Meteoric Particles Research Articles

Модернизация интегратора R0 для вычисления эфемерид астероидов: учет релятивистских и негравитационных эффектов

Currently, there are many tools for calculating the trajectories of asteroids, comets, and meteor particles in the Solar System. However, only a portion of them are available to the astronomical community. Many of them do not always meet the requirements for accuracy and calculation speed. Since there is no universal solution here, the development of new methods that combine speed and accuracy following specific problems of celestial mechanics does not lose its importance. There is an attempt to combine the advantages of two trajectory calculation methods in this work. The first of them was developed at Saint Petersburg State University to quickly calculate the trajectories of a large number of particles and was implemented as a program R0. A significant disadvantage of this R0 realization is relatively low accuracy. The second one is designed to calculate the trajectory with maximum accuracy and is implemented in the form of the ASSIST software package. However, it provides lower performance. One of the reasons is the usage of complex motion equations. Some simplified models are compared with data obtained using NASA services. An assessment of the applicability of the upgraded R0 program is given. However, only part of them are available to the astronomical community. Many of them do not always meet the requirements for accuracy and calculation speed. Since there is no universal solution here, the development of new methods that combine speed and accuracy following specific problems of celestial mechanics does not lose its importance. There is an attempt to combine the advantages of two trajectory calculation methods in this work. The first of them was developed at Saint Petersburg State University to quickly calculate the trajectories of a large number of particles and was implemented as a program R0. A significant disadvantage of this R0 realization is relatively low accuracy. The second one is designed to calculate the trajectory with maximum accuracy and is implemented in the form of the ASSIST software package. However, it provides lower performance. One of the reasons is the usage of complex motion equations. Some simplified models are compared with data obtained using NASA services. An assessment of the applicability of the upgraded R0 program is given.

Decadal and Annual Variations in Meteoric Flux From Ulysses, Wind, and SOFIE Observations

AbstractOur solar system is filled with meteoric particles, or cosmic dust, which is either interplanetary or interstellar in origin. Interstellar dust (ISD) enters the heliosphere due to the relative motion of the sun and the interstellar flow. Interplanetary dust (IPD) comes primarily from asteroid collisions or comet sublimation, and comprises the bulk of material entering Earth's atmosphere. This study examines variations in ISD and the IPD flux at Earth using observations from three different satellite techniques. First are size‐resolved in situ meteoroid detections by the Ulysses spacecraft, and second are in situ indirect dust observations by Wind. Third are measurements of meteoric smoke in the mesosphere by the Solar Occultation For Ice Experiment (SOFIE). Wind and Ulysses observations are sorted into the interstellar and interplanetary components. Wind ISD show the anticipated correlation to the 22‐year solar magnetic cycle, and are consistent with model predictions of ISD. Because Wind does not discriminate particle size, the IPD measurements were interpreted using meteoric mass distributions from Ulysses observations and from different models. Wind observations during 2007–2020 indicate a total meteoric influx at Earth of 22 metric tons per day (t d−1), in reasonable agreement with long‐term averages from SOFIE (25 t d−1) and Ulysses (32 t d−1). The SOFIE and Wind influx time series both show an unexpected correlation to the 22‐year solar cycle. This relationship could be an artifact, or may indicate that IPD responds to changes in the solar magnetic field.

Исследование стойкости поверхности спутников к эрозийному износу

The purpose of the research was to study the high-speed impact interaction of a stream of meteor particles and the space satellite surface. The paper describes the effects arising from the movement of microparticles in a material, gives models of the solid particle–metal surfaces interaction, and introduces experimental and analytical dependencies. Within the study, we identified the main factors and estimated their influence on the wear of the surface parts. Furthermore, we examined the mechanism of material destruction depending on the ratio between the hardness of the wear particles and the material. The paper describes various ways of protecting satellites from the influence of the space environment: the use of high-strength and high friction resistance materials, e.g. tungsten, titanium, in the manufacture of the load-bearing structure; the limitation of the spacecraft operation time in space; the use of protective screens and multilayer walls. We studied friction and erosion caused by single particles, the possibility of thermally localized deformation, i.e. adiabatic shear, resulted from local heating, and introduced the mechanism of plastic materials erosion caused by small size abrasive particles. The response of the material at such particle velocities is little known. The study postulates that the material removal (wear) when the surface of the spacecraft is exposed to a stream of abrasive particles results from the interaction of several simultaneously occurring processes due to the separate or combined influence of the components of the stream of these particles. It is recommended that when considering the erosion of material in the stream around the space environment, it is necessary to take the following into account: collisions of particles with each other inside the oncoming stream; crushing of individual particles; screening of the treated surface by particles bouncing off it; a wide range of angles of incidence of particles at a certain point in time; influence of the treated surface on the trajectory of cosmic particles; subsurface damage to the material due to repeated impacts with microparticles; adsorption effect of reducing the strength of the spacecraft surface material at the interface between the spacecraft surface and the stream, etc.

