The Geminid meteor stream and asteroid 3200 Phaethon

Williams, I. P.; Wu, Zhijun

doi:10.1093/mnras/262.1.231

Cited by 132 publications

(90 citation statements)

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“…About 2 kyr ago, Phaethon's orbital eccentricity was highest, causing its perihelion value to reach q ∼ 0.126 au, which is significantly lower than its current value q ∼ 0.14 au. This has been noted before (e.g., Williams & Wu 1993). Several authors studied the possibility of a recent formation of the Geminids stream, including that near 0 AD when the perihelion had its last minimum (see, e.g., Ryabova 2007 or; for a more detailed overview, Jenniskens 2006).…”

Section: Orbital Evolutionmentioning

confidence: 72%

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Near-Earth asteroid (3200) Phaethon: Characterization of its orbit, spin state, and thermophysical parameters

Hanuš

Delbò

Vokrouhlický

et al. 2016

A&A

110

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Context. The near-Earth asteroid (3200) Phaethon is an intriguing object: its perihelion is at only 0.14 au and is associated with the Geminid meteor stream. Aims. We aim to use all available disk-integrated optical data to derive a reliable convex shape model of Phaethon. By interpreting the available space-and ground-based thermal infrared data and Spitzer spectra using a thermophysical model, we also aim to further constrain its size, thermal inertia, and visible geometric albedo. Methods. We applied the convex inversion method to the new optical data obtained by six instruments and to previous observations. The convex shape model was then used as input for the thermophysical modeling. We also studied the long-term stability of Phaethon's orbit and spin axis with a numerical orbital and rotation-state integrator.Results. We present a new convex shape model and rotational state of Phaethon: a sidereal rotation period of 3.603958(2) h and ecliptic coordinates of the preferred pole orientation of (319 • , −39 • ) with a 5 • uncertainty. Moreover, we derive its size (D = 5.1 ± 0.2 km), thermal inertia (Γ = 600 ± 200 J m −2 s −1/2 K −1 ), geometric visible albedo (p V = 0.122 ± 0.008), and estimate the macroscopic surface roughness. We also find that the Sun illumination at the perihelion passage during the past several thousand years is not connected to a specific area on the surface, which implies non-preferential heating.

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Section: Orbital Evolutionmentioning

confidence: 72%

“…Phaethon has been dynamically associated with the Geminid meteor stream (Gustafson 1989;Williams & Wu 1993;Jenniskens 2006, and references therein), one of the most prominent annually periodic meteor streams. For this reason, activity around Phaethon has been searched for.…”

Section: Introductionmentioning

confidence: 99%

Near-Earth asteroid (3200) Phaethon: Characterization of its orbit, spin state, and thermophysical parameters

Hanuš

Delbò

Vokrouhlický

et al. 2016

A&A

110

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“…Assuming an albite diffusion coefficient, meteoroids smaller than 200 − 100 μm will lose 90% of the initial sodium content after 1000−4000 years, which is the probable age of the Geminid stream (e.g. Ryabova, 2007;Beech, 2002;Williams and Wu, 1993;Gustafson, 1989). Using an orthoclase diffusion coefficient, 90% sodium loss occurs in bodies smaller than 30−60 μm.…”

Section: Results For Geminidsmentioning

confidence: 99%

Quantitative model of the release of sodium from meteoroids in the vicinity of the Sun: Application to Geminids

Čapek

Borovička

2009

Icarus

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International audienceA considerable depletion of sodium was observed in Geminid meteoroids. To explain this phenomenon, we developed a quantitative model of sodium loss from meteoroids due to solar heating. We found that sodium can be lost completely from Geminid meteoroids after several thousands of years when they are composed of grains with sizes up to ∼100 μm. The observed variations of sodium abundances in Geminid meteor spectra can be explained by differences in the grain sizes among these meteoroids. Sodium depletions are also to be expected for other meteoroid streams with perihelion distances smaller than ∼0.2 AU

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“…Tables 1-3 contain the current orbital period, P , perihelion distance, q, and inclination, i, of the parent bodies taken from Williams & Wu (1993) the JPL Small-Body Database (http://ssd.jpl.nasa.gov). Note that the current orbits may differ from the situation at the time when the meteoroid stream was formed.…”

Section: Known Parent Bodiesmentioning

confidence: 99%

Properties of meteoroids from different classes of parent bodies

Borovička

2006

Proc. IAU

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Abstract. Meteoroids observed to disintegrate in the terrestrial atmosphere can be directly linked to their parent bodies in case that they belong to certain meteor showers. We present a list of two dozens of parent bodies reliably associated with well recognized meteor showers. Among the parent bodies are long period comets, Halley-type comets, Jupiter family comets, comets of the inner solar system (such as 2P/Encke) and asteroids.Physical and chemical properties of meteoroids coming from various parents are compared on the basis of meteor heights, decelerations, light curves and spectra. Jupiter family comets produce meteoroids with the lowest strength, namely porous aggregates of dust grains with bulk densities of about 0.3 g cm −3 or less. Halley type material is somewhat stronger and the material related to comet Encke is even stronger. In addition, small strong constituents, perhaps similar to carbonaceous chondrites, can be encountered within the normal cometary material. The strength of cometary material is also enhanced by long-term exposure to cosmic rays and by solar heating in the vicinity to the Sun (r < 0.2 AU). Both these processes lead to the loss of volatile sodium. Southern δ-Aquariids, Geminids and partly also Quadrantids were influenced by solar radiation. We argue that these showers, the asteroids associated with them ((3200) Phaethon and 2003 EH 1), and the whole interplanetary complexes they belong to are of cometary origin. The argument is supported by lower than chondritic Fe/Mg ratio found in Geminids as well as in Halley type comets. The typical property of stony meteoroids of asteroidal origin is the presence of internal cracks which cause that the incoming meteoroids are much weaker than the recovered meteorites.

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The Geminid meteor stream and asteroid 3200 Phaethon

Cited by 132 publications

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Near-Earth asteroid (3200) Phaethon: Characterization of its orbit, spin state, and thermophysical parameters

Near-Earth asteroid (3200) Phaethon: Characterization of its orbit, spin state, and thermophysical parameters

Quantitative model of the release of sodium from meteoroids in the vicinity of the Sun: Application to Geminids

Properties of meteoroids from different classes of parent bodies

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