asteroids are the closest to the Virginids by orbital elements. The D-criterion method was used in the analysis.

Meteor Hazard for Interplanetary Flights in the Ecliptic Plane

To increase the safety of interplanetary missions, it is necessary to have estimates of the meteor hazard along the flight trajectory. Meteoroid particles of known meteor showers that cross the ecliptic plane at a distance of 1 AU from the Sun are observed as “shooting stars” in the Earth’s atmosphere. However, such meteor streams are principally not observable in interplanetary space. The existence of some meteor streams can be predicted using periodic comets as indicators. During their evolution, cometary nuclei expel meteoritic particles, which remain in the parent orbit for millennia. Thus, the orbits of comets can be considered coinciding with the orbits of young meteor streams produced by the decay of cometary nuclei. We have calculated the coordinates of the regions of intersection of known periodic comets with the ecliptic plane, which are considered as regions of increased meteor hazard. Old meteoroid streams originating from totally decayed comets may be tens and hundreds of times more numerous than young streams. All of them are potential sources of direct meteor collisions with space probes. To assess the risk of interplanetary missions, the planned flight trajectory of FOBOS-GRUNT is compared with the regions of expected meteor streams, and the dates of the most dangerous encounters are given.

The κ-Cygnid Meteor Shower and Its Relationship with Near-Earth Asteroids

This study is focused on the relationships between the κ-Cygnid meteor shower and different groups of asteroids crossing the Earth’s orbit (the so-called near-Earth objects (NEOs)). The analysis is based on the visible structure of the meteor shower and a comprehensive strategy for estimating the proximity of orbits of two bodies. The κ-Cygnid meteor shower (abbreviated as KCG) is observed from August 3 to August 25 every year; it is classified as a minor shower, and the size of its mean orbit is around 3.2 AU, while the geocentric velocity is 20.9 km/s. No parent body (PB) of the shower has been found among comets so far. Relationships between the shower and asteroids, as potential PBs of the shower, are under active examination; some hypotheses on this subject can be found on the website of the Meteor Data Center (MDC) of the International Astronomical Union (IAU).

On the Plasma–Dust Processes Accompanying Meteor Showers

Plasma–dust processes in the Earth’s ionosphere related to transit of meteor bodies and spreading of meteor trail are analyzed. Processes that occur in the meteor trail itself and those taking place in the Earth’s atmosphere upon transit of a meteor body, along with their influence on observers and operation of various technical systems, are investigated. In particular, mechanisms explaining acoustic phenomena accompanying meteor transit during meteor showers are proposed. The mechanism of formation of dusty plasma in meteoroid trails is described. It is demonstrated that charging of dust particles of the meteoroid material creates conditions for the appearance of dust acoustic waves. Dust acoustic perturbations are driven as a result of development of modulation instability of electromagnetic waves emitted by the meteor trail and have frequencies typical of dust sound (0.003–60 Hz). The reports of witnesses revealed that observers on the Earth can hear low-frequency sounds appearing during meteor showers. It is suggested that the sound reaches the Earth’s surface as a result of transfer of oscillations from dust particles to neutrals the concentration of which in the atmosphere is high. The mechanisms of fragmentation of meteor bodies and charging of formed dust particles are analyzed. Characteristic charges of dust fragments for nano- and micrometer-scale particles are estimated. Particles of different shape are considered. The growth rates that give rise to modulation excitation of low-frequency dust acoustic perturbations are calculated. Conditions leading to development of a modulation instability are found.

Prediction of meteoroid stream structure based on meteoroid fragmentation

Every day, large number of meteoroids enter the Earth’s atmosphere and deposit their mass either in atomic form or in ionic form depending on whether it has undergone ablation or fragmentation. The heavier meteoroids undergo fragmentation while the lighter ones are more prone to ablate. In this paper, we would like to speculate meteoroid stream structure of Leonid meteor shower based on fragmenting meteoroids. A 23 revolutions old meteoroid trail left behind by the comet 55P/Tempel-Tuttle in the year 1213 AD, which instigated Leonid meteor shower in the year 2010 is considered for our study. We have calculated mass of the meteoroids, echo durations and percentage of fragmentation. From the observed echo durations of meteoroids, estimated masses and from the percentage of fragmentation, we visualize the stream structure to be like the lighter particles wrapping up the heavier ones. The results we draw from these three different studies are matching with each other. To our knowledge, we are the first to speculate on the meteor stream structure based on fragmentation and making it a new tool in meteor stream evolution. Based on echo durations, it has been observed that 72% of the activity during the shower is contributed by lighter particles of the stream. It is found that about 20% of the meteoroids have undergone fragmentation indicating the minimal role of heavier particles (> $$10^{-6}$$ g) during Leonid Meteor Shower (LMS). The masses of the meteors are estimated to be in the range of $$10^{-10}$$ – $$10^{-5}$$ g.

Modeling the past and future activity of the Halleyid meteor showers

Context.We present a new numerical model of theη-Aquariid and Orionid meteor showers.Aims.The model investigates the origin, variability, and age of theη-Aquariid and Orionid apparitions from 1985 to the present day in order to forecast their activity over the next several decades.Methods.Through the numerical integration of millions of simulated meteoroids and a custom-made particle weighting scheme, we model the characteristics of everyη-Aquariid and Orionid apparition between 1985 and 2050. The modeled showers are calibrated using 35 yr of meteor observations, including the shower activity profiles and interannual variability.Results.Our model reproduces the general characteristics of the present-dayη-Aquariids and part of the Orionid activity. Simulations suggest that the age of theη-Aquariids somewhat exceeds 5000 yr, while a greater fraction of the Orionids is composed of older material. The 1:6 mean motion resonance with Jupiter plays a major role in generating some (but not all) Halleyid stream outbursts. We find consistent evidence for a periodicity of 11.8 yr in both the observations and modeled maximum meteor rates for the Orionids. Weaker evidence of a 10.7 yr period in the peak activity for theη-Aquariids needs to be investigated with future meteor observations. The extension of our model to future years predicts no significant Orionid outbursts through 2050 and four significantη-Aquariid outbursts, in 2023, 2024, 2045, and 2046.

Assessing the multiscale “meteor shower” effect from oil to the central and eastern European stock indices

AbstractThis paper investigates the idiosyncratic volatility spillover effect from the Brent oil futures market to the 11 stock markets of Central and Eastern European economies. As volatility proxies, we use regime‐switching conditional volatilities, obtained from two‐states MS‐GARCH model. In order to determine the level of this effect in different market conditions and in different time‐horizons, we combine wavelet methodology with the quantile regression approach. Our results indicate that the volatility spillover effect is not particularly strong across the countries and the wavelet scales, except in those conditions when stock market volatility is exceptionally high. Also, the wavelet‐based quantile parameters report that the volatility transmission effect gradually subsides with the flow of time, and it applies for the majority of the indices. Romanian BET index experiences the strongest volatility spillover effect from oil in conditions when Romanian stock market is under extreme stress. The reason for this finding probably lies in the facts that Romania is the largest oil and gas producer among all CEECs, and oil and gas markets tend to comove strongly. Based on findings of wavelet quantile parameters and wavelet correlations, we can conclude that hedgers and portfolio managers can build their portfolio strategies, combining Brent oil futures with the CEE indices.