Analysis of modern observations of meteor showers based on PTM methods

The work is focused on the analysis of modern observations of meteoroids included in the data bank formed by both professional researchers and amateur astronomers. Based on the modern physical theory of meteoroids (PTM), a new method for analyzing measurements developed, which provides the accuracy comparable with the results of radar observations. Due to the fact that the accuracy of the new method for analyzing meteoroids observations has increased significantly, it became possible to process observations of the Perseid and Leonid showers over a period of 120 years. The use of PTM made it possible for the first time to explain the distribution of meteor echo signals observed at an altitude of 2 MHz, at which the upper part of this distribution refers to an altitude of 140 km. In the process of work, a database of orbital characteristics of meteoroids was created. A method has been developed for modeling the probability of hitting a certain area of a meteor particle with a mass greater than a certain specified value and determining the density of a meteor shower from radio observations as well as a new “tomography” method for calculating the density distribution of sporadic meteors in the sky using radar observations of meteors at the same station with a goniometer. The method allows calculating the density of a meteor shower on the celestial sphere with an angular resolution of 2°. The use of these methods served as a proof that the distribution density of meteoroid showers on the celestial sphere has two planes of symmetry: the first coincides with the plane of the ecliptic, passing through the poles of the Earth, the other one is perpendicular to the plane of the ecliptic.

Aircraft-based observation of meteoric material in lower-stratospheric aerosol particles between 15 and 68° N

Abstract. We analyse aerosol particle composition measurements from five research missions between 2014 and 2018 to assess the meridional extent of particles containing meteoric material in the upper troposphere and lower stratosphere (UTLS). Measurements from the Jungfraujoch mountaintop site and a low-altitude aircraft mission show that meteoric material is also present within middle- and lower-tropospheric aerosol but within only a very small proportion of particles. For both the UTLS campaigns and the lower- and mid-troposphere observations, the measurements were conducted with single-particle laser ablation mass spectrometers with bipolar-ion detection, which enabled us to measure the chemical composition of particles in a diameter range of approximately 150 nm to 3 µm. The five UTLS aircraft missions cover a latitude range from 15 to 68∘ N, altitudes up to 21 km, and a potential temperature range from 280 to 480 K. In total, 338 363 single particles were analysed, of which 147 338 were measured in the stratosphere. Of these total particles, 50 688 were characterized by high abundances of magnesium and iron, together with sulfuric ions, the vast majority (48 610) in the stratosphere, and are interpreted as meteoric material immersed or dissolved within sulfuric acid. It must be noted that the relative abundance of such meteoric particles may be overestimated by about 10 % to 30 % due to the presence of pure sulfuric acid particles in the stratosphere which are not detected by the instruments used here. Below the tropopause, the observed fraction of the meteoric particle type decreased sharply with 0.2 %–1 % abundance at Jungfraujoch, and smaller abundances (0.025 %–0.05 %) were observed during the lower-altitude Canadian Arctic aircraft measurements. The size distribution of the meteoric sulfuric particles measured in the UTLS campaigns is consistent with earlier aircraft-based mass-spectrometric measurements, with only 5 %–10 % fractions in the smallest particles detected (200–300 nm diameter) but with substantial (> 40 %) abundance fractions for particles from 300–350 up to 900 nm in diameter, suggesting sedimentation is the primary loss mechanism. In the tropical lower stratosphere, only a small fraction (< 10 %) of the analysed particles contained meteoric material. In contrast, in the extratropics the observed fraction of meteoric particles reached 20 %–40 % directly above the tropopause. At potential temperature levels of more than 40 K above the thermal tropopause, particles containing meteoric material were observed in much higher relative abundances than near the tropopause, and, at these altitudes, they occurred at a similar abundance fraction across all latitudes and seasons measured. Above 440 K, the observed fraction of meteoric particles is above 60 % at latitudes between 20 and 42∘ N. Meteoric smoke particles are transported from the mesosphere into the stratosphere within the winter polar vortex and are subsequently distributed towards low latitudes by isentropic mixing, typically below a potential temperature of 440 K. By contrast, the findings from the UTLS measurements show that meteoric material is found in stratospheric aerosol particles at all latitudes and seasons, which suggests that either isentropic mixing is effective also above 440 K or that meteoric fragments may be the source of a substantial proportion of the observed meteoric material.

