Meteoroid orbits from video meteors. The case of the Geminid stream

Hajduková, M.; Koten, Pavel; Kornoš, Leonard; Tóth, Juraj

doi:10.1016/j.pss.2017.01.004

Cited by 16 publications

(7 citation statements)

References 46 publications

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“…A large portion of the difference between the two was caused by the overall deceleration of the meteor, but our results suggest that at least 100 m s −1 of this difference could be due to the inherent observational biases of both systems. Finally, we note that the 200 m s −1 to 500 m s −1 initial velocity underestimation for the Geminids described by Hajdukova Jr et al (2017) is well explained by our analysis.…”

Section: Model Validationsupporting

confidence: 80%

“…Hajdukova Jr et al (2017) have recently shown that most orbits of video meteors suffer from a significant bias in semi-major axis due to underestimated initial velocities. They point out that initial velocities of the Geminids are usually underestimated as much as 200 m s −1 to 500 m s −1 compared to simulations and high-precision manual reduction done by Koten et al (2004).…”

Section: Introductionmentioning

confidence: 99%

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Modelling the measurement accuracy of pre-atmosphere velocities of meteoroids

Vida

Brown

Campbell-Brown

2018

Monthly Notices of the Royal Astronomical Society

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Many existing optical meteor trajectory estimation methods use the approximation that the velocity of the meteor at the beginning of its luminous phase is equivalent to its velocity before atmospheric entry. Meteoroid kinetic energy loss prior to the luminous phase cannot be measured, but for some masses and entry geometries neglecting this loss may lead to non-negligible deceleration prior to thermal ablation. Using a numerical meteoroid ablation model, we simulate the kinematics of meteoroids beginning at 180 km with initial velocities ranging from 11 km s −1 to 71 km s −1 , and compare model velocities at the moment of detection to measurements. We validate the simulations by comparing the simulated luminous beginning heights with observed beginning heights of different populations of meteors detected with different optical systems. We find that most low-velocity meteoroids have a significant velocity difference of 100 m s −1 to 750 m s −1 (depending on meteoroid type, mass, and observation system). This systematic underestimate of meteoroid speeds also results in systematically lower semi-major axes for meteoroid orbits.

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Section: Model Validationsupporting

confidence: 80%

Section: Introductionmentioning

confidence: 99%

Modelling the measurement accuracy of pre-atmosphere velocities of meteoroids

Vida

Brown

Campbell-Brown

2018

Monthly Notices of the Royal Astronomical Society

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“…This core is also likely responsible for the narrow Geminids feature observed by PSP's WISPR imager (Battams et al 2020). Radar observations of smaller meteoroids (Hajduková Jr et al 2017) more subject to additional non-gravitational perturbations indicate that 1σ of the reconstructed width at the β-stream source region discussed here is ∼0.03 au.…”

Section: B Geminids β-Stream Ejection Geometrymentioning

confidence: 61%

Collisional Evolution of the Inner Zodiacal Cloud

Szalay¹,

Pokorný²,

Malaspina³

et al. 2021

Preprint

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The zodiacal cloud is one of the largest structures in the solar system and strongly governed by meteoroid collisions near the Sun. Collisional erosion occurs throughout the zodiacal cloud, yet it is historically difficult to directly measure and has never been observed for discrete meteoroid streams. After six orbits with Parker Solar Probe (PSP), its dust impact rates are consistent with at least three distinct populations: bound zodiacal dust grains on elliptic orbits (α-meteoroids), unbound β-meteoroids on hyperbolic orbits, and a third population of impactors that may either be direct observations of discrete meteoroid streams, or their collisional byproducts ("β-streams"). β-streams of varying intensities are expected to be produced by all meteoroid streams, particularly in the inner solar system, and are a universal phenomenon in all exozodiacal disks. We find the majority of collisional erosion of the zodiacal cloud occurs in the range of 10 − 20 solar radii and expect this region to also produce the majority of pick-up ions due to dust in the inner solar system. A zodiacal erosion rate of at least ∼100 kg s −1 and flux of β-meteoroids at 1 au of 0.4 − 0.8 × 10 −4 m −2 s −1 is found to be consistent with the observed impact rates. The β-meteoroids investigated here are not found to be primarily responsible for the inner source of pick-up ions, suggesting nanograins susceptible to electromagnetic forces with radii below ∼50 nm are the inner source of pick-up ions. We expect the peak deposited energy flux to PSP due to dust to increase in subsequent orbits, up to 7 times that experienced during its sixth orbit.

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“…The first well-documented observation of the Geminids occurred in 1862 (Greg 1872;King 1926) and this stream has been studied considerably in the last half-century, both via observations (e.g., Jenniskens 1994;Arlt & Rendtel 2006;Brown et al 2008;Jewitt & Li 2010;) and from a theoretical/modeling framework (e.g., Fox et al 1982Fox et al , 1983Ryabova 2007Ryabova , 2008Ryabova , 2016Ryabova , 2017Ryabova , 2021Williams & Ryabova 2011). Many reviews of this shower have also been undertaken in the literature (e.g., Zigo et al 2009;Jakubík & Neslušan 2015;Neslušan 2015;Hajduková et al 2017).…”

Section: Introductionmentioning

confidence: 99%

Formation, Structure, and Detectability of the Geminids Meteoroid Stream

Cukier

Szalay

2023

Planet. Sci. J.

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The Geminids meteoroid stream produces one of the most intense meteor showers at Earth. It is an unusual stream in that its parent body is understood to be an asteroid, (3200) Phaethon, unlike most streams, which are formed via ongoing cometary activity. Until recently, our primary understanding of this stream came from Earth-based measurements of the Geminids meteor shower. However, the Parker Solar Probe (PSP) spacecraft has transited near the core of the stream close to its perihelion and provides a new platform to better understand this unique stream. Here, we create a dynamical model of the Geminids meteoroid stream, calibrate its total density to Earth-based measurements, and compare this model to recent observations of the dust environment near the Sun by PSP. For the formation mechanisms considered, we find with the exception of very near perihelion the core of the meteoroid stream predominantly lies interior to the orbit of its parent body and we expect grains in the stream to be ≳10 μm in radius. Data–model comparisons of the location of the stream relative to Phaethon’s orbit near perihelion are more consistent with a catastrophic formation scenario, with the core stream residing near or outside the orbit of its parent body consistent with PSP observations. This is in contrast to a cometary formation mechanism, where even near the Sun the meteoroid stream is interior to the orbit of its parent body. Finally, while PSP transits very near the core of the stream, the impact rate expected from Geminids meteoroids is orders of magnitude below the impact rates observed by PSP, and hence undetectable in situ. We similarly expect the upcoming DESTINY+ mission to be unable to detect appreciable quantities of Geminids grains far from (3200) Phaethon.

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Meteoroid orbits from video meteors. The case of the Geminid stream

Cited by 16 publications

References 46 publications

Modelling the measurement accuracy of pre-atmosphere velocities of meteoroids

Modelling the measurement accuracy of pre-atmosphere velocities of meteoroids

Collisional Evolution of the Inner Zodiacal Cloud

Formation, Structure, and Detectability of the Geminids Meteoroid Stream

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