A survey of southern hemisphere meteor showers

Jenniskens, Peter; Baggaley, J.; Crumpton, Ian; Aldous, Peter; Pokorný, Petr; Janches, Diego; Gural, Peter S.; Samuels, David; Albers, Jim; Howell, Andreas; Johannink, Carl; Breukers, Martin; Odeh, Mohammad; Moskovitz, Nicholas; Collison, Jack; Ganju, Siddha

doi:10.1016/j.pss.2018.02.013

Cited by 32 publications

(31 citation statements)

References 28 publications

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“…Meteors were associated with showers using the table of Sun-centered ecliptic shower radiant positions given in Jenniskens et al (2018). This table, which is based on CAMS data, includes radiant drift and provides numerous, scattered sets of reference parameters per shower.…”

Section: Methodsmentioning

confidence: 99%

Realistic gravitational focusing of meteoroid streams

Moorhead

Clements

Vida

2020

Monthly Notices of the Royal Astronomical Society

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The number density and flux of a meteoroid stream is enhanced near a massive body due to the phenomenon known as gravitational focusing. The greatest enhancement occurs directly opposite the massive body from the stream radiant: as an observer approaches this location, the degree of focusing is unbound for a perfectly collimated stream. However, real meteoroid streams exhibit some dispersion in radiant and speed that will act to eliminate this singularity. In this paper, we derive an analytic approximation for this smoothing that can be used in meteoroid environment models and is based on real measurements of meteor shower radiant dispersion.

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Section: Methodsmentioning

confidence: 99%

Realistic gravitational focusing of meteoroid streams

Moorhead

Clements

Vida

2020

Monthly Notices of the Royal Astronomical Society

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“…Listed parameters are IAUMDC's three-letter code and name, solar longitude of peak activity, radiant in J2000 reference frame and geocentric speed at peak activity, orbital elements including a, e, i, and TJ, the technique that detected the shower (O = optical, R = radar), the estimated age from § 3.1.2 (if available), and proposed parent body in the IAUMDC catalog. The data spreadsheet is available here and a Jupyter notebook that used to prepare this a The IAUMDC catalog (version 2018 November 9) listed only radar detection of this shower, but optical detection has been reported by Jenniskens et al (2018). b The IAUMDC catalog gives C/2003 Q1 (SOHO) as a likely parent, but we find no published research that proposed or discussed this linkage.…”

Section: Age-width-tj Mapmentioning

confidence: 99%

“…The deployment of optical and radar network across the world (e.g. Janches et al 2015;Pokorný et al 2017;Jenniskens et al 2018;Li et al 2018) will increase the temporal coverage and orbit statistics and enhance our understanding of young streams. Another possibility is that these streams are trapped in resonances and are therefore somewhat immune against dispersion.…”

Section: Possible Biases and Implicationmentioning

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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“…524. In the IAU MDC list, version we used, this shower was given in three modifications (Andreić et al 2013;Jenniskens et al 2016aJenniskens et al , 2018. The mean geophysical parameters of these modifications are given in Table 3 and mean orbits in Table 4.…”

Section: Identification Of Real Shower In the Iau MDC Listmentioning

confidence: 99%

“…Some authors have attempted to work out or improve a method of prediction of particular shower, often on the basis of known parent body (Koten & Vaubaillon 2015;Ryabova 2016;Sugar et al 2017;Vaubaillon 2017;Ryabova & Rendtel 2018a,b). All this effort is highly desirable in the current era when a number of new showers as well as a number of new members of known showers are reported every year (e.g., Jones 2018;Jenniskens et al 2018;Koukal 2018;Molau et al 2018a,b,c;Shiba et al 2018;Toth et al 2018;Vida et al 2018a,b;Wisniewski et al 2018, if we consider only the last year).…”

Section: Introductionmentioning

confidence: 99%

Modeling of the meteoroid stream of comet C/1975 T2 and λ-Ursae Majorids

Hajduková

Neslušan

2019

A&A

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Aims. We study the meteoroid stream of the long-period comet C/1975 T2 (Suzuki-Saigusa-Mori). This comet was suggested as the parent body of the established λ-Ursae Majorid meteor shower, No. 524. Methods. We modeled 32 parts of a theoretical meteoroid stream of the parent comet considered. Each of our models is characterized with a single value of the evolutionary time and a single value of the strength of Poynting-Robertson effect. The evolutionary time ranges from 10 000 to 80 000 yr. It is the period during which the evolution of the stream part is followed. In each model, the dynamical evolution of 10 000 test particles was then followed, via a numerical integration, from the time of the modeling up to the present. At the end of the integration, we analyzed the mean orbital characteristics of particles in the orbits that approach the Earth’s orbit, which thus enabled us to predict a shower related to the parent comet. The predicted shower was subsequently compared with its observed counterparts. We separated the latter from the databases of real meteors. As well, we attempted to identify the predicted shower to a shower recorded in the International Astronomical Union Meteor Data Center (IAU MDC) list of all showers. Results. Almost all modeled parts of the stream of comet C/1975 T2 are identified with the corresponding real shower in three video-meteor databases. No real counterpart is found in the IAU MDC photographic or radio-meteor data. In the IAU MDC list of showers and in our current study, this shower is identified with the established λ-Ursae Majorid shower, No. 524. Hence, our modeling confirms the results of previous authors. At the same time we exclude an existence of other meteor shower associated with C/1975 T2.

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A survey of southern hemisphere meteor showers

Cited by 32 publications

References 28 publications

Realistic gravitational focusing of meteoroid streams

Realistic gravitational focusing of meteoroid streams

Debris of Asteroid Disruptions Close to the Sun^∗

Modeling of the meteoroid stream of comet C/1975 T2 and λ-Ursae Majorids

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A survey of southern hemisphere meteor showers

Cited by 32 publications

References 28 publications

Realistic gravitational focusing of meteoroid streams

Realistic gravitational focusing of meteoroid streams

Debris of Asteroid Disruptions Close to the Sun∗

Modeling of the meteoroid stream of comet C/1975 T2 and λ-Ursae Majorids

Contact Info

Product

Resources

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Debris of Asteroid Disruptions Close to the Sun^∗