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.

Dynamics of spherical space debris of different sizes falling to Earth

AbstractSpace debris larger than 1 cm can damage space instruments and impact Earth. The low‐Earth orbits (at heights smaller than 2,000 km) and orbits near the geostationary‐Earth orbit (at 35,786 km height) are especially endangered because most satellites orbit at these latitudes. With current technology, space debris smaller than 10 cm cannot be tracked. Smaller space debris fragments burn up and evaporate in the atmosphere, but larger ones fall to Earth's surface. For practical reasons, it would be important to know the mass, composition, shape, velocity, direction of motion, and impact time of space debris re‐entering the atmosphere and falling to Earth. Since it is very difficult to measure these physical parameters, almost nothing is known about them. To partly fill this gap, we performed computer modeling with which we studied the dynamics of spherical re‐entry particles falling to Earth due to air drag. We determined the time, velocity, and angle of impact as functions of the launch height, direction, speed, and size of spherical re‐entry particles. Our results can also be used for semispherical meteoroid particles of the interplanetary dust entering the Earth's atmosphere.

MATERIAL OF COMETARY NUCLEI AND ASTEROIDS CAN BE STUDIED IN THE EARTH’S ORBIT

The Solar system is formed from a pri- mary gas-dust cloud. Asteroids and cometary nuclei are made of the same substance. Therefore, the study of their debris will help determine their properties. It is best to investigate the substance of meteoroids in the laboratory. The presence of radioactive chemical elements in meteor- ites provides important information about their age. The study of the isotopic composition and content of uranium and thorium gives an age of a meteorite substance of 4.6 billion years. Measurement of cosmogenic isotopes in meteorites and analysis of their content allows us to de- termine the size, mass and age of meteoritic bodies before falling to Earth. By measuring the content of tritium and helium in a meteorite, the average intensity of the cosmic rays bombarding the sample is estimated. Every day, 100- 1000 tons of meteorite material falls on the Earth’s sur- face. A large mass falls to the surface under the action of meteor showers. Meteor showers are formed from the remnants of the nuclei of known comets and asteroid bod- ies. To study the substance of the nucleus of comet Chur- yumov-Gerasimenko, a spacecraft was sent to it worth about 1 billion euros. We offer, that to study the material of some nuclei of comets and asteroids, it is possible to take meteoroid samples directly in outer space in the Earth’s orbit. There, meteoroid particles must be captured, preserved and delivered to Earth for a thorough study. To capture matter from a specific parent cometary nucleus or asteroid in outer space, traps made of silicon dioxide, which are filled with airgel, can be used. The material of the traps allows you to capture particles flying at high speed without overheating them. This allows you to save organic and other molecules in such particles. Such traps should be activated at the moments of maximums of the selected meteor showers.

