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Table 1

Envisioned meteoroid streams contributing to the meteoroid flux in the L1 Lagrange point, and listed from their January to December appearance periods.

Meteoroid Parent Type e q vg Reference
stream Body (AU) (km s-1)

Quadrantids 2003 EH1 Ann. show 0.989 0.141 41 Jenniskens (2006)
and dust trails

April Lyrids C/1861 G1 Thatcher Ann. show 0.921 0.921 47 Jenniskens (2006)
and dust trails

Eta Aquariids 1P/ Halley Ann. show 0.968 0.662 67 Christou et al. (2008)
and dust trails

Tau Herculids Dust trail: ? 0.97 15
May 31, 2017
73P/Schwasmann event Jenniskens (2006)
-Wachmann 3 produced by (Table 6g)

Perseids Ann. Show: 0.951 0.948 60
and dust trail
109P/ Aug 11, 2016
Swift-Tuttle event Jenniskens (2006)
produced by
1862 trail

Kappa Cygnids Unknown Ann. show 0.763 0.980 23 Jenniskens (2006)

Taurids 2P/ Encke Ann. show 0.853 0.35 28 Jenniskens (2006)

Leonids 55P/Tempel-Tuttle Ann. show 0.918 0.985 72 Jenniskens (2006)
and dust trails

Geminids 3200 Phaeton Ann. show 0.898 0.141 34 Jenniskens (2006)

Ursids Ann. Show: 0.961 0.947 33
and dust trail
Dec 22nd, 2016
8P/ event Jenniskens (2006)
Tuttle produced by (Table 5b)
young filament
(outwards towards
Earth orbit)

Notes. The listed streams are probably contributing with old meteoroids forming the annual shower plus some punctual encounters with young dust trails (the year indicated for each trail corresponds with the year of perihelion in which it was created). Known dust trail events are listed, indicating in bold the most favorable ones. Eccentricity (e) and perihelion distance (q) are also given from Jopek et al. (2003, 2010). vg indicates the geocentric velocity relative to the Earth which roughly corresponds to the impact velocity.

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