Increasing Geminid meteor shower activity

Ryabova, G. O.; Rendtel, J.

doi:10.1093/mnrasl/slx205

Cited by 18 publications

(12 citation statements)

References 14 publications

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“…For the statistical analyses of the meteor pairs' existence, the shower activity is necessary to be known. Ryabova & Rendtel (2018) showed that the activity of the Geminid meteor shower is increasing for the last 30 years. According to Figure 3 in this paper, the visual ZHR was between 130 and 140 in 2006.…”

Section: Geminid Activitymentioning

confidence: 99%

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Search for pairs and groups in the 2006 Geminid meteor shower

Koten,

Čapek,

Spurný

et al. 2021

Preprint

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Context. The question of the existence of pairs and groups among the meteor showers is opened for a long time. The double station video observation of the 2006 Geminid meteor shower, one of the most active annual showers, is used for the search of such events. Aims. The goal of the paper is to determine whether the observed pairs of Geminid meteors are real events or cases of random coincidence. Methods. The atmospheric trajectories of the observed meteors, photometric masses, and both time and spatial distances of meteoroids in the atmosphere were determined using a double station video observation. Time gaps among them were analysed statistically. The Monte Carlo simulation was used for the determination of the probability of random pairings. Results. Higher than expected number of candidates for pairs was found among 2006 Geminids. Evaluation of Poisson distribution shows that a significant fraction of them may be real cases. However, the Monte Carlo simulation did not confirm this result and provided a different view. Analysis of geometrical positions of candidate pairs also did not support the presence of real pairs and groups. Although we cannot exclude that some of them may be physically connected pairs, all the observed cases can be explained as the coincidental appearance of unrelated meteors.

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Section: Geminid Activitymentioning

confidence: 99%

“…The age of the stream is no longer that few thousand years. Its activity is increasing in the last few decades (Ryabova & Rendtel 2018). Jenniskens (2006) suggests that it will reach its maximum around 2050.…”

Section: Introductionmentioning

confidence: 99%

Search for pairs and groups in the 2006 Geminid meteor shower

Koten,

Čapek,

Spurný

et al. 2021

Preprint

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“…As one of the most reliably active meteor shower events, the Geminid stream has been extensively observed and characterized using several methodologies (Jenniskens, 2006). Ryabova (1999) estimated the age of the stream to be less than a few thousand years, which was corroborated by Beech (2002) who placed constraints of 1000 − 4000 yr. A series of papers has used radar and video observations to construct a detailed model of the structure of the stream (Ryabova, 2007(Ryabova, , 2012(Ryabova, , 2016(Ryabova, , 2017Ryabova and Rendtel, 2018). The ejection velocity was calculated using the apparent width at 1 au by Ryabova (2016) to be 1 km s −1 .…”

Section: Introductionmentioning

confidence: 99%

Dynamical Evolution and Thermal History of Asteroids (3200) Phaethon and (155140) 2005 UD

MacLennan,

Toliou,

Granvik

2020

Preprint

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The near-Earth objects (NEOs) (3200) Phaethon and (155140) 2005 UD are thought to share a common origin, with the former exhibiting dust activity at perihelion that is thought to directly supply the Geminid meteor stream. Both of these objects currently have very small perihelion distances (0.140 and 0.163 au for Phaethon and 2005 UD, respectively), which results in them having perihelion temperatures of or exceeding 1000 K. NEO population models compared to discovery statistics suggest that low-perihelion objects are destroyed over time by a temperature-dependent mechanism that becomes relevant at heliocentric distances < 0.3 au. Thus, the current activity from Phaethon is relevant to the destruction of NEOs close to the Sun, which most likely has produced meteor streams linked to asteroids in the past.We model the past thermal characteristics of Phaethon and 2005 UD using a combination of a thermophysical model (TPM) and orbital integrations of each object. Temperature characteristics such as maximum daily temperature, maximum thermal gradient, and temperature at varying depths are extracted from the model, which is run for a predefined set of a and e. Next, dynamical integrations of orbital clones of Phaethon and 2005 UD are used to estimate the past orbital elements of each object. These dynamical results are then combined with the temperature characteristics to model the past evolution of thermal characteristics such as maximum (and minimum) surface temperature and thermal gradient.We find that dwarf planet (2) Pallas is unlikely to be the parent body for Phaethon and 2005 UD, and it is more likely that the source is in the inner part of the asteroid belt in the families of, e.g., (329) Svea or (142) Polana. The orbital histories of Phaethon and 2005 UD are characterized by cyclic changes in e, resulting in perihelia values periodically shifting between present-day values and 0.3 au. Currently, Phaethon is experiencing relatively large degrees of heating when compared to the recent 20, 000 yr. We find that the subsurface temperatures are too large over this timescale for water ice to be stable, unless actively supplied somehow. The near-surface thermal gradients strongly suggest that thermal fracturing may be very effective at breaking down surface regolith. Observations by the DESTINY+ flyby mission will provide important constraints on the mechanics of dust-loss from Phaethon and, potentially, reveal signs of activity on 2005 UD.

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“…A few prominent streams, such as the well-known Geminid meteoroid stream, are easily detectable and have been studied for decades (e.g. Denning 1893;Plavec 1950;Whipple 1983;Jones et al 2016;Hui & Li 2017;Ryabova & Rendtel 2018, and many others). However, most of the Sun-approaching streams are weakly active and have not received a lot of attention (Ye 2018).…”

Section: Introductionmentioning

confidence: 99%

Debris of Asteroid Disruptions Close to the Sun^∗

Granvik

2019

ApJ

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The under-abundance of asteroids on orbits with small perihelion distances suggests that thermallydriven disruption may be an important process in the removal of rocky bodies in the Solar System. Here we report our study of how the debris streams arise from possible thermally-driven disruptions in the near-Sun region. We calculate that a small body with a diameter 0.5 km can produce a sufficient amount of material to allow the detection of the debris at the Earth as meteor showers, and that bodies at such sizes thermally disrupt every ∼ 2 kyrs. We also find that objects from the inner parts of the asteroid belt are more likely to become Sun-approacher than those from the outer parts. We simulate the formation and evolution of the debris streams produced from a set of synthetic disrupting asteroids drawn from Granvik et al. (2016)'s near-Earth object population model, and find that they evolve 10-70 times faster than streams produced at ordinary solar distances. We compare the simulation results to a catalog of known meteor showers on Sun-approaching orbits. We show that there is a clear overabundance of Sun-approaching meteor showers, which is best explained by a combining effect of comet contamination and an extended disintegration phase that lasts up to a few kyrs. We suggest that a few asteroid-like Sun-approaching objects that brighten significantly at their perihelion passages could, in fact, be disrupting asteroids. An extended period of thermal disruption may also explain the widespread detection of transiting debris in exoplanetary systems.

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Increasing Geminid meteor shower activity

Cited by 18 publications

References 14 publications

Search for pairs and groups in the 2006 Geminid meteor shower

Search for pairs and groups in the 2006 Geminid meteor shower

Dynamical Evolution and Thermal History of Asteroids (3200) Phaethon and (155140) 2005 UD

Debris of Asteroid Disruptions Close to the Sun^∗

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Increasing Geminid meteor shower activity

Cited by 18 publications

References 14 publications

Search for pairs and groups in the 2006 Geminid meteor shower

Search for pairs and groups in the 2006 Geminid meteor shower

Dynamical Evolution and Thermal History of Asteroids (3200) Phaethon and (155140) 2005 UD

Debris of Asteroid Disruptions Close to the Sun∗

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Product

Resources

About

Debris of Asteroid Disruptions Close to the Sun^∗