On Mautner-Type Probability of Capture of Intergalactic Meteor Particles by Habitable Exoplanets

Both macro and microprojectiles (e.g., interplanetary, interstellar and even intergalactic material) are seen as important vehicles for the exchange of potential (bio)material within our solar system as well as between stellar systems in our Galaxy. Accordingly, this requires estimates of the impact probabilities for different source populations of projectiles, including for intergalactic meteor particles which have received relatively little attention since considered as rare events (discrete occurrences that are statistically improbable due to their very infrequent appearance). We employ the simple but comprehensive model of intergalactic microprojectile capture by the gravity of exoplanets which enables us to estimate the map of collisional probabilities for an available sample of exoplanets in habitable zones around host stars. The model includes a dynamical description of the capture adopted from Mautner model of interstellar exchange of microparticles and changed for our purposes. We use statistical and information metrics to calculate probability map of intergalactic meteorite particle capture. Moreover, by calculating the entropy index map we estimate the concentration of these rare events. We further adopted a model from immigration theory, to show that the time dependent distribution of single molecule immigration of material indicates high survivability of the immigrated material taking into account birth and death processes on our planet. At present immigration of material can not be observationally constrained but it seems reasonable to think that it will be possible in the near future, and to use it along other proposed parameters for life sustainability on some planet.

On Mautner-Type Probability of Capture of Intergalactic Meteor Particles by Habitable Exoplanets

Both macro and microprojectiles (e.g., interplanetary, interstellar and even intergalactic material)are seen as important vehicles for the exchange of potential (bio)material within our solar system as wellas between stellar systems in our Galaxy. Accordingly, this requires estimates of the impact probabilitiesfor different source populations of projectiles, including for intergalactic meteor particles which havereceived relatively little attention since considered as rare events (discrete occurrences that are statisticallyimprobable due to their very infrequent appearance). We employ the simple but yet comprehensivemodel of intergalactic microprojectile capture by the gravity of exoplanets which enables us to estimatethe map of collisional probabilities for an available sample of exoplanets in habitable zones around hoststars. The model includes a dynamical description of the capture adopted from Mautner model ofinterstellar exchange of microparticles and changed for our purposes. We use statistical and informationmetrics to calculate probability map of intergalactic meteorite particle capture. Moreover, by calculatingthe entropy index map we measure the concentration of these rare events. We further adopted a modelfrom immigration theory, to show that the transient distribution of birth/death/immigration of materialfor the simplest case has a high value.

On Mautner-Type Probability of Capture of Intergalactic Meteor Particles by Habitable Exoplanets

Both macro and microprojectiles (e.g., interplanetary, interstellar and even intergalactic material) are seen as an important vehicle for the exchange of (bio)material within our solar system as well as between stellar systems in our Galaxy. Accordingly, this requires estimates of the impact probabilities for different source populations of projectiles, specifically for intergalactic meteor particles which have received relatively little attention since considered as rare events (discrete occurrences that are statistically improbable due to their very infrequent appearance). We employ the simple but yet comprehensive model of intergalactic microprojectile capture by the gravity of exoplanets which enables us to estimate the map of collisional probabilities for an available sample of exoplanets in habitable zones around host stars. The model includes a dynamical description of the caption adopted from Mautner model of interstellar exchange of microparticles and changed for our purposes. We use statistical and information metrics to calculate probability map of intergalactic meteorite particle capture. Moreover, by calculating the entropy index map we measure the concentration of these rare events. By adopting a model from immigration theory, we show that the transient distribution of birth/death/immigration of material for the simplest case has a high value.

Development of meteor astronomy at the Odessa University during the period of Ukraine's independence

The article using the methods of bibliographic and source study analysis and systems approach highlights the state and main trends in the development of meteor astronomy in Odessa during the time of independent Ukraine. At the beginning of the 21st century, continuous meteor patrol was restored at the Odessa Astronomical Observatory, which was intensively conducted at the Observatory during Soviet times. It was based on the use of the television and telescopic method, which was used in the CIS for the first time. The advantages of using the television telescopic method in comparison with the photographic and radar methods for solving the fundamental problems of meteor astronomy are noted. The text gives valuable information on the features of continuous meteor patrols at the observation station Kryzhanovka and the work of the expeditionary automatic meteor patrol on Snake Island (Odessa region, Ukraine). The methods of conducting telescopic television observations and processing observational material developed by Odessa researchers are considered. The main directions of meteoric studies conducted in the Odessa Astronomical Observatory using television meteor patrol materials were determined. Studying the physics of meteoric phenomena, obtaining exact coordinates of individual meteor radiant, spectral observations of meteors, studying double and multiple meteors, studying the structure and density of meteoric dust particles, solving interaction problems meteor showers with the Earth’s atmosphere, statistics of meteor phenomena in the Earth’s atmosphere are the main directions of meteoric studies of Odessa Astronomical Observatory. The scientific potential of Yu. M. Gorbanev in the field of meteor astronomy of, the leader of the meteoric group, O. V. Holubaieva, the head of the meteor's television patrol at the Kryzhanovka observation station in 2003-2011, as well as participation in the meteor research S. H. Kimakovskyi, I. I. Kimakovskyi, S. V. Podlesniak, I. A. Stognieieva, L. A. Saresta, A. F. Prinzykov, V. A. Shestopalov, etc are noted. Conclusions are drawn about the importance of conducting meteoric research for the development of fundamental and applied science.

Meteor Observations at Kazan Federal University (Russia)

SummaryThis poster paper described initial results of recent meteor observations in Kazan obtained with a new meteor radar, SKiYMET. Significant improvements in the number of registrations are being recorded, enabling better statistics.Radar observations of meteors have been carried out and archived since the mid-20th Century; at Kazan University (56°N, 49°E) they commenced in 1956, and have continued with only a few interruptions. A quasi-tomographic method (developed in-house in 2000) has been used to determine the coordinates of radiants of meteor showers, and to derive the orbital elements of small showers (microshowers).The observations provide valuable information about the distribution of meteoric matter near the Earth’s orbit. That information supports studies of stratospheric temperatures. A new radar, SKiYMET, was deployed in 2015 and measured parameters such as meteor speeds, but in 2016 its software was supplemented by an in-house package which performed more efficient pre-filtering of the primary data to eliminate non-meteor reflections from various sources. The new filtering algorithm has reduced substantially the threshold S/N ratio for detecting meteors (so fainter meteors can now be recorded), while the package also enables meteor velocities to be calculated much more efficiently than with SKiYMET, improving significantly the quality and statistical indicators of the processed data. By detecting a much larger number of meteors, it enables more detailed studies of the distribution of meteor velocities per day and per season.Daily meteor counts for 2016–2017, extracted from the observations by the KFU programme, yielded significantly higher rates than with SKiYMET. These results support much better statistics, and also enable much finer details to be discerned. In particular, plots of meteor rates against speed are found to exhibit two maxima, one near 30 km s−1 and one near 55 km s−1. This bifurcation in the relationship can also be discerned in the seasonal dependences of the speed distribution.Improvements in the measurements of the speeds of meteor particles entering the atmosphere reveal an increase in the numbers with higher speeds (> 50 km s−1). The distributions of speeds and heights show a rather strong dependence of the meteor speed upon altitude; as predicted by meteor physics, those with higher speeds begin to burn at higher altitudes. A local increase in the number of meteors that have speeds of about 55 km s−1 has also been reported in the literature. The increase could be associated with heterogeneities in the distribution of meteoric matter in the vicinity of the Earth’s orbit.

Assessing the meteoroid risk in near earth space

Abstract The meteoroid risk in circumterrestrial space is basically caused by 1-10 mm meteoroid bodies. Meteoroid particles of such dimensions cannot be registered by modern monitoring astronomical instruments. Observable are only meteor phenomena they cause. This work analyses the activity of main meteor showers over several years and assesses the danger from meteoroids with a size of more than 1 mm. The results of calculating the meteoroid risk during these showers’ maximum activity periods have shown that despite its low values it is sufficiently close to the maximum allowable risk. This already constitutes a recognizable danger, and such a danger needs to be taken into consideration.

Formation of Plasma Around a Small Meteoroid: Simulation and Theory

AbstractHigh‐power large‐aperture radars detect meteors by reflecting radio waves off dense plasma that surrounds a hypersonic meteoroid as it ablates in the Earth's atmosphere. If the plasma density profile around the meteoroid is known, the plasma's radar cross section can be used to estimate meteoroid properties such as mass, density, and composition. This paper presents head echo plasma density distributions obtained via two numerical simulations of a small ablating meteoroid and compares the results to an analytical solution found in Dimant and Oppenheim (2017a, https://doi.org/10.1002/2017JA023960, 2017b, https://doi.org/10.1002/2017JA023963). The first simulation allows ablated meteoroid particles to experience only a single collision to match an assumption in the analytical solution, while the second is a more realistic simulation by allowing multiple collisions. The simulation and analytical results exhibit similar plasma density distributions. At distances much less than λT, the average distance an ablated particle travels from the meteoroid before a collision with an atmospheric particle, the plasma density falls off as 1/R, where R is the distance from the meteoroid center. At distances substantially greater than λT, the plasma density profile has an angular dependence, falling off as 1/R2 directly behind the meteoroid, 1/R3 in a plane perpendicular to the meteoroid's path that contains the meteoroid center, and in front of the meteoroid. When used for calculating meteoroid masses, this new plasma density model can give masses that are orders of magnitude different than masses calculated from a spherically symmetric Gaussian distribution, which has been used to calculate masses in the past.

Study the combustion processes of space debris in the Earth’s atmosphere by meteoric TV camera

Abstract Space debris of millimeter dimensions is almost not detectable by normal methods of observation from Earth. However, particles of such sizes can cause damage to the spacecraft. and even eliminate it. Estimating the status of impurity of near-Earth space mainly based on mathematical models, which are confirmed only for large particles. The millimetric fractions of space debris elements remain unexplored. In case of invasion of debris particles into the planet’s atmosphere, they burn down as well as meteoric particles of natural origin. In this work, the observation technique of separation of debris particles and particles of natural origin is described. Also, the results of the detection of particles from space debris received during the TV observations on the wide-angle camera patrol camera FAVOR (Russia, Northern Caucasus).

Forecast of the Comet 46P/Wirtanen Meteor Shower Activity in 2017 and 2019

The article presents the description of possible activity from the comet 46P/Wirtanen meteor shower. The proximity of this comet to the Earth orbit in 1984–2042 increases probabily for the Earth to encounter meteoroid particles released by this comet. For the nearest years two cases of such activity are found—in 2017 and 2019 and their characteristics and circumstances are presented.

Physical model for motion of low-mass meteor particle grazing upper atmosphere layers

Physical model for motion of low-mass meteor particle grazing upper atmosphere layers

Prediction of the consequences of a high-velocity collision between meteoric particles and elements of a titanium alloy protective structure

Calculation-experimental studies of a high-velocity collision between VT1-0 titanium plates and ultrafine- and coarse-grained structures with a steel spherical impactor are illustrated. Fine-grained VT1-0 titanium plate samples have been obtained using the abc pressing method. Ballistic measurements have been performed using a 30-mm smooth-bore ballistic installation at velocities of about 2500 m/s. A high-velocity collision has been calculated in the scope of an elastoplastic model of interacting materials with regard to destruction and a different phase state at velocities reaching 15 km/s. It has been indicated that the mechanical properties of the VT1-0 alloy are improved when proceeding from a coarse-grained structure to an ultrafine- grained structure; however, in this case, the result of shock loading is hardly affected in the considered velocity range. Titanium plates can be used as screens to protect the main structure of the aircraft from a high-velocity collision.

Three-body resonance in meteoroid streams

Mean-motion resonances play an important role in the evolution of various meteoroid streams. Previous works have studied the effects of two-body resonances in different comets and streams. These already established two-body resonances were mainly induced either by Jovian or Saturnian effects but not both at the same time. Some of these resonances have led to spectacular meteor outbursts and storms in the past. In this work, we find a new resonance mechanism involving three bodies -- i.e. meteoroid particle, Jupiter and Saturn, in the Perseid meteoroid stream. Long-term three-body resonances are not very common in real small bodies in our solar system although they can mathematically exist at many resonant sweet spots in an abstract sense in any dynamical system. This particular resonance combination in the Perseid stream is such that it is close to the ratio of 1:4:10 if the orbital periods of Perseid particle, Saturn and Jupiter are considered respectively. These resonant Perseid meteoroids stay resonant for typically about 2 kyr. Highly compact dust trails due to this unique resonance phenomenon are present in our simulations. Some past and future years are presented where three-body resonant meteoroids of different sizes (or subject to different radiation pressures) are computed to come near the Earth. This is the first theoretical example of an active and stable three-body resonance mechanism in the realm of meteoroid streams.